HD 219134: A Nearby System with Multiple Transits

by Paul Gilster on March 10, 2017

While we’ve all had our eyes fixed on TRAPPIST-1 (amid the still lingering excitement of the discovery of Proxima Centauri b), news about another stellar neighbor has caused only a faint stir. But what’s happening around HD 219134 (Gliese 892) is noteworthy, and it’s interesting to see that Michaël Gillon (University of Liège – Belgium) has had a hand in it. Gillon, after all, led the work on TRAPPIST-1’s two waves of exoplanet discoveries, culminating in the startling assemblage of seven Earth-sized worlds around the dim ultracool dwarf star.

download

HD 219134 is an orange K-class star (K3V) in the constellation Cassiopeia, and only about half the distance, at 21.25 light years, as TRAPPIST-1 (about 40 light years out). It was known before the recent Gillon et al. paper in Nature Astronomy that we had a super-Earth, HD 219134 b, in orbit here, which was soon joined by two more super-Earths, a gas giant and, a few months later, another two planets, making for a total of six.

This system characterization was radial velocity work using the HIRES Spectrograph at the Keck I telescope which you can track in A Six-Planet System Orbiting HD 219134 — Steven Vogt was lead author on that paper. I notice that Greg Laughlin, also at UC-Santa Cruz and a co-author on the Vogt paper, has singled out the latest work by Gillon and team on his systemic site. That’s because Gillon adds to the one already known transiting world (HD 219134 b) another transiting planet (HD 219134 c), which gives us the closest transiting exoplanet to Earth yet found.

Image: Exoplanet hunter Michaël Gillon (University of Liège, Belgium).

Both transits are Spitzer detections, and both planets have mass and radius estimates that make a rocky composition possible (4.74 ± 0.19 M and 1.602 ± 0.055 R for HD 219134 b, and 4.36 ± 0.22 M and 1.511 ± 0.047 R for HD 219134 c). Laughlin adds that this system “…very cleanly typifies the most common class of systems detected by the Kepler Mission — multiple-transiting collections of super-Earth sized worlds with orbital periods ranging from days to weeks. Upscaled versions, that is, of the Jovian planet-satellite members of our own solar system.”

Screenshot from 2017-03-10 08-46-47

Image: From the systemic site, the HD 219134 system plotted on a mass-period diagram of exoplanets found through the various methods of detection. Credit: Greg Laughlin.

We can expect to hear a good deal more about HD 219134 in upcoming space-based observations. Unfortunately, the K-class star is too bright for some, though not all, James Webb Space Telescope instruments. JWST may be able to detect atmospheric signatures for both transiting planets if they have extended atmospheres dominated by hydrogen. More compact atmospheres dominated by H2O or CO2 would demand precisions out of reach for JWST because of stellar brightness. The paper adds: “…the precisions are limited not by the photon noise but by the instrumental systematics.”

However, we may not be done with transits in this system. The detection of the HD 219134 c transit increases the probability that planets d and f also transit. From the paper:

Using the formalism of previous work, we compute posterior transit probabilities of 13.1% and 8.1% for planets f and d, respectively, significantly greater than their prior transit probabilities of 2.5 and 1.5%… A transit detection for one or both of these planets would increase further the importance of the system for comparative exoplanetology, and a search for their transits is thus highly desirable. Although such a transit search is probably out of reach of ground-based telescopes, it could be performed again by Spitzer, whose operations have been extended to end-2018, or by the space missions TESS [Transiting Exoplanet Survey Satellite] and CHEOPS [CHaracterising ExOPlanet Satellite], which are both due to launch in 2018.

Nearby transiting planets around a small star make HD 219134 a target we’ll be investigating for a long time to come. We can begin to put constraints on possible atmospheres for the two inner worlds in this system, and also tighten up our figures for planetary mass and radius while gaining valuable insights into the formation of super-Earths. You can see how the high-priority target catalog is growing for future observations, and we can expect our space-based assets to continue to add to it as TESS and CHEOPS come online.

The paper is Gillon et al., “Two massive rocky planets transiting a K-dwarf 6.5 parsecs away,” published online by Nature Astronomy 2 March 2017 (full text).

tzf_img_post

{ 17 comments }

Kepler Data on TRAPPIST-1 Coming Online

by Paul Gilster on March 9, 2017

K2 Campaign 12 is an observational window that comes at the right time. Operating as the K2 mission, the Kepler spacecraft collected data from December 15, 2016 to March 4 of this year on the TRAPPIST-1 system. With seven planets, at least six of them likely to be rocky worlds, TRAPPIST-1 is suddenly high on everyone’s target list for future observation. The new Kepler data are a key part of this, as Geert Barentsen, K2 research scientist at NASA’s Ames Research Center at Moffett Field, California, explains:

“Scientists and enthusiasts around the world are invested in learning everything they can about these Earth-size worlds. Providing the K2 raw data as quickly as possible was a priority to give investigators an early look so they could best define their follow-up research plans. We’re thrilled that this will also allow the public to witness the process of discovery.”

The raw cadence data — ‘cadence’ refers to the time between observations of the same target — are available from the archive at MAST. Note that these are raw data files, absent any vetting or processing. Data that have been put through this process will be available some time in June. On the NASA Kepler & K2 site, Barentsen described the use of the data this way:

While we recommend that scientists only use the pipeline-processed data products in journal papers, we do encourage our community to share their understanding of the raw data with the public by blogging or tweeting tutorials and analyses. This public TRAPPIST-1 data set offers a unique opportunity to let a wider audience witness the process [of] scientific discovery.

trappist1_mask

Image: Simulated image of TRAPPIST-1’s location on the detector, from the “Create Optimal Aperture” component of the Photometric Analysis module. The 11×11-pixel aperture of K2 ID 200164267 is represented by the yellow dots. The output module for TRAPPIST-1 is 19.4, its channel is 68, and it’s located approximately at pixel row 27, column 992. Credit: MAST/STScI.

Meanwhile, the raw, uncalibrated data are intended as an aid to astronomers as they prepare proposals due this month for further investigations of TRAPPIST-1 by telescopes on Earth. Needless to say, the data gathered here, once refined and fully examined, will also factor into observations of the TRAPPIST-1 planets by the James Webb Space Telescope.

K2 Campaign 12 offers 74 days of monitoring, the longest, nearly continuous set of observations of the star yet, and as this NASA news release explains, the data give us the chance to refine earlier measurements of the TRAPPIST-1 planets, refine the orbit and mass of the seventh planet (TRAPPIST-1h), and delve into the magnetic activity of the host star.

The preparation for this observing run began in May of 2016, when the discovery of the first three planets in the system was announced. The Kepler spacecraft’s operating system was then tweaked to make needed pointing adjustments for Campaign 12. A good bit of serendipity went into the observations, for the original coordinates for Campaign 12 were set in October of 2015 before the TRAPPIST-1 planets were known. Had the exoplanet discovery not occurred when it did, Campaign 12 might have missed the system entirely.

“We were lucky that the K2 mission was able to observe TRAPPIST-1. The observing field for Campaign 12 was set when the discovery of the first planets orbiting TRAPPIST-1 was announced, and the science community had already submitted proposals for specific targets of interest in that field,” said Michael Haas, science office director for the Kepler and K2 missions at Ames. “The unexpected opportunity to further study the TRAPPIST-1 system was quickly recognized and the agility of the K2 team and science community prevailed once again.”

Another indication of the importance of the TRAPPIST-1 planets, and the likelihood that atmospheres here will be among the first investigated as we begin the search for biomarkers.

exoplanet20170223b

{ 20 comments }

The seven planets circling the star TRAPPIST-1 have been lionized in the media, and understandably so, given that more than one have the potential for habitability. But of course M-dwarfs call up the inevitable problems associated with such tiny stars. Habitable planets must orbit close to the star, with the probability of tidal lock and subsequent climatic issues. Moreover, the flare activity particularly in young M-dwarfs gives cause for concern.

It’s the latter issue that Jack T. O’Malley-James and Lisa Kaltenegger (both at Cornell, where Kaltenegger is director of the Carl Sagan Institute) have explored in a new paper to be published in The Astrophysical Journal. As the paper explains, the question of habitability becomes troubling when we realize how frequently an M-dwarf can flare. Proxima Centauri, an M5 star, undergoes intense flares every 10 to 30 hours, with effects on the planet in its habitable zone that are still unknown. Can a planet with high doses of ultraviolet radiation remain habitable under such bombardment?

We probe such questions with particular urgency because 75 percent of the stars in the neighborhood of the Sun are M-dwarfs, and we’re about to send the TESS mission (Transiting Exoplanet Survey Satellite) into space to look for habitable zone planets around nearby stars. TESS will be able to do this for late M and early K stars, and as Kaltenegger notes, the mission is expected to uncover hundreds of planets between 1.25 and 2 Earth radii in size, and tens of Earth-sized planets, some of them likely to be in the habitable zone.

proxima_b-107lfxs-768x499

Image: Artist’s impression of the Alpha Centauri stellar system as viewed from the surface of the habitable-zone planet Proxima b. Credit: ESO/M. Kornmesser

TESS findings will be handed off to future ground and space-based missions for detailed study, making it likely that the first habitable zone planet that we can characterize will orbit a nearby M star. Recent studies have looked at the biological effects of radiation for atmospheres corresponding to different times in the evolution of the Earth, finding that such a planet orbiting an inactive M-dwarf would receive a lower ultraviolet flux than Earth.

But active M-dwarfs are another story. Planets orbiting such a star would receive bursts of UV in their tight, habitable zone orbits, increasing the surface UV flux by as much as two orders of magnitude for up to several hours. Add in the fact that M stars remain active for longer periods than G-class stars like the Sun, and the scenario looks dicey for life indeed. Consider the atmospheric effects, as noted in the paper:

The close proximity of planets in the HZ of cool stars can cause the planet’s magnetic field to be compressed by stellar magnetic pressure, reducing the planet’s ability to resist atmospheric erosion by the stellar wind. X-ray and EUV flare activity can occur up to 10-15 times per day, and typically 2-10 times, for M dwarfs (Cuntz & Guinan, 2016), which increases atmospheric erosion on close-in planets. This results in higher fluxes of UV radiation reaching the planet’s surface (Lammer et al. 2007; See et al., 2014) and, potentially, a less dense atmosphere.

We also have to keep in mind that in such close orbits, the effect of the star’s stellar wind would be orders of magnitude stronger in the habitable zone than what Earth experiences. The result: Erosion of any protective ozone shield and potential loss of at least some of the atmosphere. Biological molecules under such conditions can undergo mutation. We’re fortunate that on our planet, the ozone layer blocks the most damaging UV wavelengths. For life to flourish, some way of protecting it from this radiation is thus a prerequisite.

Screenshot from 2017-03-08 09-37-51

Going underwater is one solution, or burrowing deep into the ground, a strategy that could prove life-saving but also make detection by remote instruments extremely difficult. But there is one adaptation that would be detectable: photoprotective biofluorescence. In this process, protective proteins absorb harmful wavelengths and re-emit them at longer, safer wavelengths. Some species of coral are believed to use this mechanism to protect symbiotic algae needed for energy, with fluorescent proteins absorbing blue and UV photons and re-emitting them at longer wavelengths.

Image: This is Figure 1 from the paper, showing an example of coral fluorescence. Coral fluorescent proteins absorb near-UV and blue light and reemit it at longer wavelengths (see e.g. Mazel & Fuchs 2003). Image made available under Creative Commons CC0 1.0 Universal Public Domain Dedication.

Biofluorescence occurs when specialized fluorescent molecules are excited by high-energy light, causing them to absorb part of that energy and release the rest at lower-energy wavelengths. Such biofluorescent light can only be seen when the organism is being illuminated, which could be the key to their detection on other worlds. From the paper:

Photoprotective biofluorescence (the “up-shifting” of UV light to longer, safer wavelengths, via absorption by fluorescent proteins), a proposed UV protection mechanism of some coral species, would increase the detectability of biota, both in a spectrum, as well as in a color-color diagram. Such biofluorescence could be observable as a “temporal biosignature” for planets around stars with changing UV environments, like active flaring M stars, in both their spectra as well as their color.

The color-color diagram referred to above is frequently used in the study of star-forming regions, and as a way of comparing the apparent magnitudes of stars. Here one observes the magnitude of an object successively through two different filters — the difference in brightness between two bands at certain wavelengths is what is referred to as ‘color.’ One brightness range is plotted on the horizontal axis, while another range is plotted on the vertical axis.

kaltenegger

Image (click to enlarge): A color-color diagram. This is Figure 10 from the paper. Caption: Color-color diagrams of planet models with an atmosphere and 50% cloud cover, and a surface that is completely covered by biofluorescent corals, fluorescent minerals, or vegetation compared to the colors of planets in our own Solar System, before (grey – labelled A, B, C, D) and during fluorescence at each of the four common emission wavelengths. Credit: Jack O’Malley-James / Lisa Kaltenegger.

The authors argue that color-color diagrams can distinguish biological sources of fluorescence from abiotic ones, as the change in color that biofluorescence produces differs from all other forms of the phenomenon:

Using a standard astronomy tool to characterize stellar objects, a color-color diagram, one can distinguish planets with and without biofluorescent biosignatures. The change in color caused by biofluorescence differs, in position and magnitude, from that caused by abiotic fluorescence, distinguishing both.

The authors point out that Proxima b will be a prime target to search for biofluorescence with the upcoming European Extremely Large Telescope. But TESS should give us a number of useful targets as we examine stars during flare periods looking for a biofluorescent biosphere. In other words, it may be that in the case of a planet orbiting an active M-dwarf, it’s precisely the high UV flux that will allow us to detect a biosphere that would otherwise be hidden.

The paper is O’Malley-James and Kaltenegger, “Biofluorescent Worlds: Biological fluorescence as a temporal biosignature for flare stars worlds,” to be published in The Astrophysical Journal (preprint). A second paper from Lisa Kaltenegger, “UV Surface Habitability of the TRAPPIST-1 System,” is now under review at Monthly Notices of the Royal Society. More on that one when I have a copy to work with.

tzf_img_post

{ 19 comments }

Ceres: Close Look at Occator Crater

by Paul Gilster on March 7, 2017

We’ve looked recently at the possibility of cryovolcanism on Ceres with regard to the unusual feature called Ahuna Mons (see Ice Volcanoes on Ceres?). Now we have further evidence that outbursts of brine from beneath the surface have been occurring over long periods of time, and that some of these eruptions have been recent. The work comes out of analysis of data from the Dawn mission by scientists at the Max Planck Institute for Solar System Research (MPS), and moves the debate to the unusual crater called Occator.

standard_sans_both

Image: This view of the whole Occator crater shows the brightly colored pit in its center and the cryovolcanic dome. The jagged mountains on the edge of the pit throw their shadows on parts of the pit. This image was taken from a distance of 1478 kilometers above the surface and has a resolution of 158 meters per pixel. NASA/JPL-Caltech/UCLA/MPS/DLR/IDA.

Dawn’s Low Altitude Mapping Orbit (December 2015 to September 2016) took the spacecraft to within 375 kilometers of the surface, allowing highly resolved images of Ceres’ surface to be obtained. The geological structures on display within Occator, tracked by the Dawn Framing Cameras and its infrared spectrometer, include smaller, younger craters along with fractures and avalanches, all presenting us with a look into the crater’s evolution.

The bright dome in Occator crater’s central pit, now known as Cerealia Facula, is one of Ceres’ most intriguing features. Infrared data have shown it to be rich in carbonates. Beyond the pit itself, we also find other bright areas called Vinalia Faculae, considerably paler and evidently thinner, though likewise containing carbonates along with dark surrounding material. The MPS researchers, led by Framing Camera lead investigator Andreas Nathues, have evaluated images of Occator from various distances and different angles of view.

It took more than a single impact to produce what we see in Occator crater, though that impact was likely the trigger for subsequent cryovolcanism. As explained by Nathues:

“The age and appearance of the material surrounding the bright dome indicate that Cerealia Facula was formed by a recurring, eruptive process, which also hurled material into more outward regions of the central pit. A single eruptive event is rather unlikely.”

standard_sans_both (2)

Image: False color mosaic showing parts of Occator crater. The images were taken from a distance of 375 kilometers. The left side of the mosaic shows the central pit containing the brightest material on Ceres. It measures 11 kilometers in diameter and is partly surrounded by jagged mountains. In the middle of the pit a dome towers 400 meters high covered by fractures. It has a diameter of three kilometers. The right side of the mosaic shows further, less bright spots in Occator crater. NASA/JPL-Caltech/UCLA/MPS/DLR/IDA.

What’s especially interesting here is the age issue, for this is the first time scientists have determined the age of the bright material. As this MPS news release explains, Nathues and team believe the central pit in Occator, which contains a jagged ridge, is all that is left of a former central mountain that would have formed as a result of the impact that created the crater about 34 million years ago. The age estimate comes from studying smaller craters formed from later impacts, and the Dawn images are so highly resolved that the crater count — and the age estimates that emerge from it — are the most accurate to date. The bright material of the dome is made up of much younger material, about four million years old.

standard_sans_both (1)

Image: This 3d-anaglyph for the first time shows a part of Occator crater in a combination of anaglyphe and false-color image. NASA/JPL-Caltech/UCLA/MPS/DLR/IDA.

Domes like this, interpreted as signs of cryovolcanism, appear on the Jovian moons Callisto and Ganymede, and the new work argues that the same process is happening on Ceres. The original Occator impact would have caused subsurface brine to move closer to the surface, allowing water and dissolved gases to form a system of vents. Fractures on the surface formed, from which brine began to erupt, depositing salts that led to the formation of the dome.

The process may still be active, though at a much lower level. Imagery of the area at certain angles has revealed what appears to be haze, a phenomenon the researchers explain as the result of sublimating water ice. Imagery from Dawn taken at distances as far as 14000 kilometers have shown unmistakeable variations in brightness that follow a diurnal rhythm. Says Guneshwar Singh Thangjam (MPS):

“The nature of the light scattering at the bottom of Occator differs fundamentally from that at other parts of the Ceres surface. The most likely explanation is that near the crater floor an optically thin, semi-transparent haze is formed.”

I should add, though, that there is a great deal we have yet to learn about this haze, as explained in one of two papers on this work:

The available data are insufficient for an analysis of the optical properties of this haze, but it is most likely an optically thin and semi-transparent layer forming at near-surface level. Diurnal albedo variations that correspond to Occator’s longitude have been detected by radial velocity changes (Molaro et al. 2016) supporting the existence of a temporarily varying haze layer. The detection of water-ice signatures at Oxo [a second crater at which haze has been detected] further supports ongoing sublimation activities on Ceres. Although we expect the maximum haze concentration above the central spot in Occator, it is remarkable that our data also indicate activity at the secondary spots.

The water sublimation, and thus the intensity of the haze, varies with the degree of sunlight. This explanation makes Ceres the closest body to the Sun that experiences cryovolcanism. It is the age difference — the bright deposits are 30 million years younger than the crater — as well as the distribution of the bright material within the crater itself, that tells us how active Occator crater has been and, on a much smaller scale, continues to be to this day.

The paper is Nathues et al., “Evolution of Occator Crater on (1)Ceres,” The Astronomical Journal Volume 153, Number 3 (17 February, 2017). Abstract available. See also G. Thangjam et al., “Haze at Occator Crater on Dwarf Planet Ceres,” The Astrophysical Journal Letters Volume 833, Number 2 (15 December, 2016). Abstract / Preprint.

tzf_img_post

{ 20 comments }

Fragmented Asteroid Develops Comet-like Tails

by Paul Gilster on March 6, 2017

You wouldn’t expect main belt asteroids to develop tails like comets — their orbits are circular enough that they don’t undergo the kind of temperature swings many comets experience in their plunge toward perihelion — but we do have some twenty cases of asteroids that do exactly that. The photo below, showing imagery from the 10.4-meter Great Canary Telescope, gives us views of asteroid P/2016 G1, with a smudgy dust trail splayed out behind the object.

fig21

Image: Asteroid P/2016 G1 at three different times in 2016: late April, late May and mid June. The arrow in the center panel points out an asymmetric feature that can be explained if the asteroid initially ejected material in a single direction, perhaps due to an impact. Credit: Fernando Moreno (Institute of Astrophysics of Andalusia, Spain).

Moreno and team, who have specialized in the dust environment near main belt objects, have now uncovered another intriguing asteroid, this one with an even more curious tail. Asteroid P/2016 J1 turns out to be an asteroid pair, of a kind that seem to occur not infrequently in the main belt. The likely origin of the pair is an impact that broke a single asteroid into two parts, but astronomers studying the object also believe it could have fragmented because of an excess of rotational speed. Asteroid pairs gradually drift apart from each other, their gravitational link not strong enough to hold them together, but they remain in roughly similar orbits around the Sun.

p_2016_j1

Image: Images of the P/2016 J1 asteroid pair taken on May 15th, 2016. They show a central region, the asteroid, and a diffuse blot corresponding to the dust tail. Credit: Moreno et al.

Moreno notes what makes P/2016 J1 unusual: Both fragments show dust structures similar to a comet, making this the first time we have seen an asteroid pair undergoing simultaneous activity. Both elements of the pair became activated near perihelion, between the end of 2015 and the beginning of 2016, and they displayed their tail-like structures for up to nine months.

Moreno and team used the Great Telescope of the Canary Islands (GTC) and the Canada-France-Hawaii Telescope (CFHT) to study the P/2016 J1 pair, discovering that the asteroid fragmented about six years ago, based on analysis of its orbital evolution. This makes it the youngest asteroid pair known. The asteroid pair takes 5.65 years to complete an orbit, meaning that the fragmentation would have occurred on the previous orbit.

Screenshot from 2017-03-06 09-26-32

Image: This is part of Figure 1 from Moreno et al.’s paper on P/2016 J1. Images of P/2016 J1-A and J1-B obtained with MegaCam on the 3.6m CanadaFrance-Hawaii-Telescope on March 17, 2016 (a), and with OSIRIS at the 10.4m Gran Telescopio Canarias on May 15, 2016, May 29, 2016, and July 31, 2016 (b,c,d). In panels (a),(b),(c), and (d), the physical dimensions are 170982×33925, 133788×26545, 135616×26908, and 184964×36699 km, respectively. Credit: Moreno et al.

The tail is not directly caused by the original fragmentation, but seems to have happened as an after-effect. Moreno believes we are looking at dust emissions caused by the sublimation of ice that was originally exposed by the breakup. This contrasts with the earlier asteroid tail on P/2016 G1, which Moreno and colleagues believe was the result of an impact. The team’s models show that the ejected material on P/2016 G1 was not isotropically emitted.

hs-2013-52-a-print.jpg

Image: Another view of an activated asteroid with a tail, this one showing Hubble Space Telescope images of the asteroid P/2013P5. Credit: NASA/ESA.

The paper on P/2016 J1 is Moreno et al., “The splitting of double-component active asteroid p/2016 J1 (PANSTARRS),” The Astrophysical Journal Letters Vol. 837, No. 1 (2017). Abstract / preprint. The paper on P/2016 G1 is Moreno et al., “Early Evolution of Disrupted Asteroid P/2016 G1 (PANSTARRS),” The Astrophysical Journal Letters Vol. 836 No. 2 (2016). Abstract / preprint.

tzf_img_post

{ 4 comments }

‘Dust Traps’ and Planet Formation

by Paul Gilster on March 2, 2017

Are we homing in on a ‘missing link’ in our theories of planet formation? Perhaps so, judging from the work of researchers at Swinburne University of Technology, Lyon University and St. Andrews University. The work does not challenge a central principle in current thinking, that planets form out of disks of gas and dust grains around young stars. We know that these dust grains grow into centimeter-sized aggregates. We also know that, much later, planetesimals (kilometers in size) grow into planetary cores.

What has been missing is an understanding of how the early ‘pebbles’ are able to aggregate into asteroid-sized objects. One problem is that drag in the disk produced by surrounding gas makes the grains move inward toward the star, a movement that can deplete the disk. The paper describes this as a ‘radial drift barrier,’ in which the grains settle to the midplane of the disk and drift inwards as they lose angular momentum. Taken to its conclusion, the process can lead to accretion into the star, preventing disk grains from ever forming planetesimals.

The second issue: Larger dust grains with higher relative velocities can experience collisions that make aggregation impossible. This is the so-called ‘fragmentation barrier,’ where dust grains shatter instead of sticking after collisions.

How, then, do planets actually form? The researchers have created simulations developing a theory involving ‘dust traps,’ high-pressure locations in the disk where dust grains accumulate as drift motion slows. The accumulation of growing and fragmented grains interacts with circumstellar gas to create these areas, in which trapped particles can grow. At reduced speeds within the traps, the grains avoid fragmentation. The process is depicted in the image below.

dust-trap-formation

Image: The stages of the formation of dust traps. The central (yellow) star, surrounded by the protoplanetary (blue) disk. The dust grains make up the band running through the disk. Credit: © Volker Schubert.

Thus dust grains modify the structure of the surrounding gas. Sarah Maddison (Swinburne University) explains:

“What we have been able to identify is the key role of the drag of dust on the gas. Often in astronomy, the gas tells the dust how to move, but when there is a lot of dust, the dust tells the gas how to move. This effect, known as aerodynamic drag back-reaction, is usually negligible. However, the effect becomes important in dust rich environments, like those found in the planet formation process.”

Back-reaction, in other words, slows the drift of dust grains inward toward the star, giving them time to grow in size to the point where drag from the gas no longer determines their fate. The gas is pushed outwards to form the high pressure region the team calls a dust trap. Concentrated dust grains in the dust traps then spark the subsequent formation of planets.

The process functions in the team’s simulations for a wide range of initial disk structures and dust to gas ratios. From the paper:

We demonstrate that this process is extremely robust and that self-induced dust traps form in different disc structures, with different fragmentation thresholds, and for a variety of initial dust-to-gas ratios. Changing these parameters result in self-induced dust traps at different locations in the disc, and at different evolutionary times.

The process, then, should be widespread despite differences in the stellar environment. The key thing is that the formation of the dust traps makes subsequent planet formation possible. How the fragmentation of dust grains operates determines the result:

While seemingly counter-intuitive, fragmentation is a vital ingredient for planet formation as it helps to form dust traps at large distances from the star. Indeed, fragmentation only allows grains to grow exterior to a certain radial distance and when grains decouple from the gas and start piling up, they do so near that radius. Stronger fragmentation, with a lower fragmentation threshold, implies that this radius lies farther away from the star. This would suggest that most discs thus retain and concentrate their grains at specific locations in time-scales compatible with recent observations of structures in young stellar objects.

The researchers have found a way to overcome the planetary formation bottleneck, allowing micrometer-sized dust grains to grow to centimeter-size and above, forming the structures that will eventually be incorporated into planetesimals. The process of going from planetesimal to planet, the researchers argue, has been considered through various mechanisms, but the missing piece has always been the preservation of the original dust grains in the disk long enough for aggregation to occur before their accretion into the star. Here, at least, we have a theoretical mechanism to explain how the grains are preserved and can grow.

The paper is Gonzalez, Laibe & Maddison, “Self-induced dust traps: overcoming planet formation barriers,” Monthly Notices of the Royal Astronomical Society 467 (2) (2017), pp. 1984-1996 (abstract / preprint).

tzf_img_post

{ 11 comments }

The binary system SDSS 1557, about 1000 light years from Earth, was thought to be a single white dwarf star until detailed measurements revealed that the brighter star was being gravitationally influenced by a hither unseen brown dwarf. And that, in turn, has given us an intriguing look at possible planetary formation around both members of a close binary. We’ve found gas giants in such systems, but researchers led by Jay Farihi (University College London) have found signs of rocky debris here that point to the possibility of planets of a much different composition.

“Building rocky planets around two suns is a challenge,” says Farihi, “because the gravity of both stars can push and pull tremendously, preventing bits of rock and dust from sticking together and growing into full-fledged planets. With the discovery of asteroid debris in the SDSS 1557 system, we see clear signatures of rocky planet assembly via large asteroids that formed, helping us understand how rocky exoplanets are made in double star systems.”

FOR-WEB-SDSS-1557-V5c

Image: A disc of rocky debris from a disrupted planetesimal surrounds white dwarf plus brown dwarf binary star. The white dwarf is the burned-out core of a star that was probably similar to the Sun, the brown dwarf is only ~60 times heavier than Jupiter, and the two stars go around each other in only a bit over two hours. Credit: Mark Garlick, UCL, University of Warwick and University of Sheffield.

Can planets, or at least their debris, survive the red giant expansion phase that leads to a white dwarf? Yes, says the new paper on this work, noting that we now have more than three dozen planetary system remnants that have been found through study of circumstellar disks of white dwarfs; we also have several hundred white dwarfs that show signs of accretion of planetary debris.

The debris around SDSS 1557 is spread around the two stars, offering a helpful target for the team’s analysis. Working with observations from the Gemini Observatory South instrument and the European Southern Observatory’s Very Large Telescope, the team found material with high metal content including silicon and magnesium, which could be identified as it was drawn onto the surface of the white dwarf. Such atmospheric pollution has become a tool for the analysis of white dwarf systems. In this case, the UCL team found that 1017 grams of matter — the equivalent of a 4 km asteroid — produced the observed result.

The paper on this work points out that planets of Neptune up to Jupiter size are unlikely to form where they have been found in Kepler detections of circumbinary planets, but are likely the result of migration. However, models exist for smaller planet formation within the snowline, which gives us the possibility of planets like the famous ‘Tatooine,’ from George Lucas’ Star Wars. And work on polluted white dwarfs adds weight to the idea.

From the paper:

The current paradigm of disrupted and accreted asteroids has been unequivocally confirmed by numerous studies, including the recent detection of complex and rapidly evolving photometric transits from debris fragments orbiting near the Roche limit of one star. To date, all polluted white dwarfs with detailed analyses indicate the sources are rocky planetesimals comparable in both mass and composition to large Solar System asteroids, and thus objects that formed within a snow line. These findings unambiguously demonstrate that large planetesimal formation in the terrestrial zone of stars is robust and common.

image002

Dr. Farihi is on record (on his homepage) as saying that he believes we will learn more about extrasolar terrestrial planets using white dwarfs than any other method. The reason: The atmospheres of cool white dwarfs feature hydrogen and helium that can easily become polluted by small amounts of heavy elements. Work like the current paper reminds us that we can use this metal pollution to measure the composition of rocky material around the star.

The debris responsible for white dwarf atmospheric pollution is believed to come from tidally destroyed asteroids whose parent bodies were large and differentiated. Farihi notes that we may be looking at the parent bodies of planetesimals or even fragments of major planets, with compositions similar to material found in our own inner Solar System. He estimates that 20% to 30% of all white dwarfs are orbited by the remains of terrestrial planetary systems.

Image: Dr. Jay Farihi, among some exceedingly interesting standing stones. Credit: Jay Farihi/UCL.

The SDSS 1557 discovery calls for continuing follow-ups, for as co-author Boris Gänsicke (University of Warwick) points out, the signature is transient. Says Gänsicke:

“Any metals we see in the white dwarf will disappear within a few weeks, and sink down into the interior, unless the debris is continuously flowing onto the star. We’ll be looking at SDSS 1557 next with Hubble, to conclusively show the dust is made of rock rather than ice.”

So at SDSS 1557 we have all the markers of a parent body that formed within the snowline, which implies that rocky planet formation in circumbinary orbits within a close double system is feasible. The paper concludes: “These observations therefore support a picture where additional mechanisms can promote planetesimal growth in the terrestrial zones of close binary stars, which are predicted to be substantially wider than in planet forming disks around single stars.”

The paper is Farihi, Parsons & Gänsicke, “A circumbinary debris disk in a polluted white dwarf system,” Nature Astronomy 1 March 2017 (abstract / preprint).

tzf_img_post

{ 12 comments }

A Volcanic View of the Habitable Zone

by Paul Gilster on February 28, 2017

Our understanding of habitable zones is a work in progress, but the detection of multiple planets with potentially water-bearing surfaces around TRAPPIST-1 is heartening. Today we examine the prospect of extending the habitable zone further out from the host star than previously thought possible. The idea is found in new work by Ramses Ramirez and Lisa Kaltenegger (both at the Carl Sagan Institute at Cornell University). Volcanism is the key, allowing interactive effects that pump up greenhouse warming and sustain habitability.

KalteneggerRamirez460

Go back for a moment to the habitable zone limits that Andrew LePage looked at yesterday in his analysis of TRAPPIST-1. The classical habitable zone — allowing liquid water to exist on the surface — has an inner edge at which surface temperatures become high enough to lead to a runaway greenhouse and the rapid loss of water. The outer edge is defined by the distance beyond which CO2 can no longer produce the needed greenhouse effect to keep the surface warm.

Image: Ramses Ramirez, research associate at Cornell’s Carl Sagan Institute, left, and Lisa Kaltenegger, professor of astronomy and director of the Sagan Institute. Credit: Carl Sagan Institute.

But consider, say Ramirez and Kaltenegger, the effect of additional greenhouse gases on these worlds at the outer edge of the HZ. Here’s some context: The warming effect of hydrogen atmospheres has already been considered on young planets, allowing a primordial super-Earth to stay above freezing at the surface out to distances in the range of 10 AU. The paper explains that this greenhouse effect comes from what is known as collision-induced absorption, the result of so-called ‘self-broadening’ when H2 molecules collide.

The problem: Primordial hydrogen in the large amounts needed isn’t sustainable over geological timescales, meaning a super-Earth without a renewable hydrogen source would lose hydrogen to space. But volcanism can be the renewable source needed. The authors point out that climate studies of the early Earth and Mars both show that volcanism could have outpaced the escape of H2. Hydrogen here is not a major atmospheric constituent but is continually replenished by volcanism that offsets H2 loss.

Now we are in a situation where any atmospheric CO2 can interact with hydrogen to increase the greenhouse warming potential for the planet over long time periods. The effect could extend a habitable zone by between 30 and 60 percent. Says Ramirez:

“On frozen planets, any potential life would be buried under layers of ice, which would make it really hard to spot with telescopes. But if the surface is warm enough – thanks to volcanic hydrogen and atmospheric warming – you could have life on the surface, generating a slew of detectable signatures.”

Tavurvur_volcano_edit

Image: The eruption of the Tavurvur volcano in Papua New Guinea, part of the Rabaul Caldera on New Britain. Can similar eruptions produce the factors needed for habitability at the outer edge of the habitable zone? Credit: Taro Taylor edit by Richard Bartz – originally posted to Flickr as End Of Days, CC BY 2.0.

In terms of our own Solar System, the researchers point out that the addition of 30% H2 can extend the habitable zone to 2.4 AU, putting its outer edge in the main asteroid belt (the habitable zone around Sol is normally considered to extend to 1.67 AU, just beyond the orbit of Mars). Because we’ll be looking for atmospheric biosignatures with upcoming instruments like the James Webb Space Telescope and the European Extremely Large Telescope, we’ll want to factor this extended habitable zone into our list of search candidates.

In their paper, which appears in The Astrophysical Journal Letters, the researchers use climate models to compute the boundaries of what they are calling the ‘volcanic hydrogen habitable zone’ for concentrations of hydrogen between 1% and 50% — finding that at a hydrogen concentration at the upper end of that range, the effective stellar flux needed to support the outer edge of the habitable zone decreases by ~35% to 60%, with the corresponding orbital distances to remain habitable increasing by 30% to 60%. The effective temperatures (TEFF of the stars examined range from 2,600K to 10,000K — the stellar classes range from M dwarfs to A-type main sequence stars.

Given these prospects, how do we go about searching for life signatures on outer planets with sizeable amounts of atmospheric hydrogen? It’s a vexing question:

Certain atmospheric spectral features, including N2O and NH3, which can, but do not have to be produced biotically, could be detected in H2 -dominated atmospheres (Seager et al., 2013; Baines et al., 2014). Such volcanic-hydrogen atmospheres may also be able to evolve methane-based photosynthesis (Bains et al., 2014). Distinguishing biosignatures from abiotic sources in such atmospheres will be challenging.

Note the possibilities that must be distinguished here:

NH3 can be formed abiotically through reaction of N2 and H2 in hydrothermal vents on planets with reducing mantles (Kasting et al., 2014). N2O can be formed a number of ways including through atmospheric shock from meteoritic fall-in, lightning, UV radiation (e.g. Ramirez, 2016) and through solar flare interactions with the magnetosphere (Airapetian et al., 2016). Thus, future biosignature studies should focus on modeling biotic and abiotic sources for these gases in thin volcanic-hydrogen atmospheres.

Clearly there is plenty of work ahead, but a combined greenhouse effect from hydrogen, water and CO2 could be the key to expand stellar habitable zones and widen our observational window. As Kaltenegger puts it, “Where we thought you would only find icy wastelands, planets can be nice and warm – as long as volcanoes are in view.” And warming hydrogen, all too easily lost into space, can be renewed by the same kind of volcanic hydrogen that puffs up planetary atmospheres, making that much stronger a signal for the detection of biomarkers.

Does TRAPPIST-1, then, have the capacity for yet another planet in the habitable zone? Kaltenegger isn’t ready to go that far, saying “…uncertainties with the orbit of the outermost Trappist-1 planet ‘h’ mean that we’ll have to wait and see on that one,”

The paper is Ramirez and Kaltenegger, “A Volcanic Hydrogen Habitable Zone,” The Astrophysical Journal Letters 837, No. 1 (2017). Abstract available.

tzf_img_post

{ 62 comments }

The (Potentially) Habitable Worlds of TRAPPIST-1

by Paul Gilster on February 27, 2017

When the news about the seven planets of TRAPPIST-1 broke, I immediately wondered what Andrew LePage’s take on habitability would be. A physicist and writer with numerous online essays and a host of articles in magazines like Scientific American and Sky & Telescope, LePage is also a specialist in the processing and analysis of remote sensing data. He has put this background in data analytics to frequent use in his highly regarded ‘habitable planet reality checks,’ which can be found on his Drew ex Machina site. Having run a thorough analysis of the TRAPPIST-1 situation the other day, Drew now gives us the gist of his findings, which move at least several of the TRAPPIST-1 planets into a potentially interesting category indeed.

By Andrew LePage

Andrew_LePage_2014_small

Like so many other people interested in exoplanets, I made it a point to watch NASA’s press conference live on February 22. Based on the list of participants released by NASA a couple of days earlier, a number of people (myself included) suspected that this was going to be an announcement about new findings of the TRAPPIST-1 planetary system. Back in May of 2016, a team of scientists led by Michaël Gillon (University of Liège – Belgium) had announced the discovery of three Earth-size exoplanets orbiting TRAPPIST-1 – a very small red dwarf star known as an ultracool dwarf named after ESO’s ground-based TRAPPIST (TRAnsiting Planets and PlanetesImals Small Telescope) telescope which had spotted the transits of these exoplanets during an observing campaign in 2015. This star and its system of transiting planets was a natural target for follow up observations by ground and space-based instruments.

As it turned out, NASA’s press conference did involve an announcement of the results of new observations of TRAPPIST-1. A total of 1,333 hours of new photometry including 518 hours of data from NASA’s Spitzer Space Telescope had been acquired since the original discovery paper about TRAPPIST-1 had been submitted by Gillon et al.. Most helpful of all was a virtually uninterrupted 20-day observation run by Spitzer from September 19 to October 10, 2016 which allowed a thorough evaluation of the system. In the end, Gillon et al. had identified the transits of a total of seven exoplanets orbiting TRAPPIST-1 – the largest number of exoplanets found so far orbiting a star. Most exciting of all was the claim that three of these Earth-size exoplanets were potentially habitable.

As my published work over the past couple of decades can testify, I am a long-time believer that the galaxy is filled with habitable planets (and moons!). However, I have also been quite skeptical of frequently dubious claims made by some in recent years that various new exoplanetary discoveries are potentially habitable. Back in May 2016 when Gillon et al. originally announced the discovery of the first three exoplanets found orbiting TRAPPIST-1, the ESO press release and other sources claimed that they were all potentially habitable. My published review of the data available at the time showed no support for this claim: two of the new exoplanets were much more likely to be slightly larger and hotter versions of Venus while the orbit of the third exoplanet was so poorly constrained that nothing meaningful could be said yet about its potential habitability. Naturally I was quite skeptical about this new claim being made by some of the same scientists about TRAPPIST-1. With a copy of the new discovery paper by Gillion et al. in hand along with other peer-reviewed papers on this system published in recent months, I performed a fresh review of the potential habitability of the exoplanets in this system.

eso1706e

Image: This diagram shows the changing brightness of TRAPPIST-1 over a period of 20 days in September and October 2016 as measured by NASA’s Spitzer Space Telescope and various ground instruments. The dips in brightness caused by transiting exoplanets are clearly seen. (ESO/M. Gillon et al.)

Definition of the Habitable Zone

A thorough assessment of the habitability of any extrasolar planet would require a lot of detailed data on the properties of that planet, its atmosphere, its spin state and so on. Unfortunately, at this very early stage, the only information typically available to scientists about extrasolar planets is basic orbit parameters, a rough measure of its size and/or mass and some important properties of its sun. Combined with theoretical extrapolations of the factors that have kept the Earth habitable over billions of years (not to mention why our neighbors are not), the best we can hope to do at this time is to compare the known properties of extrasolar planets to our current understanding of planetary habitability to determine if an extrasolar planet is “potentially habitable”. And by “habitable”, I mean in an Earth-like sense where the surface conditions allow for the existence of liquid water on the planet’s surface – one of the presumed prerequisites for the development of life as we know it. While there may be other worlds that might possess environments that could support life, these would not be Earth-like habitable worlds of the sort being considered here.

One of the important criteria which we can use to determine if a planet is potentially habitable is the amount of energy it receives from its sun known as the effective stellar flux or Seff. According to the work by Ravi Kopparapu (Penn State) and his collaborators on the limits of the habitable zone (HZ) based on detailed climate and geophysical modeling, the outer limit of the HZ is conservatively defined as corresponding to the maximum greenhouse limit of a CO2-rich atmosphere where the addition of any more of this greenhouse gas would not increase a planet’s surface temperature any further. For a star like TRAPPIST-1 with a surface temperature of 2559 K, this conservative outer limit for the HZ as defined by Kopparapu et al. (2013, 2014) has an Seff of 0.22 corresponding to a orbital semimajor axis of 0.048 AU. This Seff value for the outer limit of the HZ is lower than the 0.36 for a planet orbiting a more Sun-like star because ultracool dwarf stars emit so much of their energy in the infrared part of the spectrum where atmospheric absorption is important.

The inner limit of the HZ is conservatively defined by Kopparapu et al. (2013, 2014) by the runaway greenhouse limit where a planet’s temperature would soar even with no CO2 present and lose all of its water in a geologically brief time in the process. For an Earth-size planet orbiting TRAPPIST-1, this happens at an Seff value of 0.91 which corresponds to a distance of 0.024 AU. Once again, this Seff value for the inner edge of the HZ is lower than the 1.11 for a Sun-like star because TRAPPIST-1 radiates so much of its energy in the infrared.

Because of the tight orbits of these exoplanets and the constraints placed on their eccentricity, it is likely that they are synchronous rotators with the same side perpetually facing their sun. Detailed climate modeling over the last two decades now shows that synchronous rotation is probably not the impediment to habitability as it was once thought. In fact, it has been shown that slow or synchronous rotation can actually result in an increase of the Seff for the inner edge of the HZ. According to the recent work by Jun Yang (University of Chicago) and collaborators, the inner edge of the HZ for a slow rotator orbiting a star like TRAPPIST-1 would have an Seff of 1.44 corresponding to an orbital distance of just 0.019 AU.

eso1706m

Image: This diagram shows a comparison of the properties of the newly discovered planets of TRAPPIST-1 with the inner planets of our solar system. (NASA)

The Exoplanets of TRAPPIST-1

The first two exoplanets in this system, TRAPPIST-1b and c, have radii of 1.09 RE (or Earth radii) and 1.06 RE, respectively. While it was claimed back in May 2016 that these two exoplanets were potentially habitable, their Seff values of 4.3 and 2.3 are higher than the 1.9 value for Venus, which is most definitely not a habitable planet. With their Venus-like sizes, Venus-like rotation states and Seff values in excess of Venus’, these are most likely to be non-habitable, Venus-like worlds contrary to the original claims made in May 2016. Fortunately, Gillon et al. have now adopted the more conservative definition of the HZ of Kopparapu et al. (2014, 2014) so this dubious claim was not repeated in the new discovery paper.

As we move outward from the parent star of this system, things begin to become a bit more interesting. What is now designated TRAPPIST-1d has a radius of 0.77 RE which is intermediate between Earth and Mars in size and is therefore likely to be a rocky planet. With an Seff of 1.14, TRAPPIST-1d would seem to be comfortably inside the HZ for a slow rotator as defined by Yang et al.. However, as Gillon et al. mention in their new paper, more recent work by Kopparapu et al. (2016) has shown that Coriolis effects for synchronous rotators with short orbital periods will alter the global circulation pattern in a way which affects cloud formation on the dayside – clouds which help to reflect away much of the energy the planet receives from its sun moderating the surface temperature in the process. With an orbital period (and presumably a period of rotation) of just four days, TRAPPIST-1d is probably rotating too quickly to maintain sufficient cloud cover on its dayside to keep from experiencing a runaway greenhouse effect. While it is certainly worthy of continued detailed study, it would seem that the chances that TRAPPIST-1d is potentially habitable are not very promising and Gillon et al. do not categorize this new find of theirs in that way.

The situation with TRAPPIST-1e is substantially better and it has been identified in the new work by Gillon et al. as being potentially habitable. With an Seff of 0.66, this exoplanet is comfortably inside the conservatively defined HZ of TRAPPIST-1. With a radius of 0.91 RE, it is only slightly smaller than Earth and is not expected to be a volatile-rich mini-Neptune with poor prospects of being habitable. If it were not for the still unresolved issues associated with orbiting so close to an ultracool dwarf and how that affects the volatile inventories of such worlds, TRAPPIST-1e could be considered one of the best candidates currently known for being a potentially habitable exoplanet. Undoubtedly, detailed climate modeling of this exoplanet will help to determine the range of water and other volatile content values which could yield a habitable world much as is being done for our Earth-size neighbor, Proxima Centauri b, as well as the growing list of other potentially habitable red dwarf exoplanets.

The next planet out, TRAPPIST-1f, was also identified as being potentially habitable in the new work by Gillon et al.. Its Seff value of 0.38 is comparable to that of Mars but, since so much of the energy emitted by TRAPPIST-1 is in the infrared, it is still comfortably inside the conservatively defined HZ for this star. While the radius of 1.05 RE would suggest that TRAPPIST-1f is a rocky world like the Earth, other data hint otherwise and raises some possible problems.

Because of the packed nature of this planetary system with its orbits near resonance, it is expected that they would strongly interact with each other gravitationally producing variations in their transit timings. Gillon et al. performed an analysis of these transit timing variations (TTV) derived from all of their photometry data and found them to be on the order of tens of seconds to more than a half an hour – more than sufficient to estimate the masses of the inner six planets. Unfortunately, the uncertainties associated with current TTV-derived mass values are still rather large while the calculated densities (which can be used to help constrain the bulk compositions of these exoplanets) are even more uncertain still. What can be said is that all of these exoplanets are approximately Earth-mass (or ME) objects. The calculated densities with their large uncertainties are also not inconsistent with a rocky composition… the one exception being TRAPPIST-1f.

TRAPPIST-1f has a TTV-derived mass of 0.68±0.18 ME – the most accurately known mass in this system so far. This yields a density that is 0.60±0.17 times that of Earth’s which is suggestive of a volatile-rich bulk composition. It could be that TRAPPIST-1f is a mini-Neptune with a deep hydrogen-rich atmosphere overlaying layers of high temperature/pressure phases of ice rendering it non-habitable. It might also be more of an ocean planet with a CO2-rich atmosphere a few times denser than the Earth’s capping a deep ocean of liquid water. Hubble observations might help to eliminate the former possibility by searching for hydrogen in an extended atmosphere although observations by JWST and other future instruments will be required to begin to explore the latter possibility.

But before too much is read into the apparent low density of this exoplanet, it should be remembered that TTV-derived masses are notorious for changing by rather large amounts as new data become available. NASA’s Kepler spacecraft is currently wrapping up Campaign 12 of its extended K2 mission where it observed a star field which includes TRAPPIST-1. With a virtually continuous photometric data set running from December 15, 2016 to March 4, 2017, it should be possible to calculate more accurate TTV-derived masses in the coming months.

It may turn out that the uncertainties in the mass and density of TRAPPIST-1f have been underestimated and it is actually a denser rocky world like the Earth. But even if the low density of TRAPPIST-1f is confirmed and it is unlikely to be potentially habitable, it nevertheless strongly suggests that small planets orbiting ultracool dwarfs can retain substantial amounts of their water and other volatiles contrary to some of the less optimistic predictions that have been made. This would markedly improve the habitability prospects of many red dwarf planets. For now, TRAPPIST-1f is a reasonable candidate for being potentially habitable – definitely better than TRAPPIST-1d but maybe not as good as e.

eso1706f

Image: This diagram shows the relative sizes of the orbits of the seven planets orbiting TRAPPIST-1. The shaded area shows the extent of the habitable zone (HZ) with alternative boundaries indicated by dashed lines. (ESO/M. Gillon et al.).

The last of their discoveries identified by Gillon et al. as being potentially habitable is TRAPPIST-1g. With a radius of 1.12 RE, it is unlikely to be a mini-Neptune but its currently ill-defined density as well as the fact that the smaller and closer TRAPPIST-1f may be volatile-rich makes it impossible to exclude the possibility. With a Seff of 0.26, TRAPPIST-1g is towards the outer edge but still comfortably inside the HZ for such a cool star. Once again, the claim made by Gillon et al. that this is a potentially habitable exoplanet it a reasonable one given what we currently know about this world. The final planet in this system, TRAPPIST-1h, still has an ill-defined orbit but it seems likely that it is outside of the HZ.

Summary

Contrary to my initial reservations, it does appear that the claim that the TRAPPIST-1 system contains three potentially habitable exoplanets has merit given what we currently know about them. There are obviously unresolved issues about how much of their original volatile inventories these exoplanets have managed to retain despite the higher luminosity of their parent star during its earliest history as well as its subsequent bouts of chromospheric activity like flares not to mention the relatively high flux of X-ray and extreme ultraviolet radiation that have already been observed. While losses of volatiles are expected, it is still not known with any certainty how this will ultimately affect the habitability of these and a growing list of similar red dwarf exoplanets. The fact that the initial TTV analysis of this system implies that TRAPPIST-1f has a volatile-rich bulk composition is a hopeful sign that exoplanets in the HZ of small red dwarfs can retain their volatiles, which improves the habitability prospects of such worlds.

Fortunately, TRAPPIST-1 with its seven transiting, Earth-size exoplanets is an ideal laboratory for exploring the question of how such worlds evolve and whether they can be habitable. New observations from NASA’s Hubble Space Telescope are already working their way through the peer-review process which may help constrain the properties of these exoplanets. We should also expect an analysis of the new Kepler data to provide more information in the next few months on the properties of these exoplanets especially better TTV-derived mass (and density) estimates. It is also possible that additional exoplanets will be found orbiting TRAPPIST-1, although it is unlikely that more will be found in the already tightly packed HZ. The commissioning of NASA’s James Webb Space Telescope and other instruments in the years to come also promises to shed much light on the properties of these exoplanets and their potential habitability. The excitement generated by these new finds is definitely well deserved.

A more detailed discussion of the history of TRAPPIST-1 observations, the properties of its exoplanets and their potential habitability can be found at “Habitable Planet Reality Check: The Seven Planets of TRAPPIST-1” (http://www.drewexmachina.com/2017/02/25/habitable-planet-reality-check-the-seven-planets-of-trappist-1/).

Selected References

Michaël Gillon et al., “Temperate Earth-sized Planets Transiting a Nearby Ultracool Dwarf Star”, Nature, Vol. 533, pp. 221-224, May 12, 2016

Michaël Gillon et al., “Seven temperate terrestrial planets around the nearby ultracool dwarf star TRAPPIST-1”, Nature, Vol 542., pp. 456-460, February 23, 2017 (preprint of paper is available from the ESO at http://www.eso.org/public/archives/releases/sciencepapers/eso1706/eso1706a.pdf)

R.K. Kopparapu et al., “Habitable zones around main-sequence stars: new estimates”, The Astrophysical Journal, Vol. 765, No. 2, Article ID. 131, March 10, 2013

Ravi Kumar Kopparapu et al., “Habitable zones around main-sequence stars: dependence on planetary mass”, The Astrophysical Journal Letters, Vol. 787, No. 2, Article ID. L29, June 1, 2014

Ravi Kumar Kopparapu et al., “The Inner Edge of the Habitable Zone for Synchronously Rotating Planets around Low-mass Stars Using General Circulation Models”, The Astrophysical Journal, Vol. 819, No. 1, Article ID. 84, March 2016

Jun Yang et al., “Strong Dependence of the Inner Edge of the Habitable Zone on Planetary Rotation Rate”, The Astrophysical Journal Letters, Vol. 787, No. 1, Article id. L2, May 2014

tzf_img_post

{ 41 comments }

SPECULOOS: Nearby Red Dwarfs

by Paul Gilster on February 24, 2017

2159_posternormalsize

Let’s turn the clock back a bit on the TRAPPIST-1 discoveries with a reminder of Hubble work on this system announced last July. A team led by Julien de Wit (MIT) used the Hubble Space Telescope’s Wide Field Camera 3 to look for atmospheres on TRAPPIST-1b and 1c, two of the three planets then known around this star. The researchers were able to take advantage of a rare simultaneous transit, when both planets crossed the star within minutes of each other, an event that has been calculated to occur only every two years.

The result: No sign of the kind of hydrogen-dominated atmospheres we would expect on gaseous worlds. That was good news, for reasons that Nikole Lewis (Space Telescope Science Institute) explained:

“The lack of a smothering hydrogen-helium envelope increases the chances for habitability on these planets. If they had a significant hydrogen-helium envelope, there is no chance that either one of them could potentially support life because the dense atmosphere would act like a greenhouse.”

Image: NASA’s latest exoplanet ‘travel poster.’ From the JPL caption: “Some 40 light-years from Earth, a planet called TRAPPIST-1e offers a heart-stopping view: brilliant objects in a red sky, looming like larger and smaller versions of our own moon. But these are no moons. They are other Earth-sized planets in a spectacular planetary system outside our own. These seven rocky worlds huddle around their small, dim, red star, like a family around a campfire.” The poster can be downloaded here. Credit: NASA-JPL/Caltech.

This was, of course, before we knew there were seven planets in this system, but it was clear at the time that future observations would be needed to tell us what kind of atmospheres these worlds had, if any, and what their surface conditions might be. The paper in Nature also noted the need for spectroscopic analysis to look for methane or water features, all part of estimating the depth of any atmospheres on the two worlds.

I hark back to this story because we’re proceeding with exactly the kind of focused work the de Wit team was calling for in the summer of 2016. For it turns out that the discovery of TRAPPIST-1’s first three planets, and the four subsequent ones, was part of a larger project called the Search for habitable Planets EClipsing ULtra-cOOl Stars (SPECULOOS), whose goal is to search for planets in the habitable zones of the nearest 500 ultracool stars and brown dwarfs.

Its acronym created as a nod to a Flemish spiced shortbread, SPECULOOS is in the early stages of its work. At the European Southern Observatory’s Paranal Observatory in Chile, four robotic telescopes make up the observing infrastructure, each of them housing a one-meter primary mirror and cameras sensitive in the near-infrared. The project involves scientists from the University of Liège (Belgium) as well as other universities, and is under the leadership of Michaël Gillon, who has led the TRAPPIST-1 planetary discovery effort.

Thus the TRAPPIST effort (TRAnsiting Planets and PlanetesImals Small Telescopes) is actually folded into the larger SPECULOOS survey, as is a second ESO effort at Oukaïmden Observatory in Morocco. But SPECULOOS is designed to survey ten times as many red dwarfs as TRAPPIST does, and according to this ESO news release, it is expected to discover a number of systems similar to TRAPPIST-1, at least in terms of the number of planets involved, if perhaps not as fortuitously angled to give us seven transits.

Thus the Hubble work of 2016 can be placed within a larger context, the ongoing effort to survey nearby red dwarfs and brown dwarfs and determine which of these are most suitable for studying their atmospheres. By examining the mass, radius and orbital parameters of such worlds and analyzing possible atmospheres, SPECULOOS will feed future observatories like the James Webb Space Telescope and the 39-meter European Extremely Large Telescope with the target list they need.

The excitement of this ‘golden age’ of exoplanet discovery can only build as we realize that these upcoming observatories, along with missions like TESS (Transiting Exoplanet Survey Satellite) and CHEOPS (CHaracterising ExOPlanets Satellite) are not that far in the future (TESS is scheduled for launch in 2018, and CHEOPS should be ready for launch by then). Having made a statistical analysis of the broad exoplanet population with Kepler, we now turn to stars closer to home, and the possibility of finding biomarkers in their atmospheres.

eso1615c_pano

Image: Planets in a compact red dwarf system. Credit: ESO.

In addition to the paper on TRAPPIST-1’s seven planets cited yesterday, I also want to cite the de Wit et al. paper referenced above, “A combined transmission spectrum of the Earth-sized exoplanets TRAPPIST-1 b and c ‘,” Nature 537, (01 September 2016), 69–72 (abstract) and Gillon et al., “Temperate Earth-sized planets transiting a nearby ultramool dwarf star,” Nature 533 (12 May 2016), 221–224 (abstract).

tzf_img_post

{ 23 comments }