by Paul Gilster | Jul 13, 2020 | Deep Sky Astronomy & Telescopes |
I track brown dwarfs closely because they have so much to teach us about the boundary between planet and star. I’m also intrigued by what might be found on a planet orbiting one of these objects, though life seems unlikely. Brown dwarfs begin losing their thermal energy after formation and continue cooling the rest of their lives, a period I’ve seen estimated at only about 10 million years. We know nothing about how long abiogenesis takes — not to mention how common it is — but the outlook for brown dwarf planets and astrobiology seems bleak.
It’s intriguing, though, that we’ve identified a number of brown dwarfs with planetary systems, including 2M1207b, MOA-2007-BLG-192Lb, and 2MASS J044144b, and in the latest news from the NEOWISE mission, we have two brown dwarfs that stand out for other reasons. What used to be the Wide-Field Infrared Survey Explorer would become a tool for the detection of near-Earth objects, but data from the earlier WISE incarnation is still turning up red and brown dwarfs. Along the way, the Backyard Worlds: Planet 9 project, armed with the talents of 150,000 citizen scientists, has more than proven its worth, but more on that in a moment.
Image: This artist’s concept shows a brown dwarf, a ball of gas not massive enough to power itself the way stars do. Despite their name, brown dwarfs would appear magenta or orange-red to the human eye if seen close up. Credit: William Pendrill (CC BY).
The brown dwarfs in question are notable because of their extreme lack of iron. In fact, a typical brown dwarf would have up to 30 times more iron and other metals than we find in either. Low levels of metallicity are something we would expect in ancient exoplanet systems, where supernovae spewing metals were scarce in nearby space, but the mechanisms involved remain problematic. Marc Kuchner is principal innvstigator for Backyard Worlds: Planet 9:
“A central question in the study of brown dwarfs and exoplanets is how much does planet formation depend on the presence of metals like iron and other elements formed by multiple earlier generations of stars. The fact that these brown dwarfs seem to have formed with such low metal abundances suggests that maybe we should be searching harder for ancient, metal-poor exoplanets, or exoplanets orbiting ancient, metal-poor stars.”
Adam Schneider (Arizona State) found one of the brown dwarfs, WISE 1810, back in 2016. Enter Backyard Worlds: Planet 9, which counts among its discoveries more than 1,600 brown dwarfs as well as the oldest known white dwarf, surrounded by a debris disk. Schneider was able to use WiseView, a tool created by Backyard Worlds citizen scientist Dan Caselden, to track the object’s motion, an indication of its relative proximity. The second brown dwarf is WISE 0414, this one discovered by a group of citizen scientists whose names deserve recognition: Paul Beaulieu, Sam Goodman, William Pendrill, Austin Rothermich, and Arttu Sainio.
Image: These images show the newly discovered brown dwarf WISE 1810 as seen with the WiseView tool. The object has an orange hue in these false-color images. In both images, a gray arrow on the left indicates the object’s position in 2010; the black arrow on the right indicates its position in 2016. Credit: Schneider et al. 2020.
The needed follow-up by astronomers using near-infrared spectroscopy confirmed that what the citizen scientists had found by working through hundreds of WISE images were indeed brown dwarfs. At the Jet Propulsion Laboratory, Federico Marocco and Eric Mamajek confirmed WISE 0414 using the Hale Telescope at Palomar Observatory in California. The unusual composition of both objects was apparent, as noted in the paper:
We find that the high proper motion objects WISEA 0414?5854 and WISEA 1810?1010 have exceptionally unusual spectroscopic and photometric properties that likely reflect significantly subsolar metallicities. The best-fitting models for these objects suggest very low metallicities ([Fe/H] ? ?1), though no single model provides a satisfactory fit across all wavelengths. Further astrometric and spectroscopic observations are warranted to better characterize these enigmatic systems.
What caught my eye in this paper is its discussion of what the authors call a “stellar-substellar transition phase.” Metal-poor brown dwarfs — and these are extreme examples — show higher rates of cooling than other dwarfs. Moreover, hydrogen fusion does not stop abruptly as we scale down from star to brown dwarf, but rather, can continue in an interesting way:
…covering a narrow range of masses and large range of effective temperatures over which “unstable fusion” can occur. The masses encompassed by this transition, and the range of temperatures it spans depend on the metallicity and age of the population, with a more pronounced spread expected for metal-poor halo subdwarfs.
Some seven objects meeting this description have previously been found. WISE 1810 and 0414 have the lowest masses and effective temperatures yet discovered in this grouping. The authors point out as well that using proper motion instead of colors to identify cold, low luminosity objects has its advantages, including detecting dwarfs with spectra as unusual as these.
The paper is Schneider et al, “WISEA J041451.67-585456.7 and WISEA J181006.18-101000.5: The First Extreme T-type Subdwarfs?” accepted at the Astrophysical Journal (preprint).
by Paul Gilster | Jul 10, 2020 | Culture and Society |
The pandemic has everyone’s attention, but it’s not too early to ask what lessons might be learned from public response to it. In particular, are there nuggets of insight here into what might occur with another sudden and startling event, the reception of a signal from another civilization? John Traphagan takes a look at the question in today’s essay. Dr. Traphagan is a social anthropologist and Professor of Religious Studies, in the Program in Human Dimensions of Organizations, and Mitsubishi Fellow at the University of Texas at Austin. He also holds a visiting professorship at Waseda University in Tokyo, as well as being a board member of SSoCIA, the Society for Social and Conceptual Issues in Astrobiology. His research focuses on the relationship between science and culture and falls into two streams: life in rural Japan and the culture and ethics of space exploration. John has published numerous scientific papers and several books, including Science, Culture, and the Search for Life on Other Worlds (Springer, 2016). His most recent book, Cosmopolitan Rurality, Depopulation, and Entrepreneurial Ecosystems in 21st Century Japan, was published in 2020 by Cambria Press. This essay is a shorter version of a more detailed paper that is slated to appear in JBIS.
by John W. Traphagan
For people interested in the potential outcome of contact with extraterrestrial life, whether intelligent or otherwise, the Covid-19 pandemic is a timely case-study that can help us think through some of the challenges first Contact with ETI or even simple life might present for humans, because it represents a potential existential threat to the entire population of our planet. And that threat has forced governments into actions with widespread social, political, and economic implications up to world-wide depression.
Like the emergence of Covid-19, first contact, in particular, has the potential to set in motion political machinations on the part of nation-states as national security interests are identified. If resources or information associated with contact are considered important to control by governments (see our earlier article On SETI, International Law, and Realpolitik in Centauri Dreams), then unexpected events which threaten global political and economic stability, regardless of the risks associated with contact itself may unfold. Indeed, this has been one of the outcomes of the Covid-19 pandemic in which there was early concern about the potential impact of policy responses to the pandemic and the associated collapse in oil prices. This could easily have led to political instability in already unstable areas of the world such as parts of the Middle East.
In general, successful human response to a pandemic (such as Covid-19) is based on a combination of credible action by governments, strong leadership from international organizations such as WHO, and responsible behavior by nation-states concerned with the well-being of their populations. The same factors apply to contact with extraterrestrial life. In the event of an encounter with life from another world, public safety and health (including mental health) depend on: 1) timely and credible actions by governments where contact is made; 2) clear direction and leadership from international organizations and the scientific community to coordinate a global response; and 3) responsible behavior on the part of governments naturally concerned with protecting parochial national interests.
In the case of non-intelligent extraterrestrial life, such as microbial life, the parallels with the Coronavirus pandemic are obvious, but are still complicated by the fact that we do not know how introduction of an alien microorganism into Earth’s ecosystem would affect life on Earth. But contact with any form of extraterrestrial life presents risks that have the potential to place our species in a position similar to what we are currently facing with Covid-19, which represents a global threat necessitating a global response.
So, what can we learn from the pandemic? There are at least four tactical points to take away from our current situation:
1. Differential values play a significant role in how governments respond to the pandemic, despite the fact that Covid-19 represents a global threat to human life.
2. Each nation-state is largely going it alone in assessing the level of threat and developing appropriate responses to the pandemic based on risk assessments.
3. There has been limited cooperation and some governments have withdrawn from the international political environment or even tried to thwart international organizations such as WHO.
4. Responses to government rules such as wearing masks in public have varied and in some cases been resisted.
The key point to take away from the Covid-19 pandemic for those interested in the potential risks and influences of contact with ETI is that different responses and policies are products of cultural, ideological, and political variations among and within nations of the world. Factors such as population density and socio-economic status also play a significant role in how the virus has spread and how governments and individuals have responded. And structural patterns of social and political life—such as the presence of systemic racism in the US—clearly shape how different people are affected by the pandemic. There is no reason to think contact with ETI would be different.
Culture matters. There are at least three strategic lessons we can draw from this observation:
• The world is unlikely to react as one. Even if it is determined that ETI poses an existential threat to humanity a well-coordinated and unified response to either physical or remote contact with ETI is unlikely, unless significant changes in human political behavior occur.
• Culture will drive state and sub-state response. Cultural variation evident in complex and conflicting value systems will influence nation-states and other groups as they interpret and respond to contact.
• Diversity of perspective, a significant advantage in assessing options, can be a hindrance to unified action. Diverse cultural, political, and economic characteristics that humans display and experience have the potential not only to provide multiple options in responding to contact, but may work against a successful response.
We should be concerned. In the face of potential existential threat, unified and coordinated action is central to successful results—thousands of years of experience with warfare have shown this clearly to be the case. Unless we prepare for the fact of diversity in human responses to contact, rather than being a source of strength and options when facing contact that diversity may work against a coordinated effort.
It would help for the SETI scientific community to move away from the often tacit assumption that humans live and operate within a single, unified (or monolithic) civilization to a concept of both our world and potential other worlds that expects diversity in cultures, interpretations, and likely responses to a contact scenario. Recognition of the potential for contact to stimulate increased conflict and disagreement among human groups—again as is evident in the Coronavirus pandemic—rather than to unify humanity in response to a real or perceived global threat, would represent a good starting point for thinking about protocols for contact.
by Paul Gilster | Jul 9, 2020 | Exoplanetary Science |
I hadn’t planned to write about the recent work out of the University of Exeter on Beta Pictoris, but yesterday’s article on KELT-9b dealt with planetary alignment, given that the planet shows marked spin-orbit misalignment. At Beta Pictoris, an international team of researchers led by Exeter’s Stefan Kraus has carried out measurements of the spin-orbit alignment of Beta Pictoris b, a gas giant orbiting a young star in an orbit about as distant as Saturn from the Sun. Here we have the first spin-orbit alignment measurement of a directly imaged planetary system.
How such alignments occur is clearly relevant to planet formation theories. There’s a bit of astronomy history here, for spin-orbit issues became significant for both Immanuel Kant (1724-1804) and Pierre-Simon Laplace (1749-1827), who looked at spin-orbit alignment in our own Solar System. It was apparent to both that the planets known to them orbited the Sun not only in alignment with each other but in alignment with the Sun’s axis as well. Hence the idea that the entire system formed from a rotating planetary disc, and a flattened one at that.
Other planetary systems may follow different paths of development, as Kraus notes:
“It was a major surprise when it was found that more than a third of all close-in exoplanets orbit their host star on orbits that are misaligned with respect to the stellar equator. A few exoplanets were even found to orbit in the opposite direction than the rotation direction of the star. These observations challenge the perception of planet formation as a neat and well-ordered process taking place in a geometrically thin and co-planar disc.”
Which is to say that close-in exoplanets can depart markedly from the apparent norm, making the study of these hot Jupiters significant for initial formation scenarios. Kraus and company went to work with the GRAVITY instrument at the Very Large Telescope Interferometer (VLTI) in Chile, exploiting the fact that a star’s spectral lines show a spatial displacement — an exceedingly small one, to be sure — caused by gas absorption in the star’s atmosphere. The team used this effect to determine the orientation of the star’s rotation axis.
Image: The new observations show that the stellar equator (right) is aligned with the orbital plane of the planet Beta Pictoris b (middle) and the plane of the extended disc of debris material that surrounds the system (left). Credit: ESO/A.M. Lagrange; ESO/A.M. Lagrange/SPHERE consortium.
At Beta Pictoris, some 63 light years from Earth, a displacement about 1/100th the apparent diameter of the star itself is used to demonstrate that planet and star are as well-aligned as our own Solar System. Thus the classic model of planet formation seems to apply, with implications for the hot Jupiters we see that demonstrate marked spin-orbit misalignment. From the paper (internal references removed for brevity):
Our finding of spin-orbit alignment for ? Pic b suggests that this planet formed in a coplanar disks without primordial misalignments. This is in contrast to theories that describe the occurence of obliquities as a natural by-product of the star formation process, for instance through turbulent motions in the star-forming cloud and fluid-dynamical effects during disk formation. In case our finding of a well-aligned system is representative for wide-separation planets, it would suggest that the population of Hot Jupiters on oblique orbits (found in RM survey at orbit separations between ? 0.02 and 0.3 au) are likely transferred to oblique orbits through dynamical processes post-formation. Possible mechanisms include planet-planet scattering, stellar flybys, or the Kozai-Lidov mechanism, where a wide companion orbiting a close binary on a highly inclined orbit can induce oscillations in inclination/eccentricity of the close pair.
Image: To derive the stellar rotation axis of Beta Pictoris the team used the unique high angular and high spectral resolution mode of VLTI/GRAVITY to measure shifts in the centroid position in the hydrogen Brackett-gamma absorption line on micro-arcsecond scales. In the blue-shifted part of the absorption line, the centroid of the emission is displaced to the North-East, which indicates that the South-Western hemisphere of the star is approaching the observer. Credit: Kraus et al. / University of Exeter.
Much depends on just how representative Beta Pictoris b really is of gas giants with wide separation from their star. The authors propose a new high-spectral resolution interferometric instrument at the VLTI to measure the spin-orbit alignment of hundreds of gas giants, dramatically increasing the data on long-period planets. Kraus is involved in a proposed VLTI
visitor instrument called BIFROST that could enable such an observing campaign. This, in turn, should stoke the discussion of planet formation and system evolution when it comes to architectures as extreme as the one we see at KELT-9.
The paper is Kraus et al., “Spin-Orbit Alignment of the ? Pictoris Planetary System,” Astrophysical Journal Letters, Vol. 897, No. 1 (29 June 2020). Abstract / Preprint.
by Paul Gilster | Jul 8, 2020 | Outer Solar System |
If all goes well (an often perilous assumption, as JWST so frequently reminds us), NASA’s Psyche mission to the intriguing asteroid of the same name will lift off in about two years. We’re now moving out of the design and planning stage into manufacturing the spacecraft hardware, this following a period of testing on the core engineering models that will deliver the spacecraft to its target in the main asteroid belt. The critical design review, a shakeout of the three science instruments and engineering subsystems, has just been passed with flying colors.
Principal investigator Lindy Elkins-Tanton (Arizona State University) calls the process “one of the most intense reviews a mission goes through in its entire life cycle.” True enough, as everything from telecommunications, power and propulsion must pass the test, not to mention the flight avionics and computing systems. We’re a long way past the digital blueprint stage, having followed it up with prototypes and engineering models of the science instruments and engineering subsystems, all performed before the flight hardware could be built.
“This is planning on steroids” said Elkins-Tanton. “And it includes trying to understand down to seven or eight levels of detail exactly how everything on the spacecraft has to work together to ensure we can measure our science, gather our data and send all the data back to Earth. The complexity is mind-boggling.”
So what’s next? Assembling and testing of the full spacecraft is to begin in February of 2021, with a deadline of April 2021 for each instrument to be delivered to the main clean room at the Jet Propulsion Laboratory. This is going to be a fascinating mission to watch from the technology standpoint, as it will involve a demonstration of the Deep Space Optical Communications system (DSOC), intended to improve communications performance by 10 to 100 times without corresponding increases in mass, volume or power.
We’re going to want to follow DSOC closely because of its deep space implications. The plan is to deploy advanced lasers in the near infrared, and a look through NASA materials on the project shows three technologies — a low-mass spacecraft pointing assembly; a flight laser transmitter; and a pair of photon-counting detector arrays — being integrated into the DSOC system, communicating with a ground-based receiver to enable efficient communications. All this by way of exploring a future that will one day demand high-definition imagery, live video feeds and real-time data transmission for long-duration missions to deep space.
So while it’s a demonstrator, DSOC is an important one, and the Psyche mission offers a test of the system’s ability to cull faint laser signals out of a noisy background. Beyond DSOC, engineers at Maxar Technologies in Palo Alto (CA) are building the main body of the spacecraft (the Solar Electric Propulsion Chassis), attaching propulsion tanks enroute to delivery early next year to JPL, followed not long after by the solar arrays critical to power the spacecraft’s systems.
The avionics subsystem is being built at JPL, where Psyche Project Manager Henry Stone notes:
“One of the things we pride ourselves on in these deep-space missions is the reliability of the hardware. The integrated system is so sophisticated that comprehensive testing is critical. You do robustness tests, stress tests, as much testing as you can – over and above. You want to expose and correct every problem and bug now. Because after launch, you cannot go fix the hardware.”
Imagine having a job where you can talk about your involvement in multiple deep space missions, the kind of thing that makes me wish for a quick rejuvenation and a new career doing exactly that at places like JPL. And then to watch the mission fly… Psyche is to launch in August of 2022, with a Mars gravity assist in May of 2023 and arrival at Psyche in 2026.
Image: This artist’s concept, updated as of June 2020, depicts NASA’s Psyche spacecraft. Set to launch in August 2022, the Psyche mission will explore a metal-rich asteroid of the same name that lies in the main asteroid belt between Mars and Jupiter. The spacecraft will arrive in early 2026 and orbit the asteroid for nearly two years to investigate its composition. Credit: NASA/JPL-Caltech/ASU/Peter Rubin.
What an interesting destination we’re dealing with. Psyche is made up mostly of iron and nickel, making it much like Earth’s core, so we may be looking at the stripped core of a differentiated planetesimal, unless the asteroid formed as a body rich in iron. If its mantle was stripped away, when did that occur, and how? Exactly how will this asteroid compare to known stony, icy objects we’ve visited? We can’t see planetary cores, but Psyche may give us a look into a planetesimal core from the era of collisions and accretion that produced the terrestrial planets.
The spacecraft will fly with a magnetometer to measure the asteroid’s magnetic field, along with a multispectral imager to collect images and data about the object’s composition and topography. Spectrometers will analyze the surface to determine its chemical abundances. The propulsion system is an electric hall thruster using xenon as the propellant. ATLO is next — Assembly, Test and Launch Operations — all beginning in February of next year. Love those NASA acronyms!
by Paul Gilster | Jul 7, 2020 | Exoplanetary Science |
Perhaps the hottest planet ever discovered spotlights yet another way to interpret light curves produced by transiting worlds. KELT-9b comes out of data gathered by the KELT transit survey, the acronym standing for Kilodegree Extremely Little Telescope. KELT consists of two robotic telescopes, one at Winer Observatory in southeastern Arizona, the other at the South African Astronomical Observatory in Sutherland, South Africa. The planet orbits an A-class star in Cygnus about 670 light years away and turned up in the KELT data in 2017.
We’ve learned a lot more about KELT-9b thanks to the TESS mission, allowing us to understand just how unusual this planet is. 2.9 times as massive as Jupiter, the world orbits its star in 36 hours, receiving 44,000 times the energy from its host that Earth receives from the Sun. Reaching 4,300 degrees Celsius, this is a tidally locked planet whose dayside is hotter than the surfaces of some stars. Its orbital path takes it almost directly above both the star’s poles.
But this mix gets even more intriguing. The primary, KELT-9, is roughly twice the size of the Sun, 56 percent hotter, and spins 38 times as fast. That makes for a complete stellar rotation in 16 hours. As you would imagine, the rapid spin causes the star to deform, flattening at the poles and broadening at the equator. As a result, we run into the phenomenon known as gravity darkening — the poles brighten as the equatorial region cools and dims by comparison.
We get a temperature differential of almost 800 degrees Celsius. The effects on the transit light curve are interesting. Beginning near the star’s poles, the transit blocks less light as KELT-9b travels over the stellar equator. We have an asymmetry here we can work with to gain information about the temperature and brightness changes over the surface of the star, learning more about its shape and orientation.
Jason Barnes (University of Idaho) is a co-author of the paper on this work:
“Of the planetary systems that we’ve studied via gravity darkening, the effects on KELT-9 b are by far the most spectacular. This work goes a long way toward unifying gravity darkening with other techniques that measure planetary alignment, which in the end we hope will tease out secrets about the formation and evolutionary history of planets around high-mass stars.”
Image: Observations from NASA’s Transiting Exoplanet Survey Satellite (TESS) have revealed new details about KELT-9b’s environment. The planet follows a close, polar orbit around a squashed star with different surface temperatures, factors that make peculiar seasons for KELT-9b. The planet’s transits begin near one of the star’s hot, bright poles and progress toward the cooler, dimmer equator. Credit: NASA’s Goddard Space Flight Center.
Depending on which part of the star is being referenced, the phenomenon behind gravity darkening is sometimes called gravity brightening, reflecting the fact that the oblate shape of such a rapidly spinning star causes higher surface gravity at the poles, producing higher temperature and brightness; by contrast, the equator is darker. Because of the temperature differential on the surface of the star, KELT-9b experiences an unusual kind of seasonality, hotter over the poles, colder over the star’s equator. A kind of summer, a kind of winter, with each season lasting nine hours, only to repeat during the brief year.
A planet like this is going to be useful for research into hot Jupiters. There is a clear trend among such worlds in that they are often spin-orbit misaligned. The paper continues:
“Its high dayside temperature provides excellent opportunities for phase curve and secondary eclipse analyses (Hooton et al. 2018; Wong et al. 2019; Mansfield et al. 2020). The high signal-to-noise ratio of its transit makes KELT-9 b a top target for transmission spectroscopy (Hoeijmakers et al. 2018, 2019; Cauley et al. 2019). In this work, we model KELT-9 b’s Transiting Exoplanet Survey Satellite (TESS) light curve including rapid stellar rotation to measure the hot Jupiter’s transit parameters, and we take advantage of the transit asymmetry caused by gravity darkening to robustly constrain the planet’s orbital geometry including its true spin–orbit orientation.
Thus this paper is unusual in being one of the few that deal with gravity darkening in analyzing an exoplanet lightcurve. Using it, the authors measure the planet’s alignment angle and discuss the effects of gravity darkening on the hot Jupiter’s atmospheric processes. In the figure below, the effects of gravity darkening are apparent in the transit.
Image: This is Figure 2 from the paper. Caption: (Left) KELT-9 b begins its transit near the star’s hot pole and moves toward the star’s cooler equator. Our transit analysis directly measures the stellar inclination ( i ), the planet’s projected alignment (?), and the orbital inclination (i.e., the impact parameter b). We find that KELT-9 varies in effective temperature by ?800 K between its hot poles and cooler equator. (Right) KELT-9 b’s phase-folded primary transit from TESS. The transit depth steadily decreases throughout the eclipse, indicating that KELT-9 b begins its transit near one of the host star’s hotter poles and moves toward the dimmer stellar equator. Credit: Ahlers et al.
Models of rapidly rotating stars are still being developed, but will be needed to analyze the high number of such stars expected to be discovered by TESS. In fact, I was surprised to learn that in a previous paper, lead author John Ahlers (NASA GSFC) had estimated on the order of 2,000 exoplanets will turn up orbiting A/F stars in the TESS data, and the expectation is that a large number of these will be spin-orbit misaligned. Thus KELT-9b gives us a window into fast rotators, which are expected to comprise a large number of the A/F systems discovered.
The paper is Ahlers et al., “KELT-9 b’s Asymmetric TESS Transit Caused by Rapid Stellar Rotation and Spin–Orbit Misalignment,” The Astronomical Journal Vol. 160, No. 1 (5 June 2020). Abstract.
