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Can we tap ionized particles in the interstellar medium as a way of exchanging momentum for propulsion? It’s a concept with a lot of pluses if it can be made to work, chief among them the fact that such a device would be propellantless. Looking at the topic today is Drew Brisbin, a postdoctoral researcher in astronomy who received his PhD from Cornell University in 2014. Dr. Brisbin has since gone on to work towards better understanding his field of specialization: the study of galaxy evolution in the early universe. He currently works at Universidad Diego Portales, in Santiago Chile, where he collaborates closely with other researchers using some of the most sensitive telescopes in the world, located in the mountainous Chilean desert. In addition to his formal work and outdoors-oriented hobbies, he also enjoys dreaming about the future of humanity. One particular dream recently seemed to warrant some further investigation, leading him to the ideas he explains today.

By Drew Brisbin


This article represents a distillation of a work published in April 2019 in the Journal of the British Interplanetary Society (reference [0]). Some technical details have been omitted for brevity, but interested readers are encouraged to read the original publication which is freely available at https://arxiv.org/abs/1808.02019. Additional commentary has been included to address what the author sees as a critical flaw in Dr. Robert Zubrin’s “Dipole Drive” concept.


In particular light of the recent public excitement and ensuing disappointment regarding the exotic “EM drive” it is worthwhile to point out that space travel without on-board propellant is eminently possible based on well established physical principles. Here a new mode of transport is proposed which relies on electric-field moderated momentum exchange with the ionized particles in the interstellar medium. The application of this mechanism faces significant challenges requiring industrial-scale exploitation of space but the technological roadblocks are different than those presented by light sails or particle beam powered craft. This mode of space travel is well suited to energy efficient travel at velocities below about five percent the speed of light (0.05 x c) and compares exceptionally well to light sails on an energy expenditure basis. It therefore represents an extremely attractive mode of transport for slow (of order multi-century long) voyages carrying massive payloads to nearby stellar neighbors. This will be a useful niche for missions that would otherwise be too energy intensive to carry out, including initial forays into nearby stellar systems with observatory probes, or long term transport of bulk materials as a precursor mission to set up colony infrastructure.


The tyranny of the rocket equation has long been recognized as an impediment to becoming a truly spacefaring species. Due to the exorbitant reaction mass required for traditional rockets in interstellar travel, there has been considerable attention to methods of space travel that circumvent the rocket equation. Laser-driven light sails are a prominent and long-standing idea (see for example [1] and references therein). While light sails are well established and also the engines of the widely publicized Breakthrough Starshot program [2] and Project Dragonfly [3], their thrust is fundamentally limited to 6.67 N/GW. For comparison, the Three Gorges Dam, the largest capacity power plant currently in operation, has a capacity of about 22.5 GW. If this power was transmitted with perfect efficiency to a light sail it would provide thrust equivalent to the force required to lift a 15 kg mass on Earth. Scaling light sails up to larger-than-gram-scale spacecraft therefore necessarily depends on humanity’s ability to harness incredible power. Furthermore, since light is only able to push, it is very difficult for light sail spacecraft to slow down at their destination, limiting missions to fly-bys unless complicated reflecting infrastructure can be sent ahead of the craft. Alternatively, direct sunlight could be used as a source of photon pressure. Unfortunately, the material properties suggested to be necessary for a practical interstellar solar sail require materials with extremely low areal densities with σ≲10-3 g/m2 [4]. Current state-of-the-art reflective films developed for light sails reach areal densities of order 10 g/m2, or four orders of magnitude too dense even without including any support structure or payload, so it is uncertain when if ever suitable materials will be developed for an interstellar solar sail [5].

Another idea using external reaction mass is the particle-beam powered spacecraft. This hinges on a sail formed by an extended electric or magnetic field which is able to deflect a remotely-beamed stream of charged particles. Since charged particles carry much more momentum per unit energy than photons this could have much lower power requirements than light sails. This concept has its origins in the Magsail, a large loop of current carrying wire which deflects passing charged particles in the interstellar medium (ISM), eliciting a drag force which could be used as a brake to slow spacecraft down to rest with respect to the ISM after a high speed journey [6]. To provide acceleration, one could simply supplant the ISM with a beamed source of high velocity charged particles [7]. Providing a long distance beam of charged particles is, however, quite difficult because of beam divergence due to particle thermal motion, interaction with interplanetary or interstellar magnetic fields, and electrostatic beam expansion in the case of non-neutral particle beams. Andrews (2003) suggests that it would be necessary to construct a highway of beam generators at least every AU or so along the route on which the craft accelerates [8]. The related concept of the electric sail instead uses an electric field generated by a positively charged grid of wires or wire spokes extending from a central hub to push against the outward streaming solar wind [9]. This concept has the near term potential to allow travel within our own stellar neighborhood with very low energy costs. The electric sail, like the Magsail however, ultimately relies on a drag force, decelerating the spacecraft to rest with respect to the surrounding medium (the outward moving solar wind in this case). It is therefore unable to accelerate beyond the heliosphere, nor can it accelerate directly inwards towards the sun while in the heliosphere.

It would be possible to overcome these obstacles by actively pushing against the charged particles of the ISM, rather than passively coming to rest with respect to the medium. These spacecraft with interstellar medium momentum exchange reactions (SWIMMERs) can accelerate with respect to the ISM, are significantly more energy efficient than light sails, would be able to decelerate at their destination, do not require pre-established infrastructure along the route and are based on elementary physical principles. Recently Dr. Robert Zubrin discussed his independent work on a “dipole drive” concept which is similar to the SWIMMER concept described here [10,11]. Although the two ideas are related and even share a similar geometry, they were arrived at independently. Furthermore the dipole drive as described, suffers from a flaw which prevents its successful acceleration in the stationary ISM. The work presented here concerns the conceptual mechanism which allows SWIMMERs to accelerate through a stationary ISM.

Both the Magsail and electric sail concepts rely on the fact that there is significant mass in the ISM (or the heliosphere) which can interact with relatively low mass structures consisting of charged or current carrying wires. How, then, could a spacecraft interact to accelerate rather than decelerate with respect to the surrounding medium?

The need for a time varying electrical voltage

Quite generally this will require a time varying electric field which can do work on the surrounding particles of the ISM. As a thought experiment, imagine a spacecraft consisting of a pair of conducting plates arranged in a parallel-plate capacitor style configuration with a switchable power source connecting them and able to charge and discharge them at will. The conducting plates, rather than being solid, are composed of a wire mesh with the vast majority of the area taken up by open space rather than metal, such that particles are easily able to pass through the plate mesh without collision. The spacecraft is moving face on through a stationary medium of charged particles (like the interstellar medium), as shown schematically in Fig. 1. For the moment take the charged particles to be macroscopic and extremely dispersed so we can easily see individual particles and identify when they are in the vicinity of the spacecraft — charged pebbles rather than atoms or elementary particles. As the spacecraft moves through the field of charged particles we can strategically switch the power source on and off to create an electric field and push on charged particles as they pass between the conducting plates, accelerating the particles backward and creating thrust to push the spacecraft forward (Fig. 1). This scenario is perfectly in line with conservation laws. momentum is conserved since the particle gains momentum in the backward direction and the spacecraft gains momentum in the forward direction. Energy is conserved as the increase in kinetic energy (of the particle and the spacecraft) is drawn directly from the power source depleting whatever energy source is being used (depleting a battery’s chemical energy, or converting beamed laser light for instance).

In practice of course, the ISM is not made of macroscopic, easily separable pebbles, but microscopic ions and electrons with tens of thousands per cubic meter or more, so we cannot consider manually switching the charged plates based on the positions of individual particles. The possibility of simply leaving the plates continuously charged, front facing plate positive, back plate negative, may initially seem workable, and this appears to be the scenario imagined in the “Dipole Drive” [10]. Introductory electricity courses train us to think about parallel plate capacitors as having a strong field in one direction between a pair of charged plates, and no field outside the plates, so it is easy to initially imagine that a positively charged ion would approach the front plate while feeling absolutely no force, feel a strong force backwards while between the plates, and then feel absolutely no force again as it recedes beyond the back plate. In fact, however, a set of finite parallel plates will indeed have electric fields outside of their gap which directly oppose the electric field inside the gap, and would perfectly negate the thrust generated by particles transitioning the gap.

This is made more clear by considering the electrical voltage rather than electric fields. Fig. 2 (top) shows schematically the voltage through the center of an idealized infinite parallel plate capacitor charged to a potential difference of 2V. Positive charges will want to “slide down” the potential ramp located between the plates, accelerating rightward. For a finite sized set of parallel plates the voltage extends a bit to the left and right of the gap, continuously decaying from the voltage at the plates to a voltage of zero at great distances as shown in Fig. 2 (middle). Note that these voltage ramps tilt in the other way than the region between the plates and will tend to accelerate positive charges in the opposite direction. For a particle entering in from the left and making it all the way through to exit out the right side, would it end up with more or less rightward velocity? Remember that voltage (often referred to as electric potential) is simply potential energy divided by charge (in SI units 1 volt = 1 joule/coulomb). Starting out very far on the left in Fig. 2, the rightward traveling particle with charge q will have some kinetic energy, KE, and zero potential energy.

As it approaches the front plate, it will begin slowing down as it rises up the potential ramp and converting kinetic energy to potential energy, eventually reaching a peak potential energy of +qV (with a kinetic energy of KE-qV). As it traverses the gap it is accelerated rightward as it slides down the potential, eventually reaching a potential energy of -qV and a kinetic energy of KE+qV. It then exits the parallel plate gap and is again forced up a potential ramp, converting kinetic energy back into potential energy, until it finally reaches distances far away from the plates where the voltage is 0 at which point it has potential energy 0 and kinetic energy KE — exactly the same as it started.

This is not a minor fluke of this particular geometry either. Any arrangement of charged plates – so long as the voltage is finite and the plate volume is finite – will leave the potential 0 at infinity. In [11] Zubrin has suggested that Debye shielding (the phenomenon of oppositely charged free particles in a plasma tending to cluster around charged objects and screen out the electric field) would somehow ameliorate this issue, but that is not the case. The effect of Debye shielding will be for the front facing positive plate to accumulate a cloud of electrons and the back plate to accumulate a cloud of positive ions, making the voltage ramps just outside the plate pair more steeply return to zero, as shown in Fig. 2 (bottom). Nonetheless, the potential remains 0 at large distances and in the end passing particles enter and leave the system with the exact same kinetic energy. This does not preclude the particles from changing direction, either being reflected back in the direction they came, or deflected to the side if they interact with the parallel plates at an angle, so such a configuration could certainly be used to either steer or decelerate with respect to the charged particle medium, but such a system with constant voltages cannot do work on charged particles which begin and end far away, and cannot accelerate with respect to them (it could still be useful to accelerate up to the velocity of the solar wind inside our heliosphere, much like the electric sail).

If the goal is to accelerate in the dead of the ISM, it is essential that a time-varying electrical potential be used to do work on the passing particles. There are multiple ways to do this, but one simple implementation, illustrated in Fig. 3, could feature a pusher plate made of a large grid of wires moving face-on through the ISM (much like the proposed geometry of a standard electric sail). Unlike a standard electric sail, however, the grid of wires would actually be two identical layers of wire sandwiching a strong insulator between them to keep the two layers physically apart and electrically isolated. These wire grids or tethers could be made from very fine superconducting wire and the entire ensemble could be spun to create tension and keep the wire grids extended without heavy support structure. The two faces of the pusher plate would be charged and discharged cyclically. In the “primer” portion of the operation cycle, the front layer in the pusher plate is raised to a positive potential and the back layer to an equal negative potential. Due to edge effects of the finite plates and the self-shielding behavior of plasmas, this results in a decaying electric potential of opposite sign on either side of the plates. Ions streaming towards the front positively charged layer slow down, building up an overdense clump in front of the pusher plate while an underdensity forms at the immediate location of the pusher plate. Then in the “pull” stage of the cycle the potential difference across the layers is reversed and significantly increased. The ion clump that was formed in front of the plate will be attracted to the negative front layer, pulling the spacecraft forward. As the clump approaches the pusher plate, the potential difference is turned off and the clump is allowed to coast through the plate to the other side. In the final “push” stage the same potential difference is applied and the clump is further pushed backwards by the positive back layer of the pusher plate. The clump drifts away beyond the influence of the pusher plate and the cycle repeats. Fig. 4 shows the electric potential and ion density at various cycle stages for a simple model.

By intentionally setting up clumps in the oncoming ISM we can interact with it much more like in our initial thought experiment with charged pebbles. The spacecraft gains momentum by giving backward momentum to the ISM (pushing ion clumps to the right in Fig. 4). The source of the potential difference does work in the primer stage when it sets up the positive potential, raising the electrical potential energy of the ions in front and again in the push stage when it raises the ion clump to a higher potential. Electrons encountering the potential ramps will largely be reflected but this causes only a negligible momentum drag since they are far less massive than the protons and other positively charged ions. In a real three dimensional case, there will also be loss of efficiency due to particles which do not interact perfectly in one dimension, but instead are pushed off to the side as they pass by the charged wires. Furthermore, this qualitative conceptual analysis does not account for the self influencing behavior of plasmas. This will undoubtedly strongly affect the ion (and electron) distributions and the extended electric potential. Detailed particle-in-cell simulations will be necessary to investigate the optimal tuning of cycle timings, electrical potentials, and even geometry of the charged plates as it may be advantageous in some cases to accelerate ion clumps across a series of potential differences to gain more thrust per ion, at the expense of a more complex and massive pusher plate. These simulations are beyond the scope of this work but will be a critical step in transitioning the concept from a thought experiment to a practical real world device.

Mathematical expression of an idealized case

While the effectiveness and geometry of a SWIMMER will ultimately need to be tested thoroughly by simulation, it is straightforward to represent the force on an idealized system which is able to efficiently convert electrical power, P, into backwards acceleration of nearby particles. The resulting force, FSWIMMER, is

where mp is the particle mass (of order the proton mass for the ISM), n is the density of particles, v is the velocity of the spacecraft (with respect to the stationary-particle frame), and A is the cross sectional area over which the system can interact with particles (or equivalently v x A is the volume rate of particles swept out by the spacecraft through time). The positive sign is used when accelerating with respect to the the stationary-particle frame, and the negative sign is used when decelerating. The derivation of this relationship is shown in [0].

The power referred to throughout this work is the delivered electrical power. Thus far the source of power for a SWIMMER has been ignored. There is no reason a SWIMMER could not use an onboard power source, making it totally independent of external infrastructure. This, of course, would require an exceptionally energy dense fuel source as well as a very efficient generator to achieve useful velocities for interstellar travel. Beaming power remotely to the SWIMMER is possibly a more viable strategy for interstellar travel, which invites a direct comparison to light sails. In this case an additional P/c term is included in eq. 2, corresponding to the photon pressure of the beamed energy being absorbed by the spacecraft. The total force is then:

Where P/c is either added or subtracted depending on if the beamed energy source is coming from the origin or the destination respectively. It will also be useful to consider the ratio, R, of the force on a SWIMMER to the force on an ideal light sail with equal delivered power (F=2 P/c). This ratio can be written as:

where we have used the the positive signs in the SWIMMER and photon forces indicating the spacecraft is accelerating and beamed energy is coming from the origin (as would be the case for an initial out-bound journey to another star system). In Fig. 5 R is shown as a function of velocity for a few values of A/P. There is some uncertainty surrounding the structure and properties of the local ISM, but there is general consensus that a journey to Cen A will involve passage through some combination of the Local Interstellar Cloud, the Circum-Heliospheric Interstellar Medium and the G Cloud. Therefore, a conservatively low ion density of n=0.07 cm-3, consistent with the estimated densities in these clouds, (see for example [13]) is used in Fig. 5. Fig. 5 shows the force initially rising with velocity due to the fact that at higher velocities the SWIMMER plates are sweeping out larger volumes of the ISM faster and able to interact with more particles per second. The force peaks at some velocity, and then decreases since it takes more and more energy to accelerate the passing ions to yet higher velocities to get the same momentum change. Due to this initial rise in force with velocity, it may be useful to give SWIMMERs an initial velocity boost through other means (such as conventional rockets, gravitational assists, or particle beam assists) to take advantage of the forces at higher velocities.

Larger A/P values give significantly better performance at lower velocities, but trend together as velocity increases, with the force approaching (P/v) x (c+v)/c (the ratio R approaches (c+v)/(2v), shown by the red line in Fig. 5). This high velocity limit implies an order of magnitude larger force for SWIMMERs relative to light sails up to v=c/19 or about 5% the speed of light.

Example mission

To illustrate the potential of SWIMMERs for interstellar travel, it is helpful to consider a possible future mission. Further details and technical considerations are available in the published manuscript, but here we simply assume the the engineering difficulties of beaming power to interstellar distances is solved, and the onboard energy converter has a specific power capacity of 4 kW/kg (every 4 kW of delivered power requires an increase of 1 kg in the mass of the power converter equipment). The ISM is assumed to be uniform with a density of 0.07 cm-3, a temperature of 7000 K and therefore an electron Debye length, λD=21.8 m.

A relatively lower mass SWIMMER mission might have the goal of transporting a modest space probe, mpay=1000 kg to α Cen A. Accelerating within our heliosphere and decelerating at the destination are possible, and in fact relatively energy efficient but discussion of these will be left for the main publication, [0], for brevity. A modest electrical power delivered to the SWIMMER of 10 MW is assumed. The pusher plate will be made up of several long tethers. In practice these tethers will consist of very fine braided filaments to prevent failure due to micrometeoroid and interstellar dust collision, as described for the electric sail [9]. From a material mass standpoint these are considered to be single wires with an effective diameter of 30 μm. This is equivalent in material to eight filaments with diameters of about 10 μm. Given the pulsed nature of the SWIMMER electric field, the wire tethers should be made out of superconducting materials. A single charged wire will interact with charged particles passing within about λD on either side of it. The total cross sectional interaction area is given by

where L is the summed length of all the tethers. This cross sectional interaction area is somewhat of an idealization as the Debye length does not represent a hard cut off where particles suddenly cease to be effected by an electric field, and in regions where tethers intersect, part of their cross sectional areas will overlap. Nonetheless it is a sufficient estimate for our rough calculations. The mass devoted to this pusher plate will be mpusher= ρ x L x π rwire2. Where rwire represents the effective radius of the wire tether (15 μm in our case), and ρ represents the density of the tether material, which we will take to be 2570 kg/m3, the density of the popular superconducting material, magnesium diboride.

The total mass of the SWIMMER ship is comprised of mpay=1000 kg, mpower=2500 kg (given by the 10 MW supplied electric power and a 4 kW/kg specific power), and mpusher. We will take 7400 kg as the mass of the pusher plate which provides for a total summed tether length of 4.1 x 109 m. While this is seemingly a very long tether, it does not in any way represent the spatial scale of the SWIMMER, as the pusher plate will be made up of several thousand tethers, possibly splitting off from each other at greater radial distances. The summed length is merely a useful value for determining the total cross sectional area in plasmas of different temperatures and densities. In this case, from eq. 4 our SWIMMER tether length corresponds to a cross sectional interaction area of 180,000 km2 (about the size of Uruguay or the state of Washington).

We will begin our voyage as the SWIMMER enters the ISM at 100 AU with a velocity of 4.0 x 105 m/s (0.133% the speed of light and consistent with typical velocities of the solar wind). Iteratively integrating using eq. 3, we find that after just less than 300 years the spacecraft will be on the doorstep of Alpha Centauri after having travelled one parsec and achieving a final velocity of 1.66% the speed of light. Including time to initially accelerate from rest within the heliosphere and decelerate at the destination marginally increases the trip time, but we could also shorten the trip slightly by systematically shedding mass and reducing the size of the pusher plate enroute. As Fig. 5 shows, at higher velocities larger plate areas provide diminishing returns, so as the spacecraft reaches higher velocities the larger area of the pusher plate becomes dead weight. A total journey of about 300 years starting from rest in the solar system to being gravitationally captured by Cen A is reasonable for the overall journey [0].

While 300 years is a significant amount of time for a scientific endeavor, there is good precedent for multi-century science projects for worthwhile investigations (c.f. [14-16]). Furthermore, the energy expense is a pittance compared to an equivalent mission using laser-pushed light sails. An equivalent, 7400 kg probe pushed by 10 MW of laser light incident on ideal light sails (and starting with a velocity 4 x 105 m/s) would take about 1600 years to travel 1 parsec and reach a final velocity of 0.28% the speed of light. To reduce the light sail travel time to 300 years would require an average power consumption of nearly 700 MW (70x higher).


SWIMMERs represent a new mode of interstellar transport. By disposing of onboard reaction mass they circumvent the rocket equation, and by exchanging momentum with ions in the ISM they improve by orders of magnitude over the energy efficiency of traditional light sails at relatively low velocities. The key to this momentum exchange is the time varying electric field which allows SWIMMERs to create inhomogeneities in the surrounding plasma and then push on these inhomogeneities to create thrust.

SWIMMERS perform exceptionally well at lower velocities, with their advantage over light sails diminishing quickly at v > 0.05 c. Furthermore, by relying on the ambient ISM as a momentum exchange medium, they are quite versatile, able to accelerate either away or towards a beamed energy source, opening up myriad opportunities to serve as one-way transport, roundtrips or even statites remaining in stationary positions with respect to the Sun and serving as useful waypoints with infrastructure for other potential space transportation networks.

The example discussed here only scratches the surface of the possible roles for SWIMMERs in our spacefaring future. Their characteristics make them ideal for any mission with large masses in which relatively low velocities are acceptable. They are unlikely to be the sole mode of space transport due to their diminishing advantages at high velocities and their structural complexity which requires onboard power conversion systems with significant mass. They can play the role of the proverbial Mack trucks of space, transporting goods slowly and reliably at a low energy cost, while more time sensitive cargo can make use of fast yet inefficient light sails – the Ferraris of space. SWIMMERs might, for instance, be well suited to aiding the construction of a fast interstellar highway by transporting massive particle beam stations along with their fuel supply out to stationary positions between us and our target destinations. These particle beam stations could be used to swiftly carry low mass Magsails along the path or augment the power of future SWIMMERs by replacing the stationary ISM with a corridor of fast moving beamed particles.

The mission analyzed here regards a one-way interstellar trip. While it does push the limits of current technology by assuming relatively high specific power electrical systems, very thin mass-produced super conducting wire, and low mass electrical insulators which can resist large potential differences (as well as very large laser array optics which are addressed in other works regarding light sails) there is no obvious material or theoretical limits which would prevent such missions from realization. Future work in this vein will need to examine several issues ignored here. Areas of further investigation, include the efficiency of the SWIMMER drive in three dimensions; the electrical potential and cycle timings during the pulsed SWIMMER operation and how they effect the required current density of the tethers; the expected impact of interstellar dust collisions and redundant tether configurations to avoid catastrophic damage from tether breakage; and realistic limits on power conversion system capabilities.

As our understanding of interstellar travel develops, we must face the realization that, not only is it difficult, but there is no one-size-fits-all solution. Where SWIMMERs excel in one metric, other methods may excel in another. Ultimately our best strategy is to develop all possible methods in the hope that their synergy will provide a means to accomplish our goals.


0. D. Brisbin, “Spacecraft with interstellar medium momentum exchange reactions: the potential and limitations of propellantless interstellar travel”, JBIS, 72, pp.116-124, 2019.

1. R.L. Forward, “Roundtrip Interstellar Travel Using Laser-Pushed Lightsails”, J. Spacecraft and Rockets, 21, pp.187-195, 1984.

2. P. Lubin, “A Roadmap to Interstellar Flight”, JBIS, 69, pp.40-72, 2016.

3. N. Perakis, L.E. Schrenk, J. Gutsmiedl, A. Kroop, M.J. Losekamm, “Project Dragonfly: A feasibility study of interstellar travel using laser-powered light sail propulsion”, Acta Astronautica, 129, pp.316-324, 2016.

4. R. Heller, and M. Hippke, “Deceleration of High-velocity Interstellar Photon Sails into Bound Orbits at Centauri”, Astrophysical Journal Letters, 835, pp.L32, 2017.

5. D. Spieth, and R.M. Zubrin, “Ultra-Thin Solar Sails for Interstellar Travel–Phase I Final Report”, NASA Institute for Advanced Concepts, Pioneer Astronautics Inc, 1999.

6. D.G. Andrews, and R.M. Zubrin, “Magnetic sails and interstellar travel”, JBIS, 43, pp.265-272, 1990.

7. G.A. Landis, “Interstellar flight by particle beam”, in AIP Conference Proceedings, vol. 552, pp.393-396, 2001.

8. D.G. Andrews, “Interstellar Transportation using Today’s Physics”, Conference proceedings, American Institute of Aeronautics and Astronautics, 4691, 2003.

9. P. Janhunen, “Electric sail for spacecraft propulsion”, J. of Propulsion and Power, 20, pp.763-764, 2004.

10. R. Zubrin, “Dipole Drive for Space Propulsion”, JBIS, 70, pp.442-448, 2019.

11 R. Zubrin, “The Dipole Drive: A New Concept in Space Propulsion”, 70th International Astronautical Congress (IAC), Washington DC, October 2019.

12. Stilfehler, “technique of 4 strand braiding”, Wikimedia Commons file (licensed for sharing and adaptation), https://commons.wikimedia.org/wiki/File:4_Strand_Braiding.png, last accessed on 18 March 2019. Cropped and edited for 3-d effect.

13. I.A. Crawford, “Project Icarus: A review of local interstellar medium properties of relevance for space missions to the nearest stars”, Acta Astronautica, 68, pp.691-699, 2011.

14. A. Kivilaan, and R.S. Bandurski, “The one hundred-year period for Dr. Beal’s seed viability experiment”, American Journal of Botany, 68, pp.1290-1292, 1981.

15. R. Johnston, “World’s slowest-moving drop caught on camera at last”, Nature News, 18, 2013.

16. C. Cockell, “The 500-year microbiology experiment”, Microbiology Today, 95, pp.95-96, May 2014.


Amateur Astronomers Join Hunt for Exoplanets

An Australian amateur astronomer named Thiam-Guan Tan has made a name for himself in the realm of exoplanets. Tan participated in the discovery of an exoplanet that may orbit within its star’s habitable zone. LHS 1140 b is a super-Earth some 41 light years from Earth that orbits a red dwarf star. Back in September of 2016, with a number of professional observatories looking at the host star, Tan provided key data to help verify the existence of LHS 1140b.

“It was fortunate that I was able to catch a transit,” said Tan, a retired engineer with a 12-inch telescope who has also discovered several supernovae. He is quoted in a newspaper called The West Australian as saying “That night, the Centre for Astrophysics had lined up five other telescopes across Australia and Hawaii to observe but they were all clouded out.” Tan’s work with exoplanet transits continues, an illustration of the role that talented amateurs with affordable equipment (Tan’s telescope cost $15,000) can play.

Image: Thiam-Guan Tan with his telescope. Tan notes that “A couple of sources of encouragement were The Discovery of Extrasolar Planets by Backyard Astronomers (Castellano & Laughlin, 2002) and Bruce Gary’s book Exoplanet Observing for Amateurs. Credit: Thiam-Guan Tan.

In the same vein, I’ve been looking at a project called the Habitable Exoplanet Hunting Project, emerging under the guidance of coordinator Alberto Caballero, himself a dedicated amateur astronomer in Spain who is visible on YouTube through his efforts on The Exoplanets Channel. The idea of the new project is to help amateurs discover more exoplanets in the habitable zone, restricting the search to G-, K-, and M-class stars that show low flare activity. The stars examined by the project are all known to have transiting exoplanets outside the habitable zone, and all are within 100 light years of the Sun.

How to find out whether there are as yet undetected planets around such stars? Caballero looked at the amateur astronomers involved in TRESCA (Transiting ExoplanetS and CAndidates), a group organized by the Variable Star and Exoplanet Section of the Czech Astronomical Society comprising 191 observatories. He also consulted the American Association of Variable Star Observers (AAVSO) in his quest to find amateurs willing to participate in a global venture, one that could monitor specific stars at a predetermined time each week. Needless to say, the more volunteer astronomers, the better.

Image: The Parco Astronomico Lilio Savelli, Italy, an amateur observatory participating in the Habitable Exoplanet Hunting Project. Credit: Alberto Caballero.

By gathering data 24 hours a day, seven days a week, the team hopes to monitor individual targets when a transit of a habitable zone planet could occur. 32 participating amateur observatories are already onboard as the project comes online, and Caballero notes that southern sky coverage would be particularly welcome as the effort builds. You can see photos of the participating sites, some of which are quite impressive, here.

There is no shortage of targets. Among M-dwarfs, the most numerous nearby stars, there are almost 2,000 within 100 light years, and Caballero says that amateur equipment is capable of detecting habitable zone planets like the super-Earth around LHS 1140b, with a transit depth of 0.6%, as well as smaller worlds.

Caballero likewise counts 508 G-class stars within the same 100 light year radius, and well over 900 non-flare K-class stars as well. He believes that as many as 25 habitable zone planets may be discovered using these methods, if a large enough telescope network can be implemented. The chart below, showing 10 non-flare G-, K-, and M-class stars within 100 light years with known transiting exoplanets (as of March, 2019) is drawn from the project’s website.

The Habitable Exoplanet Hunting Project assumes that each amateur astronomer would need to gather data from the target star about one hour per week, provided an early goal in the range of 200 observatories can be reached. From the project’s website:

To make the process easy, the observations would be conducted at the same local time of the astronomers. For those cases when there is no observatory in a specific time zone, the observations would be assigned to the closest observatory. Adjustments would also have to be made on real time to exchange observation days when skies are cloudy. In addition, considering that most of the observatories are located in the Northern hemisphere, the Southern hemisphere observatories would have to undertake more hours of observation; for that, it would be ideal the use of robotic telescopes. Getting help from Southern AAVSO observatories could also solve the problem.

M-dwarfs would seem to be prime target stars for an effort like this because habitable zone planets are going to be close enough to the host to have short orbital periods, with high transit depth, but Caballero told Jamie Carter in this article in Forbes that his team favors K-class stars, which emit lower UV and X-ray radiation than the average G star (like the Sun), and also have a longer lifetime. It’s a telling reminder that an Earth ‘twin’ may actually orbit a slightly different kind of star, where conditions for habitability could be better than here.

Caballero’s short video explains what the project hopes to accomplish, and he tells me the network will begin a campaign on GJ 3470 some time in January. Here we have a known mini-Neptune of about 14 Earth masses with a radius 4.3 times that of Earth, orbiting a star in the constellation Cancer. So far it’s the only planet known around this M-dwarf, in a tight orbit whose proximity to the host, in addition to its size, precludes habitability (in fact, its atmosphere seems to be evaporating). GJ 3470 thus offers an ideal chance for the Habitable Exoplanet Hunting Project to show what it can do even as it enjoins amateurs to bulk up its network.


A White Dwarf’s Giant Planet

Calling it a ‘chance discovery,’ the University of Warwick’s Boris Gänsicke recently presented the results of his team’s study of some 7,000 white dwarf stars, all of them cataloged by the Sloan Digital Sky Survey. One drew particular interest because chemical elements turned up in spectroscopic studies indicating something unusual. Says Gänsicke, “We knew that there had to be something exceptional going on in this system, and speculated that it may be related to some type of planetary remnant.”

And that makes the star WDJ0914+1914 an example of what a stellar system that survived, at least partially, the red giant phase of its host star might look like as a planet orbits the Earth-sized white dwarf. This work, which draws on data from the European Southern Observatory’s X-shooter spectrograph at the Very Large Telescope in Chile, confirms hydrogen, oxygen and sulphur associated with the white dwarf, all found in a disk of gas around the star rather than being present in the white dwarf itself. Subsequent work determined that the only way to produce this particular disk configuration was through evaporation of a giant planet.

Image: Artist’s impression of the WDJ0914+1914 system. Credit: ESO.

Thus this white dwarf makes history as the site of the first detection of a surviving giant planet around this class of star. You’ll recall previous work on white dwarf atmospheres, which has given us a look at the composition of infalling material that may have been the result of the breakup of a planet, comet or asteroid (see, for example, Survivors: White Dwarf Planets).

But now we’re looking at an actual planet in the act of shedding material while still retaining its structure. The oxygen, hydrogen and sulphur found here are similar to what we see in the deeper atmospheric layers of Neptune and Uranus. Placing such a planet in a tight orbit around a white dwarf would cause high levels of ultraviolet radiation to strip away the outer atmospheric layers, creating the same kind of disk we find at WD J0914+1914.

The star’s temperature is estimated at 28,000° Celsius, while the planet is at least twice as large as the star it orbits, a world whose atmosphere is being depleted due to interactions with the star’s high energy photons. While most of the gas escapes, about 3,000 tonnes per second fall onto the disk, which is what makes the presence of the planet accessible to observers.

Image: Location of WDJ0914+1914 in the constellation of Cancer. Credit: ESO.

The planet orbits the primary at a scant 15 times the stellar radius, meaning it is 10 million kilometers away from the star, in a place that would have once been deep inside the red giant that was the white dwarf’s progenitor. The assumption here is that the planet moved closer to the star after the white dwarf had formed, perhaps through gravitational interactions with other worlds in this system. We also get a glimpse of this system’s future in the paper:

Gravitational interactions in multi-planet systems can perturb planets onto orbits with peri-centres close to the white dwarf, where tidal effects are likely to lead to circularisation of the orbit. Common envelope evolution provides an alternative scenario to bring a planet into a close orbit around the white dwarf, though it requires rather fine-tuned initial conditions and only works for planets more massive than Jupiter… As the white dwarf continues to cool, the mass loss rate will gradually decrease, and become undetectable in ~ 350 Myr… By then, the giant planet will have lost ∼ 0.002 Jupiter masses (or ∼ 0.04 Neptune masses), i.e. an insignificant fraction of its total mass.

The paper also notes a possible analogue to WD J0914+1914 in HAT-P-26b, a Neptune-mass planet orbiting a K-class star with a period of 4.26 days, adding that despite its high temperature, the small radius of WD J0914+1914 would make its planet cooler than the equivalent around a main sequence star. As to how common such planets may be, of the 7,000 white dwarfs examined by this study, only one planet has emerged. The authors point out that we can look forward to studying the roughly 260,000 white dwarfs identified by the Gaia mission, and thus could well find in this larger sample enough planets to make comparative study possible.

The paper is Gänsicke et al., “Accretion of a giant planet onto a white dwarf star,” Nature 576 (2019), 61-64 (abstract / preprint).


New Horizons: A Slowing Solar Wind Far from Earth

It should be evident why getting information about the solar wind is useful for future deep space missions. Concepts like the electric sail, recently discussed in these pages, and various forms of magnetic sail using superconductors all rely on hitching a ride on this fast-moving stream of particles and magnetic fields emanating from the Sun. A key problem has been tracking the solar wind’s behavior in space through changing solar cycles as we get to increasingly large distances from the Sun, but fortunately we do have a few assets at system’s edge.

New Horizons’ Solar Wind Around Pluto (SWAP) instrument continues to return data useful not only for Solar System science but also for understanding how the outflow from the Sun could affect spacecraft in the Kuiper Belt. Of interest here are the spacecraft’s measurements of ‘interstellar pickup ions’ in the outer heliosphere, a region through which only the two Voyagers and the two Pioneers before them have previously traveled. Pickup ions emerge when neutral material from the interstellar medium (ISM) enters the Solar System, to become ionized by the Sun’s light or by charge exchange interactions with solar wind ions.

Heather Elliott is a staff scientist at the Southwest Research Institute, deputy principal investigator of the SWAP instrument and lead author of a new paper on this work:

“Previously, only the Pioneer 10 and 11 and Voyager 1 and 2 missions have explored the outer solar system and outer heliosphere, but now New Horizons is doing that with more modern scientific instruments. Our Sun’s influence on the space environment extends well beyond the outer planets, and SWAP is showing us new aspects of how that environment changes with distance.”

Indeed. And the more eyes on the target, the better. When the Voyagers moved through the outer heliosphere, the Sun was in a very active solar cycle. New Horizons now moves through a mild solar cycle, with SWAP measuring the low flux of interstellar pickup ions with what the mission’s team describes as “unprecedented time resolution and extensive spatial coverage.” Bear in mind that we now have just one spacecraft measuring the solar wind beyond Mars, so New Horizons is our only source for the interactions between the solar wind and interstellar material.

One effect now confirmed by SWAP is that the ionization of interstellar material causes the solar wind to slow and heat up in response. Here we can draw on other spacecraft: The SWAP data can be compared to the solar wind speed measurements from 21 to 42 AU from both the Advanced Composition Explorer (ACE) and Solar TErrestrial RElations Observatory (STEREO). New Horizons was able to confirm the slowing of the solar wind evident at a distance of 21 AU (a little over the distance of Uranus from the Sun), and to show that the solar wind measured still slower, by 6-7 percent, between 33 and 42 AU.

Image: The SWAP instrument aboard NASA’s New Horizons spacecraft has confirmed that the solar wind slows as it travels farther from the Sun. This schematic of the heliosphere shows the solar wind begins slowing at approximately 4 AU radial distance from the Sun and continues to slow as it moves toward the outer solar system and picks up interstellar material. Current extrapolations reveal the termination shock may currently be closer than found by the Voyager spacecraft. However, increasing solar activity will soon expand the heliosphere and push the termination shock farther out, possibly to the 84-94 AU range encountered by the Voyager spacecraft. Credit: Southwest Research Institute; background artist rendering by NASA and Adler Planetarium.

It’s instructive to see how the boundary where the solar wind slows to less than the sound speed as it approaches the interstellar medium moves over time, a malleable feature indeed. Voyager 1 crossed this ‘termination shock’ in 2004 at 94 AU, with Voyager 2 crossing in 2007 at 84 AU. The current lower levels of solar activity presage a termination shock that is now even closer to the Sun. We’ll still be receiving New Horizons data when the spacecraft crosses the termination shock in the mid-2020s. As solar activity increases in its regular cycle, the shock may be pushed back to 84-94 AU by the time New Horizons is able to reach it.

The paper is Elliott et al., “Slowing of the Solar Wind in the Outer Heliosphere,” Astrophysical Journal Vol. 885, No. 2 (11 November 2019). Abstract.


The Purple Hills of Proxima b

In our continuing look at biosignatures that could flag the presence of life on other worlds, we’ve sometimes considered the so-called ‘red edge,’ the sharp change in reflectance of vegetation that shows up in the near-infrared. It’s worth remembering that vegetation is the largest reflecting surface on Earth (about 60 percent of the land surface), with an increase in reflectance that shows up around 700 nm. As Alex Tolley explains below, the red edge may shift depending on the evolution of plant life and the variables, including light intensity but comprising many other factors, that would affect life on M-dwarf planets. These are the first whose atmospheres we’ll be seriously examining for biosignatures, and the question of how to extrapolate from Earth life to environments as exotic as these is complex. A Centauri Dreams regular, Alex reminds us that vegetative life may prove adaptable in ways that will surprise us.

by Alex Tolley

Artist’s conception of Proxima Centauri b. Credit: M. Kommesser

Xi Jinping University, New Beijing, Mars



Contact Wendy Ho, Media Liaison.

Nov. 11, 2091

The first image of the surface ofProxima b is released today. Captured by the solar focal telescope (SoFoT), the 2-megapixel image captures the 3⁄4 illuminated planet’s surface. This is the first direct image of the planet that does not rely on using the EPSI inversion model for the reflected solar radiation. Both continents and oceans are clearly visible. The ocean appears wine-dark, and the continental landmasses are partially covered in a purplish color that is most probably vegetation. This vegetation contrasts with the orange-colored material of the deserts. There are no polar ice caps. The vegetated areas reach into the very high latitudes of both poles. The previous spectroscopic analysis had indicated that the atmosphere contained the biosignature gases oxygen and methane. The likely presence of vegetation suggests the source of this oxygen is photosynthesis. The color of the vegetation is likely due to the shift of the maximal light absorption into the red and near-infrared, as well as the lower flux of blue and green wavelengths of light in Proxima’s spectrum. This gives an orange cast to the landscape, with the bluer color of the local chlorophyll analog dimmed. The color difference seen is similar to that of undersea life on Earth which looks dark in the blue light at depth, but which are brightly colored in white light.

Professor Zhang Yong suggested that the photic zone in the oceans was likely quite shallow due to the low blue light emission of the star and that possibly the rate of photosynthesis was lower than on Earth. The Chinese star probe, New Dawn, is currently on its way to Proxima. Launched in 2077 it is expected to reach the Proxima system in 2099. The image of Proxima b is the first to have life confirmed visually and indicates that the probe will confirm life on the planet. The IAU will meet in December to select an official name for the planet and its features.

The abundance of M-dwarfs in the galaxy, as well as the M-dwarf, Proxima Centauri, having a rocky planet in the habitable zone (HZ) has renewed speculation of what adaptations photosynthetic plants might have to the red-shifted spectrum of these stars. Figure 1 below shows the difference in spectrum received by Earth compared to that of Proxima b. The red-shifted peak emission of Proxima is evident, as well as the high intensity of extremely short wavelength radiation compared to Earth.

Figure 1. Top-of-atmosphere full spectral irradiance received by Proxima b (black) and the Earth (red). An orbital distance of 0.0485 AU is assumed for Proxima b. [4]

Most speculation about the adaptation of plants concerns multicellular, terrestrial green plants that have clothed the surface of our continents. These plants are almost all green plants that contain chlorophylls a and b, whose peak absorption wavelengths are both in the blue and red end of the spectrum, and therefore reflecting wavelengths between these peaks, that we perceive as green (see figure 2). The adaptation of green plants to our sun’s spectrum leads to the speculation that plants on exoplanets around M-dwarfs will similarly adapt, with a dominant absorption that would extract more energy from the red end of the spectrum and therefore changing the apparent color of their leaves. Some have speculated that the absorption of more of the light spectrum that we are adapted to see would render the leaves almost black to our eyes.

Jack O’Malley-James, School of Physics and Astronomy, University of St Andrews:

“Plants with dim red dwarf suns for example, may appear black to our eyes, absorbing across the entire visible wavelength range in order to use as much of the available light as possible.”

In this essay, I will argue that there is evidence that chlorophylls can evolve to trap much redder light, but that this is too simplistic a story when considering how plants may evolve in response to the spectrum of M-dwarfs like Proxima.

While green plants dominate the Earth today, there are other plants that use different combinations of chlorophylls. The red algae (Rhodophyta) use chlorophylls a and d, plus a red-colored accessory pigment, phycoerythrin. These ensure that the dominant absorption is at the blue end of the spectrum, and is adapted for their deeper marine habitats where the penetrating sunlight is blue filtered. Without white light to illuminate these algae, they appear black to our eyes. The brown algae, which includes the kelps, use chlorophylls a and c and an Accessory pigment, fucoxanthin. Again, the peak absorption wavelengths are at the blue end of the spectrum as befits their subsurface, marine habitats. All these plants, whether multicellular or unicellular, capture the energy of the sun to fix carbon via photosynthesis. This reduces the carbon of the carbon dioxide (CO2) with the hydrogen in water (H2O) to produce sugars and release oxygen (O2) as a byproduct. However, this is not the only method of photosynthesis.

Figure 2. The absorption spectra of chlorophylls a and b, found in green plants and green Algae.

Bacteria also trap electromagnetic radiation and fix carbon. However, they use either hydrogen gas (H2) or hydrogen sulfide (H2S). In the latter case, they release particulate sulfur. Both of these types of photosynthesis require anoxic conditions and the bacteria live in hot springs or vents where these 2 gases are available. Both plant and bacterial chlorophylls are based on tetrapyrrole molecules. The absorption peaks of which are changed by small modifications of the structure.

Figure 3. Tetrapyrrole ring for chlorophyll a.

Figure 4. The structure of chlorophyll a. This is the primary photosynthetic chlorophyll.

While terrestrial life has evolved under our sun, there is the question of whether these light-absorbing molecules can evolve to meet the different spectra of other stars. While there is interest in whether planets in the HZ of M-dwarfs can even evolve life, that life would be limited to low energy, unicellular chemotrophs unless they can harvest the longer wavelength energy of their star.

The first question is whether these core, tetrapyrrole, light-absorbing molecules have already evolved on Earth to trap longer wavelength light. The obvious place to look is with the bacteria that live in very low light environments yet still photosynthesize to fix carbon.

The answer is yes. Of the 8 known bacteriochlorophylls, bacteriochlorophyll b that is found in purple bacteria has peak absorption wavelengths in the infrared (IR) of 835–850nm and 1020–1040nm.

Figure 5. Photosynthetic and other light-absorbing pigments. Absorbance spectra of selected chlorophylls (Chls), bacteriochlorophylls (Bchls), and carotenoids showing the wavelengths of absorption peaks. A visible spectrum colorbar is shown at the top. The y-axis scaling is arbitrary. The Chl absorbance data are of extracted pigments in methanol solution from Chen & Blankenship (2011). The Bchl a and Bchl b data are of whole cells and originate from Cogdell & van Grondelle (2003). The beta-carotene (carotenoid) spectrum is of pigment extract in hexane from Dixon et al. (2005), while the lutein (carotenoid) is from Janik et al. (2008). Pigments dissolved in solvents have absorption peaks slightly shifted from those in cells. These data are publicly available on the Virtual Planetary Laboratory Biological Pigments Database (http://vplapps.astro.washington.edu/pigments). [3]

Relatively recent work by Faries [1] and ​ Vairaprakash [2] on bacteriochlorins, modifying their side groups has shown that the peak absorption wavelength can be pushed out into the near infra-red. The number of variants in the chlorin ring exceeds that found in nature, and shows how small changes can modify the peak absorption wavelength. Figure 6 shows the results of these experiments that aimed to understand exactly how to tailor these molecules for different peak absorptions, primarily for industrial purposes. Note that all the absorption spectra retain their double peaks at each end of the visible spectrum. It should also be noted that there is clearly a drift towards a secondary peak at the short wavelengths that get shorter as the maximum peak wavelength gets longer, however this appears bound by a lower limit around 360nm, near the violet to ultraviolet transition. Whether these modifications could be produced by natural biochemistry would be interesting. The reactions needed may be outside of the possible repertoire, or too complex to prove evolutionarily viable.

Figure 6. The expansion of the spectral window for the bacteriochlorins by placement of uxochromes at designated sites affords a commensurate increase in the photochemical tailorability of this class of nature-inspired molecules. Collectively, the results provide fundamental insights into the rational design and synthesis of red- and NIR-absorbing bacteriochlorins for solar-energy and life sciences research. [2]

This bodes well for the possible evolution of photosynthesis on planets around M-dwarfs. It indicates that life could evolve to harvest energy not just of M-dwarfs, but even brown dwarfs. This would at least ensure that non-oxygenic photosynthesis by bacteria is possible to fix Carbon.

Photosynthesis in green plants consists of 2 systems, photosystem I (PS I) and photosystem 2 (PS II). PS I is the earlier system to evolve and is the reaction that drives carbon fixation in nonoxygenic, photosynthetic bacteria. PS II evolved later and uses the addition of shorter wavelength, higher energy light, captured more by chlorophyll b to split the H2O molecule to liberate O2 as a byproduct before the reactions to fix carbon.

Experimental work [5] shows that some blue light is needed for photosynthesis to operate efficiently, although red light alone will allow suboptimal photosynthesis to occur. This is important, as it implies that even terrestrial green plants should be able to grow on an exoplanet in the HZ around an M-dwarf.

So far the story suggests that photosynthesis, both oxygenic and nonoxygenic (in bacteria) should be possible under M-dwarf light. The evolution of longer wavelength absorbing light in bacterial chlorophylls, both natural and experimentally, suggests that light trapping tetrapyrrole molecules or possible analogs, should allow the evolution of photosynthesis under the light spectrum of M-dwarfs.

While O’Malley-James (see earlier quote) speculated that plants on M-dwarf planets might use more chlorophylls to capture light at different peak wavelengths, we do not see such adaptations on Earth, even though plants live in varied light condition environments. All plants seem to produce just 2 chlorophylls, with chlorophyll a being the dominant one for photosynthesis.

The question is “Why don’t plants produce more than 2 chlorophylls?” The answer lies most probably in the cost of a larger genome to code for the extra pathways and enzymes to manufacture the chlorophylls and regulate them. Instead, plants have opted for simpler, less costly solutions. The brown algae encode the biochemistry to manufacture the accessory pigment fucoxanthin, and the red algae, the protein phycoerythrin as an accessory pigment. These seem to be a tradeoff that optimizes the capture of available light energy for growth and reproduction.

However, light-capturing molecules are not the whole story. Terrestrial, multicellular plants adapt to low light conditions by a number of strategies. These include:

1. Increasing the number of chloroplasts in their cells. This is why plants in the low light understory plants of tropical jungles tend to have dark green leaves.

2. Rather than expending energy creating lignin-rich trunks to raise the leaves of trees to the sunlight, vines simply raise their leaves by climbing those trunks, or other surfaces to reach more sunlight.

One of the main objections to life on M-dwarf exoplanets is the high ultraviolet (UV) flux. On Earth, the bacterium Deinococcus radiodurans has evolved robust biology to resist radiation damage. Other organisms might respond by remaining at depth in the oceans, or under the ice to avoid the UV intensity. If the UV is inconstant, they may adapt by other means to reduce exposure. One means is to stay unicellular and attach to a motile animal than can move to safety. On Earth, we have marine slugs that ingest algae to extract their chloroplasts for photosynthesis. Maintaining algal pouches like squid do for luminescent bacteria is also a possibility.

Figure 7. The sea slug, Elysia chlorotica, eats green algae. It retains the chloroplasts so that it can harness photosynthesis for extra energy.

It is often suggested that flares will strip the atmosphere off an M-dwarf planet. If life has evolved, atmosphere stripping would freeze the oceans, creating a thick ice crust. Photosynthetic life might be able to live below that crust, trapping the light that penetrated the icy crust, or even within the ice using the tiny liquid water fraction to allow metabolism. The conclusion I draw from our one example of Earth’s plant life, is that we should be careful in extending simple logic to speculate how plants might evolve on M-dwarf planets. Lifeforms optimize a myriad of variables to gain an edge, using different strategies to maximize gene replication. As plant breeders have long since learned, it is often not possible to optimize for one feature, such as increased seed size and production, without needing to alter other features. Light intensity and spectrum are not the only variables plants will experience on M-dwarf planets and plants will find a number of ways to adapt to those conditions, probably in ways we cannot foresee based on our experience.

A final note on detection. Because of the dominance of chlorophyll a on Earth, the reflectance of the Earth has a sharp increase at wavelengths just beyond its peak absorption. This is known as the “red edge” and is suggested as a possible biosignature. O’Malley-James and Kaltenegger [6] suggest that since the early photosynthetic cyanobacteria also have the same chlorophyll type, that the red edge signature could be used even for exoplanets at a much earlier stage of the evolution of life. However, the longer wavelength peak absorption of bacteria using different bacteriochlorophylls, and the possible evolution of longer wavelength absorbing chlorophylls suggests that this red edge may shift, perhaps into the IR. If so, some flexibility in the determination of any red edge biosignature should be entertained.


1. Faries, K. M., Diers, J. R., Springer, J. W., Yang, E., Ptaszek, M., Lahaye, D., … Holten, D. (2015). “Photophysical Properties and Electronic Structure of Chlorin-Imides: Bridging the Gap between Chlorins and Bacteriochlorins.” The Journal of Physical Chemistry B, 119 (24), 7503-7515. doi:10.1021/jp511257w.

2. Vairaprakash, P., Yang, E., Sahin, T., Taniguchi, M., Krayer, M., Diers, J. R., … Holten, D. (2015). “Extending the Short and Long Wavelength Limits of Bacteriochlorin Near-Infrared Absorption via Dioxo- and Bisimide-Functionalization,”​ The Journal of Physical Chemistry B Vol. 119 (12), 4382-4395. doi:10.1021/jp512818g

3. Schwieterman, Edward. (2018). “Surface and Temporal Biosignatures.”

4. Ribas et al., “The full spectral radiative properties of Proxima Centauri,” Astronomy & Astrophysics Vol. 603, A58 (July, 2017).

5. Hogewoning, S. W., Trouwborst, G., Maljaars, H., Poorter, H., Van Ieperen, W., & Harbinson, J. (2010). “Blue light dose-responses of leaf photosynthesis, morphology, and chemical composition of Cucumis sativus grown under different combinations of red and blue light,” Journal of Experimental Botany, 61 (11), 3107-3117. doi:10.1093/jxb/erq132

6. O’Malley-James, J. T., & Kaltenegger, L. (2019). “Expanding the Timeline for Earth’s Photosynthetic Red Edge Biosignature,”. The Astrophysical Journal, Vol. 879 (2), L20. doi:10.3847/2041-8213/ab2769

7. Berdyugina, S. V., & Kuhn, J. R. (2019). “Surface Imaging of Proxima b and Other Exoplanets: Albedo Maps, Biosignatures, and Technosignatures,” The Astronomical Journal Vol. 158 (6), 246. doi:10.3847/1538-3881/ab2df3

8. Stevenson, D. S. (2017). Life Jim, But Not as We Know It. In The Nature of Life and Its Potential to Survive (Springer), 193–236. doi:10.1007/978-3-319-52911-0_5


A Closer Look at an Interstellar Comet

The interest in ‘Oumuamua and comet 2I/Borisov makes it clear that interstellar neighbors wandering into our system generate loads of media coverage. And why not: Here is a way to study material from another stellar system while remaining within our own. 2I/Borisov, for example, reaches its closest approach to Earth in early December, closing to within roughly 300 million kilometers. Whatever pushed an object like this out of the parent system cannot be known, but we’re likely dealing with gravitational disruption related to planets in the birth system. But more about that in a moment.

For thanks to Yale University astronomers Pieter van Dokkum, Cheng-Han Hsieh, Shany Danieli, and Gregory Laughlin, we have a fine new image of 2I/Borisov. This was taken on November 24 using the W.M. Keck Observatory’s Low-Resolution Imaging Spectrometer in Hawaii. The tail of the comet, according to van Dokkum, is about 160,000 kilometers long. Note the size comparison below to be reminded, as always, of the immensity of the objects we routinely study in the sky. For those of us who occasionally get jaded, here is another corrective.

Image: Left: A new image of the interstellar comet 2l/Borisov. Right: A composite image of the comet with a photo of the Earth to show scale. (Pieter van Dokkum, Cheng-Han Hsieh, Shany Danieli, Gregory Laughlin).

Gregory Laughlin points out that 2I/Borisov is evaporating as it moves through the Solar System, releasing the gas and dust so visible in its tail. Says Laughlin: “Astronomers are taking advantage of Borisov’s visit, using telescopes such as Keck to obtain information about the building blocks of planets in systems other than our own.” So true, and what an opportunity we’re opening up as we begin what will become the more routine study of such objects.

Bear in mind that according to a current Laughlin paper, written with Yale graduate student Malena Rice, we can expect a few such objects showing up every year, with much smaller (and therefore all but impossible to detect) objects coming into the Solar System in the hundreds per year. The duo studied three protoplanetary disks from the Disk Substructures at High Angular Resolution Project (DSHARP). Says Rice:

“We were looking for disks in which it was pretty clear a planet was there. If a disk has clear gaps in it, like several of the DSHARP disks do, it’s possible to extrapolate what type of planet would be there. Then, we can simulate the systems to see how much material should be ejected over time…This is actual material that makes up planets in other solar systems, being flung at us. It’s a completely unprecedented way to study extrasolar systems up close — and this field is going to start exploding with data, very soon.”

The paper on the frequency of interstellar objects is Laughlin & Rice, “Hidden Planets: Implications from ‘Oumuamua and DSHARP,” Astrophysical Journal Letters Vol. 884, No. 1 (10 October 2019). Abstract / Preprint.


Axial Tilt, Habitability, and Centauri B

Our fascination with Alpha Centauri doubtless propels at least some of the recent interest in binary star systems, as we ponder the chances for habitable worlds around the nearest stars. But given that the population of binary or multiple star systems in our galaxy is as high as it is (multiple systems are common, and about 50 percent of stars have binary companions), determining the factors that influence habitability in this environment has much broader significance. A new study out of the Georgia Institute of Technology has been looking at the issue by modeling an Earth twin in various binary scenarios.

So how does Alpha Centauri fare? We can find habitable zones in the Centauri A/B system, and into these the researchers introduced a simulated Earth around Centauri B to examine its axis dynamics. They also investigate the dynamical evolution of planets within the habitable zone of either star, generalizing from these results to the larger binary star population. The issue to be addressed: Does the axial tilt, or obliquity, of our planet, apparently a key feature in maintaining a habitable climate, survive the transition into a binary system with the features of Alpha Centauri? The answer is not encouraging for life, at least not around Centauri B.

Image: The Alpha Centauri group is the closest star system outside of our own at a distance of 4.3 lightyears; it can be found in the night sky in the constellation Centaurus. The stars Alpha Centauri A and Alpha Centauri B comprise a binary system, in which the two stars orbit one another, and close by is an additional faint red dwarf, Alpha Centauri C, also called Proxima Centauri. Some astronomers have hoped to someday find an exoplanet capable of harboring advanced life in the system, but a new study lowers those expectations while raising them for the rest of the universe. Credit: NASA/ESA Hubble Space Telescope.

Remember that Centauri B, a K-class dwarf, and the G-class Centauri A orbit each other tightly, with an orbital period of 79.91 years. We’re dealing with an elliptical orbit that varies the distance between the two stars anywhere from 35 AU to 11 AU, the latter being not much further than Saturn is from the Sun in our own system. From the perspective of a planet orbiting Centauri B, Centauri A swings relatively close and then backs away during the 80-year period, causing the simulated Earth to vary considerably in terms of obliquity. The Moon is often cited as a help in stabilizing Earth’s axial tilt, but that doesn’t help here, says lead author Billy Quarles.

“Around Alpha Centauri B, if you don’t have a moon, you have a more stable axis than if you do have a moon. If you have a moon, it’s pretty much bad news.”

From the paper:

…the added spin precession from a Luna-like moon increases the obliquity variation of an Earth-like planet orbiting α Cen B, but a different type of moon, in terms of its mass or semimajor axis, may have a negligible or more beneficial effect.

Image: Astrophysicist Billy Quarles, author of a new study on exoplanet axis tilt, stands with Georgia Tech’s largest telescope housed at its observatory. Credit: Georgia Tech / Rob Felt.

And without a moon? Quarles again:

“The biggest effect you would see is differences in the climate cycles related to how elongated the orbit is. Instead of having ice ages every 100,000 years like on Earth, they may come every 1 million years, be worse, and last much longer.”

The separation of the two stars is the key here. According to this work, Centauri A and B are simply too close for comfort, but a wider separation, which holds in most binary systems, would allow the second star’s effects to be less disruptive to the simulated Earth. I was curious about the effects of a moon, though, and went further into the paper, which notes that the disruptive effects of a moon on a simulated Earth around Centauri B are:

…in contrast to our own Earth-based expectations, where our moon does the opposite (Laskar et al. 1993b). The amount of spin precession from a moon depends on the moon’s mass and semimajor axis, where a Pluto-mass moon at a Luna-like semimajor axis aluna would have a negligible effect. A smaller semimajor axis (0.2 aluna) would allow a Pluto-mass moon to increase the spin precession and allow for larger obliquity variations. The degree to which a moon can increase the overall spin precession depends on many factors, where they are neither needed nor necessarily even desirable to obtain relatively low obliquity variations.

Image: Modeled into an orbit in the habitable zone around Alpha Centauri B, in this artist’s rendering by an author of a new study, our planet appears rather icy and inhospitable to advanced life. Credit: Georgia Tech / Billy Quarles.

Quarles points to Mars as an example of obliquity extremes influencing climate. The axial tilt of Mars varies between 10 and 60 degrees every 2 million years, as opposed to Earth’s axial tilt (between 22.1 and 24.5 degrees over a course of 41,000 years). Earth’s Moon stabilizes our planet’s obliquity, which would otherwise be affected by gravitational influences from the inner planets as well as Mars and Jupiter.

If the precession of Mars’ axis seems to have helped deplete its atmosphere, imagine an Earth precessing the same 60 degrees, which is the figure Quarles deduces for an Earth without its Moon. Clearly, the presence of a moon can have widely varying effects depending on the stellar masses and orbital parameters involved. We learn that the presence of a single large moon is just one factor in questions of habitability, and its effects are not always benign.

But the broader outlook for habitable zone planets in binary star systems seems encouraging. According to the study, a high percentage of such systems can support exo-Earths with axial tilts similarly steady to Earth’s, thus ensuring climate stability. Back to the paper:

We combine our results with population studies of binary stars (Raghavan et al. 2010; Moe & Di Stefano 2017) and find the chance that an Earth-like rotator orbiting the primary star would experience small (< 2.4°) obliquity variations is 87%, 74%, or 54%, depending on the mass of the primary (0.8, 1.0, or 1.2 M⊙ Solar-Type stars, respectively).

All told, those aren’t bad numbers given the number of multiple star systems throughout the Milky Way. The paper shows us that the evolution in axial tilt for a single Earth-like planet in the habitable zone of a binary system depends on the orbital precession induced by the companion star, while also being influenced by orbital distance, nearby terrestrial planets and moons. It’s interesting, too, to see that many disks are misaligned by around 10 percent from the binary plane, which would produce a typical obliquity variation in the neighborhood of 20%. Clearly, orbiting nearly planar with the binary would be the most desirable place to be.

It’s worth noting that the Transiting Exoplanet Survey Satellite (TESS) is expected to uncover ∼500,000 eclipsing binary systems. We’ll have no shortage of candidates for further study. Both TESS and Gaia observations, the authors say, would allow a more robust statistical approach to emerge as we examine the obliquity of planets around Sun-like stellar binaries.

The paper is Quarles et al., “Obliquity Evolution of Circumstellar Planets in Sun-like Stellar Binaries,” Astrophysical Journal Vol. 886, No. 1 (19 November 2019). Abstract / Preprint.


Seeing Titan Globally

When I think about mapping new places, I remember Vincent Van Gogh, who once said “To look at the stars always makes me dream, as simply as I dream over the black dots of a map representing towns and villages. Why, I ask myself, should the shining dots of the sky not be as accessible as the black dots on the map of France?”

Why not indeed? The exciting process of mapping new worlds continues to take place as we pursue our reconnaissance of the Solar System, now pushing well into the Kuiper Belt. Mapping Saturn’s giant moon Titan is particularly satisfying, because as you’ll recall, Voyager 1 was diverted from its original trajectory because Titan was just too interesting a target to miss. No Titan mapping then, though we did have useful scientific results, because Voyager 1 saw a world shrouded in orange smog. Cassini changed the game, of course, and now we’re looking deep beneath the clouds.

Image: The colorful globe of Saturn’s largest moon, Titan, passes in front of the planet and its rings in this true color snapshot from NASA’s Cassini spacecraft. The north polar hood can be seen on Titan (5,150 kilometers across) and appears as a detached layer at the top of the moon here. This view looks toward the northern, sunlit side of the rings from just above the ring plane. Images taken using red, green and blue spectral filters were combined to create this natural color view. The images were obtained with the Cassini spacecraft narrow-angle camera on May 21, 2011, at a distance of approximately 2.3 million kilometers from Titan. Image scale is 14 kilometers per pixel on Titan. Credit: NASA/JPL-Caltech/Space Science Institute.

Cassini made something like 120 flybys of Titan in the course of its long campaign at Saturn between 2004 and 2017, using its radar imager to penetrate the atmosphere of nitrogen and methane, while supplementing these views with data from visible and infrared instruments that could make out the larger geological features of the Mercury-sized world. Now Rosaly Lopes (JPL) has led a team of researchers in producing the first map that shows Titan’s global geology, pulling together all of these data to reveal a wide range of terrains. Says Lopes:

“This study is an example of using combined data sets and instruments. Although we did not have global coverage with synthetic aperture radar (SAR), we used data from other instruments and other modes from radar to correlate characteristics of the different terrain units, so we could infer what the terrains are even in areas where we don’t have SAR coverage.”

Image: The first global geological map of Saturn’s largest moon, Titan, is based on radar and visible and infrared images from NASA’s Cassini mission, which orbited Saturn from 2004 to 2017. Labels point to several of the named surface features. Also located is the landing site of the European Space Agency’s Huygens Probe, part of NASA’s Cassini mission. Credit: NASA/JPL-CalTech/ASU.

When we turn Titan into a map, we begin to sense how many features on the surface resemble similar features on Earth, evidencing similar geological processes at work, with methane/ethane being the operative fluid here. We’re seeing a hydrologic cycle active on a surface rich in hydrocarbon rain, a place segmented by rivers and punctuated by lakes and seas. It’s interesting to see, by the way, that David Williams (Arizona State), who was a major player in extrapolating radar images into areas not covered by radar, is also the man who will make the first global geologic map of (16) Psyche on a mission scheduled for a 2022 launch. For more on that one, see Psyche Mission Moved Up, a 2017 Centauri Dreams article.

The paper is Lopes et al., “A global geomorphologic map of Saturn’s moon Titan,” Nature Astronomy 18 November 2019 (abstract).


The Electric Sail and Its Uses

The electric sail is an intriguing propulsion concept that Pekka Janhunen at the Finnish Meteorological Institute has been championing for some years. It’s currently the subject of a NASA Phase II study and continues to draw attention despite the fact that we’re in the early stages of turning what looks like sound physical theory into engineering. What captures the imagination here is the same thing that is so attractive about solar sails — in both cases, we are talking about carrying no propellant, but instead relying on natural sources to do the work.

Here we have to be careful about terminology, because it’s all too easy to refer to solar photons as a kind of ‘wind,’ especially since the predominant metaphor is sailing. So let’s draw the lines sharply. There is indeed a ‘solar wind’ in today’s parlance, but it refers not to light but to the stream of particles, plasma and magnetic fields flowing out from the Sun into the heliosphere. An electric sail will ride this solar wind to achieve interplanetary velocities. A solar sail, on the other hand, will use solar photons, which carry no mass but do convey momentum.

Two entirely different concepts, even if both have resemblance to traditional nautical sails. Then we have the other terminological complication: A sail designed to be pushed not just by sunlight but rather by a laser or microwave beam is sometimes called a ‘light sail,’ which is how I have always referred to it, but it still uses photons for propulsion, even if they don’t come from the Sun. Maybe Manasvi Lingam and Avi Loeb have it right in their new paper to refer to photon-pushed sails of any kind as ‘light sails,’ distinguishing these from both electric and magnetic sails (magsails) that use the ‘solar wind’ as their driver. Thus:

Light sails — solar sails and those driven by beamed arrays — use electromagnetic radiation and the momentum transfer of photons. Electric sails use the particle stream of the solar wind.

The electric sail that Janhunen continues to study is the subject of Lingam and Loeb’s new paper, which has been submitted to Acta Astronautica. At the Florida Institute of Technology and Harvard University respectively, the two scientists have calculated performance possibilities for a spinning spacecraft that deploys a number of long wires to which an electrostatic charge has been induced. Solar wind protons (not photons!) reflect off these wires to produce thrust. The wires are kilometers long, and with that slight positive bias, the spacecraft carries an electron gun to manage the charge, retaining the bias against ambient solar wind electrons.

Image: The electric sail is a space propulsion concept that uses the momentum of the solar wind to produce thrust. Credit: Alexandre Szames.

Light sails, to use the Lingam and Loeb terminology, have been considered for interstellar missions for decades now (hats off to the early work of Robert Forward, Gregory Matloff and Geoff Landis, among others), but electric sails are new enough that we need information on how well an electric sail might do for this purpose. Could this technology get us to another star?

For a species like ours, anxious to see missions completed within a few human lifetimes, the answer is no. While a huge laser array like the one contemplated by Breakthrough Starshot could send a small light sail at relativistic speeds to another star, the electric sail cannot achieve the needed velocities.

A species with a different attitude toward time might fare better. The paper explains, for example, how electric sails could leverage the stellar winds of red dwarf stars, which are by far the most common kind of star in the galaxy. Because the interstellar medium itself can decelerate the sail, turning off the electron gun in deep space is essential. Careful maneuvering from star to star over millennia then allows relativistic speeds. From the paper:

…a series of repeated encounters with low-mass stars, and taking advantage of their winds, will enable the electric sail to achieve progressively higher speeds. We showed that sampling ∼ 104 stars could enable electric sails to achieve relativistic speeds of ∼ 0.2 c and that this mechanism would require ∼ 1 Myr. While this constitutes a long timescale by human standards, it is not particularly long in comparison to many astronomical and geological timescales. The ensuing relativistic spacecraft would be well-suited for tackling interstellar and even intergalactic exploration.

This is an eye-opener. We can’t rule out the possibility that species capable of operating in this time frame might deploy electric sails, but the time involved precludes their use as the primary propulsion method for interstellar missions by us. The authors note as well that because an electric sail will have a low cross-sectional area, its presence would be all but undetectable, whereas a light sail driven by a laser would demand huge amounts of energy and would be theoretically detectable at interstellar distances. So for a civilization hoping to explore in ‘stealth’ mode, an electric sail would have its advantages. These are not good SETI targets.

Returning to M-dwarf stars, the authors show that if stars are small enough (less than about 0.2 solar masses), the pressure of the stellar wind dominates over photon pressure, Speeds in the range of 500 kilometers per second seem feasible for electric sails near late-type M-dwarfs. Indeed, for F-, G- and K-class stars, electric sails fare better as propulsion systems in the vicinity of the home star than light sails.

So we are looking at a technology that, if it can be properly engineered, could play a role in shaping an interplanetary infrastructure, while yielding to faster methods for missions to other stars, unless we humans somehow attain an all but geological patience.

The paper is Lingam and Loeb, “Electric sails are potentially more effective than light sails near most stars,” in process at Acta Astronautica (preprint). For Pekka Janhunen’s concept of the electric sail as a fast interplanetary probe, see Electric Sails: Fast Probe to Uranus.


Surveying Multiple-Star Exoplanetary Systems

While the majority of exoplanet-hosting stars discovered so far are single, we do have multiple star systems in various configurations with planetary companions. This is fertile ground for study, and not just because the nearest stellar system, Alpha Centauri, contains a tight binary pair that is being closely investigated for planets. The third star here is, of course, Proxima Centauri, around which we already know of the existence of a planet in the habitable zone. The much broader question is, how likely are multiple star systems to host planets?

Tackling this question in a new study is Markus Mugrauer (Friedrich Schiller University, Jena), who has been investigating how the existence of multiple stars in a system affects the formation and development of planets. Mugrauer has been working with the second data release from the European Space Agency’s Gaia mission (made available in April of last year). This release contains data collected by Gaia during the first 22 months of its mission. Mugrauer’s survey searched for stellar companions of 1367 exoplanet host stars within about 500 parsecs of the Sun, or roughly 1600 light years, as listed in the Extrasolar Planets Encyclopedia.

Image: These images show some of the exoplanet host stars with companion stars (B, C) that were found during the project. The images are RGB composite images taken with the Panoramic Survey Telescope and Rapid Response System (PanSTARRS) in the y- (960 nm), i- (760 nm), and g-band (480 nm). The image in the middle shows a hierarchical triple star system. Credit: Markus Mugrauer, PanSTARRS.

207 companion stars turn up in this work, varying strongly in mass, temperature and stage of stellar evolution. Of these, 176 are found to be binaries, 27 triple star systems, and one is a quadruple star system, which produces a multiplicity rate of about 15 percent. In each case, Mugrauer uses the Gaia data to demonstrate that the host stars are equidistant and share a common proper motion.

The heaviest of the companion stars weighs 1.4 solar masses; the lightest is a scant 8 percent of the Sun’s mass. As might be expected from their ubiquity, most companion stars turn out to be low-mass, cool red dwarf stars, although it’s interesting to note that eight white dwarfs are also found among the faint stellar companions. The projected separation between these exoplanet hosting systems ranges from 20 AU to 9100 AU, with the highest frequency being within 1000 AU (by comparison, the mean separation of Centauri A and B is 23 AU).

Image; A triple star system approx. 800 light years from the Earth in the Leo constellation with the planetary host star K2-27 (bright star on the left). The image is an RGB composite image taken with PanSTARRS in the y- (960 nm), i- (760 nm), and g-band (480 nm). To the right of it, the first companion star (A) can be clearly distinguished. Just below K2-27 is the second companion star (C) that glows faintly red. Credit: Markus Mugrauer, PanSTARRS.

The results point to what is likely the disruptive influence of several stars in a system where planets are forming, for Mugrauer’s 15 percent incidence of multiple star systems contrasts with the frequency of multiple systems in general. From the paper;

In order to compare the companion star fraction found in this study among exoplanet host stars to that of the solar like stars in general one has to consider only the range of projected separation of the companions detected here, i.e. 19 up to the applied search radius of 10 000 au. This requires the determination of the orbital periods of the detected companions, following the procedure, as described by Raghavan et al. (2010) for wide companions…

Working these calculations, Mugrauer comes up with the following:

The range of separation 19 up to 10 000 au corresponds to orbital periods log(P[d]) = 4.59–8.67. According to the period distribution of companions of solar like stars for this range of period one expect[s] a companion star fraction of 30 ± 2  per cent, which is about twice as large as the fraction found in the study, presented here, among exoplanet host stars.

In other words, the frequency of exoplanet-hosting multiple star systems is about half what we would expect for solar-like stars in general, and the distances between companion and primary star in exoplanet systems are roughly five times greater than in ordinary systems. We may be looking at the gravitational influence of the companion on the gas and dust disk out of which planets emerge. Says Mugrauer: “These two factors taken together could indicate that the influence of several stars in a star system disrupts the process of planet formation as well as the further development of their orbits.”

Mugrauer’s work is continuing via an international observing campaign being conducted at the Paranal Observatory of the European Southern Observatory in Chile, which will apply data from Gaia to more precisely characterize newly discovered planetary host stars and their companions.

Image: HIP116454 is a planetary host star in the Pisces constellation and it is approx. 200 light years from the Earth. The star is accompanied by a significantly fainter white dwarf (B). The image is an RGB composite image composed of images taken in the i- (760 nm), r- (620 nm), and g-band (480 nm) as part of the Sloan Digital Sky Survey (SDSS). Credit: Markus Mugrauer, SDSS.

The paper is Mugrauer, “Search for stellar companions of exoplanet host stars by exploring the second ESA-Gaia data release,” Monthly Notices of the Royal Astronomical Society 13 November 2019 (full text).