Wednesday, May 31, 2017

The Small Mars Problem

Figure 1. All planets and dwarf planets orbiting within 6 astronomical units (AU) of our Sun, shown at their relative diameters.

From afar, our Solar System looks regular and well-organized. At its center is a large, massive sphere of incandescent gases (the Sun) surrounded by eight smaller and less massive spheres of heavier elements (the planets) distributed in concentric orbits out to a distance of about 4.5 billion km/2.8 billion miles.

The orbital distribution of the eight planets also seems regular, at least at first glance. Smaller, rocky worlds are confined to the inner system, while larger, gaseous worlds dominate the outer system. Planet sizes follow a curve, rising from the inner to the middle planets and then declining again from the middle to the outer planets.

In more specific terms, mass and radius increase along with distance among the three planets closest to the Sun (Mercury through Earth). Both parameters peak at the orbit of the fifth planet, Jupiter, which is almost a dozen times the radius and more than 300 times the mass of Earth. Then, from Jupiter through Uranus, the seventh planet, both mass and radius decline substantially along with distance from the Sun.

But this orderly progression of planet sizes has two notable interruptions: Mars and Neptune. If the distribution of planets were truly regular, Mars would be larger and more massive than Earth, and Neptune would be smaller and less massive than Uranus. Instead, the Red Planet has only 53% of Earth’s radius (0.53 Rea) and 11% of its mass (0.11 Mea), while the Azure Planet, at 17.2 Mea and 3.9 Rea, has about 98% of the radius of Uranus but 119% of its mass.

How did that happen?

In the present post I’m going to ignore the oddity of Neptune and concentrate on the Martian half of the question. My rationale is that Mars occupies our system’s classical habitable zone, and therefore – along with Earth and Venus – plays a critical role in theories of the habitability of extrasolar planets. If mass had been more uniformly distributed in the inner Solar System, Mars would be more massive than it is. If its mass were in the range of 1 to 2 Mea, Mars would likely be able to sustain a magnetic field, plate tectonics, surface water, and long-term habitability. Therefore, if we want to understand the potential system architectures that might support life-bearing planets, we need to understand why Mars is so small.

Figures 1 and 2 highlight the Small Mars Problem and the Great Martian Gap, which is the name I just invented for the general depletion of mass between Earth and Jupiter. The planet Mars and the dwarf planet Ceres orbit within this gap at 1.52 AU and 2.77 AU, respectively. With a little more than 1% of the mass of our Moon, Ceres accounts for fully one-third of all mass in the Asteroid Belt, which is concentrated between 2.2 and 3.3 AU (the latter boundary provided by the 2:1 resonance with Jupiter's orbit; Jewitt et al. 2009). The entire region between the orbits of Earth and Jupiter contains less than 0.12 Mea, with little Mars accounting for 99% of the total. By contrast, the region extending inward from Earth’s orbit to the Sun contains 1.87 Mea, yet Earth, the most massive object, accounts for only 53% of the total.

Figure 2. The Great Martian Gap

Blue numbers along the bottom refer to astronomical units (AU), where the Earth/Sun separation = 1. Planets are shown at their relative sizes and relative distances from the Sun, with separate scales for radius and distance. As astronomers have long noted, mass is severely depleted between the orbit of Jupiter at 5.2 AU and the orbit of Earth at 1 AU (see Weidenschilling 1977).

zigzag migration

Recent studies by Konstantin Batygin & Greg Laughlin (2015) and by Sean Raymond & colleagues (2016) have presented conflicting scenarios to explain the Small Mars Problem and the Great Martian Gap. Both involve zigzag migratory paths for Jupiter during the primordial phase of system evolution.

Batygin & Laughlin based their approach on earlier models by Kevin Walsh & colleagues (2011) and Pierens & Raymond (2011), in which Jupiter formed in the outer Solar System (somewhere beyond 3 AU) and then migrated first inward and then outward again. The popular name for this scenario (blogged here and here) is the Grand Tack. According to Batygin & Laughlin, these maneuvers not only swept most solid mass out of the region exterior to Earth’s present orbit, but also created an instability that emptied the region interior to 0.7 AU.

Raymond & colleagues took a very different approach based on the “inside out” model of planet formation presented by Chatterjee & Tan (2014). Contrary to his own earlier work, Raymond’s group proposed that Jupiter formed in the inner Solar System near the Sun, and then migrated first outward, then inward, and finally outward again, depleting the region inward of Venus and wreaking havoc beyond Earth.

sweeping secular resonances

While the Grand Tack has been more widely discussed and endorsed than the inside-out scenario, both explanations have been faulted. Now Benjamin Bromley & Scott Kenyon (2017) present an alternative approach in which “sweeping secular resonances” with Jupiter’s orbital motion, rather than any migratory scenario, become the mechanism for clearing the Great Martian Gap. Their model implies a less dramatic but equally consequential role for Jupiter, and I suspect that it can be extended to explain similar gaps observed in the architecture of multiplanet systems around other stars.

To develop their model, Bromley & Kenyon (hereafter BK17) conducted extensive numerical simulations based on earlier work by and with their collaborators Makiko Nagasawa and Edward Thommes (Nagasawa et al. 2007, Thommes et al. 2008). They also note recent work on the same problem by Xiaochen Zheng & colleagues (2017).

BK17 begin with the familiar theoretical construct of the Minimum Mass Solar Nebula (blogged here). They assume that a dusty gas nebula (generally known as a protoplanetary disk) is present at the outset of their simulations. Jupiter is fully formed at its current semimajor axis of 5.2 AU (Figure 2), having cleared a gap in the disk for 1 AU on either side of its orbital path. A swarm of planetesimals orbits inward of this gap, while Saturn orbits well beyond it. Both gas giants exert gravitational effects on their surroundings, and the disk itself has gravity. In addition, the orbit of Jupiter is slightly eccentric, but probably less so than its present value of 0.05. BK17 assume an eccentricity of 0.03 in their simulations.

The key factor in their approach is the n5 resonance (“nu-5,” Greek letter nu with superscript 5), a “secular” or “very long-term” resonance between the motion of the protoplanetary disk and Jupiter’s orbital period. BK17 define the nu-5 resonance as the location “where the local apsidal precession rate matches Jupiter’s rate of precession,” and note that a planetesimal or protoplanet at this location will be perturbed by Jupiter’s gravitational influence onto a highly eccentric orbit. The likely result will then be either collision with another planet or protoplanet, engulfment by the Sun, or ejection from the Solar System.

In the early Solar System, when the gas disk was still present, the nu-5 resonance was located in the vicinity of the present Asteroid Belt (Zheng et al. 2012). As the gas dissipated, the resonance moved inward, destabilizing (“shaking up”) the orbits of protoplanets and planetesimals and effectively clearing out a substantial mass in solids. After the gas was completely depleted, the nu-5 resonance reached its present position inside the orbit of Venus. This sweeping shake-up created the Great Martian Gap while leaving behind enough mass to build Earth and Venus, as well as their two by-blows, Mercury and Mars.

BK17 discovered that several different factors were critical to reproducing the mass of Mars and the present-day Asteroid Belt within the time constraints provided by the known age of Mars. These include the mass of the perturbing planet, its distance from the system habitable zone, and the timing and speed of the sweeping secular resonance generated by its orbital motion.

Regarding mass, BK17 find that only a “Jupiter-mass planet” can produce the magnitude of perturbation required to induce a shake-up in the protoplanetary disk of a Sun-like star. Unfortunately, they don’t provide a precise value for the necessary mass – for example, would an object of Saturn’s mass (95 Mea) be sufficient? They also note that a “super-Earth” would be massive enough to produce sweeping secular resonances in an M dwarf system, likely referring to an object in the range of 1-10 Mea (see, e.g., Kenyon & Bromley 2009).

Regarding orbital location, they find that the masses of Earth and Mars depend sensitively on the semimajor axis of Jupiter at the time of the sweeping resonance. If Jupiter had been substantially farther from the Sun, the resonance would never have reached the orbit of Mars, and Mars would have grown much bigger than it actually did – presumably massive enough to support a habitable environment. But if Jupiter had been substantially closer to the Sun, and thus closer to the system habitable zone, the resonance would have inhibited the formation of Earth in the same way that it stunted the growth of Mars when Jupiter was at 5.2 AU. Instead of one living planet, our system would have none at all.

Regarding the timing of the sweeping secular resonance, BK17 note that its schedule is determined by the lifetime of the protoplanetary disk. As we saw in an earlier post, the system age when gas dissipation commences can fall anywhere between 1 and 10 million years. At the early end of that range, according to BK17, dissipation accompanied by shake-up would have extremely negative consequences for rocky planet formation, as it would destroy planetesimals before they had time to accrete into protoplanets. At the latter end, however, the effects would be modest, since accretion would already be well advanced, potentially permitting the growth of Earth-size planets out to a distance of 3 AU. In the case of our Solar System, we can assume that the shake-up happened before a system age of about 4 million years, given radiometric evidence that Mars was fully formed by then.

The rate of disk dispersal also matters. Although many studies have found that gas dissipation happens rapidly, requiring less than half a million years from start to finish (Williams & Cieza 2011), variation is inevitable: some disks take longer than others to disperse. BK17 find that the relative speed of dissipation strongly affects the outcomes of secular resonance sweeping. If the gas dissipates quickly, the resonance sweeps inward at the same rate, resulting in minimal disruption of the planetesimal population. If the gas dissipates more slowly, the resonance becomes increasingly more destructive, clearing larger and larger quantities of solid mass from the system.

Figure 3. Calaveras street sweepers on the Day of the Dead
From a print by José Guadalupe Posada (1852-1913)

extrasolar asteroids and orbital gaps

Although BK17 are interested primarily in the evolution of our Solar System, they attempt to generalize some of their results to extrasolar locales. Their chief concern is the occurrence of extrasolar analogs of the Asteroid Belt. They argue that most systems with a gas giant in Jupiter’s approximate location (i.e., just outside the system ice line, where accretion is maximized) will experience a sweeping secular resonance whose outcome will be a ring of rocky debris in the inner system. While they concede that few such structures have been discovered to date (HD 69830 is most familiar), they attribute these limited findings to the difficulty of discerning modest aggregations of warm debris even around nearby stars. In the future, they predict, more sensitive searches will be more successful.

I suggest that the implications of their model are much broader than their relevance to extrasolar asteroid belts, and far more dispiriting. If sweeping secular resonances are common in systems with cool gas giants, then the outlook for habitable planets is even less promising than I thought. Here’s why.

An important focus of this blog is the possibility of Solar System analogs – that is, exoplanetary systems containing cool giants whose orbital parameters would permit the survival of Earth-mass planets (0.5-2 Mea) in the local habitable zone. (For recent posts on this topic, see here and here.) My January search of the Extrasolar Planets Encyclopaedia identified 17 such systems located within 60 parsecs/196 light years. All center on Sun-like stars in the range of 0.85-1.15 Solar masses, so their habitable zones have boundaries similar to those proposed for our own system (0.99-1.70 AU; Kopparapu et al. 2013).

Among the Jupiter analogs in these systems, semimajor axes range from 3 AU to 5.2 AU, and more than half orbit inside 4 AU. According to the findings of BK17, virtually all these systems will have experienced a sweeping secular resonance very similar to the one they propose for the Solar System. Because all but one of the 17 confirmed Jupiter analogs orbits closer to the local habitable zone than does our own Jupiter, the depletion of mass in this favored region is likely to be even more extreme than it was at home. Therefore, habitable planets appear to be less likely in the existing sample of Solar System analogs than they are in the Solar System.

To put it another way: BK17 have just shown that gas giant planets are even more unfriendly to the formation and survival of habitable planets than we already suspected. It’s not enough for the giant to reside outside the system ice line in a configuration that permits an Earth-like planet to maintain an Earth-like orbit. The giant must also be distant enough from the central star that the sweeping secular resonance generated by its orbit was insufficient to clear solid mass from the local habitable zone. Even Jupiter managed to evacuate mass from more than half of the radial extent of our own habitable zone, drastically reducing our system’s potential to produce life-bearing planets. Now it looks like extrasolar Jupiters might be still more likely to foreclose the possibility of life around other stars.

Batygin K, Laughlin G. (2015) Jupiter’s decisive role in the inner Solar System’s early evolution. Proceedings of the National Academy of Sciences 112, 4214-4217. Abstract: 2015PNAS..112.4214B
Bromley BC, Kenyon SJ. (2017) Terrestrial planet formation: Dynamical shake-up and the low mass of Mars. Astronomical Journal 153, 216. Abstract: 2017AJ....153..216B
Chatterjee S, Tan JC. (2014) Inside-out planet formation. Astrophysical Journal 780, 53.
Jewitt D, Moro-Martín A, Lacerda P. (2009) The Kuiper Belt and Other Debris Disks. In Astrophysics in the Next Decade, edited by Harley A. Thronson, Massimo Stiavelli, Alexander Tielens. Springer. Abstract: 2009ASSP...10...53J
Kopparapu R, Ramirez RM, Kasting JF, Eymet V, Robinson TD, Mahadevan S, Terrien RC, Domagal-Goldman S, Meadows V, Deshpande R. (2013) Habitable zones around main-sequence stars: New estimates. Astrophysical Journal 65, 131.
Kenyon SJ, Bromley BC. (2009) Rapid formation of icy super-Earths and the cores of gas giant planets. Astrophysical Journal 690, L140-L143.
Nagasawa M, Thommes EW, Kenyon SJ, Bromley BC, Lin DNC. (2007) The diverse origins of terrestrial-planet systems. In Protostars and Planets V, edited by B. Reipurth, D. Jewitt, K. Keil. University of Arizona Press, pages 639-654. Abstract: 2007prpl.conf..639N
Pierens A, Raymond SN. (2011) Two phase, inward-then-outward migration of Jupiter and Saturn in the gaseous solar nebula. Astronomy & Astrophysics 533, A131. Abstract: 2011A&A...533A.131P
Raymond SN, Izidoro A, Bitsch B, Jacobson SA. (2016) Did Jupiter’s core form in the innermost parts of the Sun’s protoplanetary disk? Monthly Notices of the Royal Astronomical Society 458, 2962-2972. Abstract: 2016MNRAS.458.2962R
Thommes E, Nagasawa M, Lin DNC. (2008) Dynamical shake-up of planetary systems. II. N-body simulations of Solar System terrestrial planet formation induced by secular resonance sweeping. Astrophysical Journal 676, 728-739. Abstract: 2008ApJ...676..728T
Weidenschilling JS. (1977) The distribution of mass in the planetary system and solar nebula. Astrophysics and Space Science 51, 153-158.
Williams JP, Cieza LC. (2011) Protoplanetary disks and their evolution. Annual Review of Astronomy and Astrophysics 49, 67-117. Abstract: 2011ARA&A..49...67W
Zheng X, Lin DNC, Kouwenhoven MBN. (2017) Planetesimal clearing and size-dependent asteroid retention by secular resonance sweeping during the depletion of the Solar Nebula. Astrophysical Journal 836, 207.

Wednesday, May 3, 2017

TRAPPIST-1 and Kepler-11: Revised Masses

Figure 1. Revised masses and radii for the seven planets of TRAPPIST-1, as estimated by Wang & colleagues (2017). Results from Gillon & colleagues (2017) are shown for comparison. Image source: Figure 5 of Wang et al. 2017, with new labels.

A few months ago, Michaël Gillon & colleagues reported a remarkable seven-planet architecture for a nearby ultra-cool red dwarf, TRAPPIST-1. In their analysis, six out of the seven transiting planets in this tightly packed system have densities in the range of Earth, Venus, and Mars – and no fewer than three occupy the system habitable zone. Those findings were based in part on a 20-day campaign of nearly continuous observation by the Spitzer Space Telescope.

Now Songhu Wang & colleagues have presented a rather different picture of the TRAPPIST-1 family, based on more than 70 days of monitoring by the Kepler Space Telescope during the K2 Mission. Even though Kepler’s current precision is inferior to that of Spitzer, the availability of data covering a much longer period of time still permits a more robust characterization of these planets than was possible for Gillon’s group. Like their predecessors, Wang & colleagues analyzed variations in transit times to estimate the masses and densities of the planets. Thanks to their augmented dataset, they were able to include all seven in their calculations, and not just the inner six.

The periods, semimajor axes, and equilibrium temperatures of the TRAPPIST planets are unchanged, and only two of them have smaller radii. Nevertheless, many planetary masses, and all densities, are dramatically different. Figure 1 and Table 1 contrast the results of Wang & colleagues with those of Gillon & colleagues. Figure 2 depicts the planets at their relative sizes and densities according to Wang’s group (revised from the first figure in my previous post on TRAPPIST-1).

Table 1. Comparison of TRAPPIST-1 parameters from Wang et al. and Gillon et al.

Period is expressed in Earth days; radius, mass, and density are expressed in Earth units.
(W) = Wang et al. 2017; (G) = Gillon et al. 2017.

a super mercury among super ganymedes?

As we compare the findings of these two teams, we need to remember that both of them reported their results with large uncertainties (as shown in Table 1). For five out of seven planets, the results on mass from both groups are formally equivalent. The exceptions are planet e, for which the difference between Wang’s highest estimate and Gillon’s lowest is only 2% of an Earth mass (0.02 Mea), and planet h, for which Gillon’s group reported no mass at all. Moreover, for the three innermost planets (b, c, d), the densities estimated by Wang’s group are formally consistent with a rocky composition like Earth’s, again within uncertainties.

But if we focus on the interpretations that each group actually prefers, the differences become too wide to bridge. According to Wang’s group, only the three innermost planets might be rocky in composition, with planet c requiring major enrichment in iron to explain its large mass. Planets b and d, on the other hand, must be either depleted in metals or enriched in volatiles, or both, to achieve their proposed densities. At 62% and 72% of Earth, respectively, their closest analogs in our Solar System are the Moon and Mars.

Figure 2. Revised densities for the planets of TRAPPIST-1

The seven planets of TRAPPIST-1 are shown at their relative sizes, with colors corresponding to the densities estimated by Wang et al. 2017. Yellow shading marks the system habitable zone. Except for planet c, all densities are lower than those preferred by Gillon et al. 2017. This result suggests an internal composition with a rocky core enveloped in a layer of ice. (Update of Figure 1 in a previous post on the same system.)

The next three planets (e, f, g), which occupy the habitable zone, have densities similar to those of Ganymede, Titan, and Callisto, the largest moons of Jupiter and Saturn. The bulk composition of those moons is approximately one-third water ice and two-thirds rock (Hussmann et al. 2015). A similar abundance of ice, possibly accompanied by depletion in metals, is needed to explain the relatively large radii and low masses of this temperate TRAPPIST trio.

For planet h, the smallest and coolest member of the family, the estimated density has such large uncertainties that we can say only that the numbers are equally consistent with a substantial hydrogen envelope (like Uranus), a composition completely dominated by hydrogen (like Saturn), or a rock/metal object with a modest percentage of water ice but no gaseous hydrogen at all (like Europa). Nevertheless, the transit timing data also provide an upper limit on this object’s mass, so we know that planet h is too lightweight to retain a hydrogen atmosphere unless it is constantly replenished by volcanic outgassing. Therefore, this little world’s bulk composition is probably similar to that of the three planets in the habitable zone.

From the new perspective offered by Wang & colleagues, the seven planets of TRAPPIST-1 present far more variety in bulk composition and surface environments than earlier data suggested. Indeed, if we accept the accuracy of these new findings – and I don’t see why we shouldn’t – we can no longer describe TRAPPIST-1 as a system with several Earth-like planets. Instead, we see a single terrestrial planet (c) enriched in iron, with an equilibrium temperature too high to permit surface bodies of water, accompanied by six lightweight planets that variously resemble scaled-up versions of Mars (density 0.71 Earth) and the three largest moons in our Solar System (Callisto, Titan, and Ganymede; respective densities 0.33, 0.34, and 0.35 Earth). Because three of the least dense planets (e, f, g) occupy the system habitable zone, our most optimistic conjecture is that they are ocean worlds with liquid seas sloshing atop layers of high-pressure ice (Kuchner 2003, Leger et al. 2004).

This isn’t an especially promising outlook for anyone who seeks exotic alien organisms, but if your models allow low-density ocean planets to support life (Noack et al. 2016), you can still imagine undulant sea creatures populating the hydrospheres of one or more of these little worlds.

Figure 3. Exotic aquatic life on Earth

Nembrotha cristata (left), a tropical sea slug, by Chriswan Sungkono; Hapalochlaena lunulata (right), a highly venomous octopus native to the Philippines, photographer unknown.

younger star, fatter planets

In related news, a team led by Megan Bedell has offered revised masses and densities for the six transiting planets of Kepler-11. This is the benchmark system for all studies of extrasolar planetology, as it was the first place where astronomers could obtain sufficiently precise data on the transit times of multiple interacting planets to permit estimation of their masses. Back in 2011, when the system was announced, everyone was shocked to learn that planets not much heavier than Earth could support greenhouse atmospheres inflated with hydrogen and helium.

By now, of course, that weirdness is pretty well digested, but Kepler-11 still retains the power to amaze. With transit data extending over the full Kepler mission, this system has already benefited from repeated analyses that led to revisions (mostly downward) in the masses of its six planets. Improved results became available for the first time in 2013, when Jack Lissauer and colleagues published new physical and orbital parameters for the whole system (blogged here).

Now, four years later, we have another update. It’s important to note that the new findings are not based on any new transit data. (As far as I know, no transits of Kepler-11 have been observed since the termination of data collection by the Kepler Mission in 2013.) Instead, the revised parameters are based on precise observations of the host star. Although previous studies have always noted a close resemblance between Kepler-11 and our Sun, Bedell & colleagues go further: they characterize the star as a “Solar twin.”

Contrary to Lissauer’s group, who estimated a stellar age in the range of 7 to 10 billion years, a stellar mass 96% Solar (0.96 Msol), and a stellar radius 105% Solar (1.05 Rsol), Bedell’s group finds that the star is a bit younger than our Sun (3.2 ±0.9 billion years versus 4.55 billion years), with a larger mass (1.04 Msol) and a slightly revised radius (1.02 Rsol). Because most planetary data depend sensitively on the properties of the host star, these new values lead to further revisions in our understanding of the planets.

Table 2. Comparison of Kepler-11 parameters from Bedell et al. and Lissauer et al.

Notes: a = semimajor axis in astronomical units; period = orbital period in days.
B 17 = Bedell et al. 2017; L 13, L 11 = Lissauer et al. 2013, 2011.

Table 2 compares three generations of data on Kepler-11. It’s readily apparent that most of the new parameters offered by Bedell’s group represent a reversion in the direction of the initial findings from 2011. Specifically, all the masses proposed by Bedell’s group are larger than the ones published by Lissauer & colleagues in 2013, as are all radii except for planet g, where we see no change. Yet in comparison with the 2013 update, the latest estimates have less extreme consequences for planetary composition.

As the authors note, the upward revisions in masses and radii result in an average increase of almost 50% in the planets’ bulk density. But the big picture stays mostly the same. As before, all Kepler-11 planets with well-constrained masses are more lightweight than Uranus (14.5 Mea). As before, planets c through f are unambiguously puffy, requiring hydrogen envelopes to bring their ample radii in line with their relatively puny masses (all <10 Mea).

The most consequential change involves planet b, to which the parameters announced in 2013 allowed Lopez & Fortney (2014) to attribute a bulk mass fraction in hydrogen of about 0.5%. Their interpretation seems counterintuitive – I mean, how could an object under 2 Mea retain any hydrogen at all after aeons of extreme irradiation? Nevertheless, to my knowledge, it has been broadly accepted.

The newly estimated density of 0.445 Earth strengthens the argument that planet b is an amalgam of rock and ice, rather like Europa, which has a bulk density of 0.55 Earth. No lightweight envelope is needed to explain its radius. Although I doubt that the findings of Bedell’s group are the last word on Kepler-11b, they offer a physically plausible model of the bulk composition of this benchmark extrasolar planet.

Bedell M, Bean JL, Meléndez J, Mills SM, Fabrycky DC, Freitas FC, Ramírez I, Asplund M, Liu F, Yong D. (2017) Kepler-11 is a Solar Twin: Revising the masses and radii of benchmark planets via precise stellar characterization. Astrophysical Journal 839, 94.
Gillon M, Jehin E, Lederer SM, Delrez L, de Wit J, Burdanov A, Van Grootel V, Burgasser A, Triaud A, Opitom C, Demory B-O, Sahu DK, Bardalez-Gagliuffi D, Magain P, Queloz D. (2016) Temperate Earth-sized planets transiting a nearby ultracool dwarf star. Nature 533, 221-224. Abstract: 2016Natur.533..221G
Gillon M, Triaud A, Demory B-O, Jehin E, Agol E, Deck KM, Lederer SM, de Wit J, Burdanov A, Ingalls JG, Bolmont E, Leconte J, Raymond SN, Selsis F, Turbet M, Barkaoui K, Burgasser A, Burleigh MR, Carey SJ, Chaushev A, Copperwheat CM, Delrez L, Fernandes CS, Holdsworth DL, Kotze EJ, Van Grootel V, Almleaky Y, Benkhaldoun Z, Magain P, Queloz D. (2017) Seven temperate terrestrial planets around the nearby ultracool dwarf star TRAPPIST-1. Nature 542, 456-460. Abstract: 2017Natur.542..456G
Hussmann H, Sotin C, Lunine J. (2015) Interiors and evolution of icy satellites. In Treatise on Geophysics, Volume 10: Physics of Terrestrial Planets and Moons, ed. G. Schubert. Elsevier B.V.
Kuchner MJ. (2003) Volatile-rich Earth-mass planets in the habitable zone. Astrophysical Journal 596, L105-L108.
Leger A, Selsis F, Sotin C, et al. (2004) A new family of planets? “Ocean Planets.” Icarus 169, 499-504.
Lissauer JJ, Jontof-Hutter D, Rowe JF, Fabrycky DC, Lopez ED, Agol E, et al. (2013) All six planets known to orbit Kepler-11 have low densities. Astrophysical Journal 770, 131. Abstract: 2013ApJ...770..131L
Luger R, Sestovic M, Kruse E, Grimm SL, Demory B-O, Agol E, Bolmont E, Fabrycky D, Fernandes CS, Van Grootel V, Burgasser A, Gillon M, et al. (2017) A terrestrial-sized exoplanet at the snow line of TRAPPIST-1. In press.
Noack L, Höning D, Rivoldini A, Heistracher C, Zimov N, Journaux B, Lammer H, Van Hoolst T, Bredehöft JH. (2016) Water-rich planets: How habitable is a water layer deeper than on Earth? Icarus 277, 215-236.
Wang S, Wu DH, Barclay T, Laughlin GP. (2017) Updated masses for the TRAPPIST-1 planets. In press. Abstract: 2017arXiv170404290W

Tuesday, April 18, 2017

HD 219134 Scorecard: 5 planets, 2 transiting

Figure 1. Architecture of the mixed-mass planetary system around HD 219134, a nearby K dwarf, as characterized by Gillon et al. 2017 and Johnson et al. 2016. All five planets are shown at their approximate relative sizes. Planets b and c are observed in transit, so their radii are known. The radii of the other planets are based on those of planets with similar masses and measured radii (e.g., planets d and e are assigned the same radii as Neptune and Saturn, respectively). See Table 1.
Fresh from their discovery of four new Earth-size planets transiting TRAPPIST-1 (a minuscule M dwarf in the Sun’s back yard), Michaël Gillon & colleagues have contributed exciting new data to our developing picture of another nearby exoplanetary system: HD 219134. The host star is a metal-rich K3 dwarf located only 6.55 parsecs away (21 light years) in the direction of Cassiopeia. Gillon & colleagues confirm a previous report by Motalebi & colleagues (blogged here) that the innermost planet (b) is visible in transit, while announcing that the second planet (c) also transits. In addition, they present radial velocity masses for both transiting planets (hereafter tranets), as well as a refined radius for planet b. For both objects, these values are consistent with a purely rocky composition.

After the 2015 announcement by Motalebi & colleagues (hereafter M15), two subsequent studies offered additional data and analyses of the HD 219134 system: Vogt & colleagues (hereafter V15, blogged here) and Johnson & colleagues (hereafter J16, blogged here). Many findings from these studies overlap, but others are mutually inconsistent, including results on the precise number of planets and their approximate masses and periods. Nonetheless, all three studies agreed that HD 219134 hosts two or more low-mass planets on hot and warm orbits, plus one gas giant less massive than Saturn outside the system ice line.

In their new study, Gillon & colleagues confine their attention to the inner system, where they identify a total of four low-mass planets. This result contrasts with the three small planets proposed by M15 and the five preferred by V15. Along with their transit findings, Gillon’s group also report the latest radial velocity data on all four planets from continuing observations with the HARPS-N spectrograph. In passing, they affirm the presence of the giant planet but do not comment on the conflicting results of the earlier studies. Table 1 summarizes their findings on planets b through f, supplemented by the findings of J16 on planet e (which J16 called planet h, even though no one has proposed as many as seven planets – i.e., b through h – for this system).

Table 1. Revised system parameters of HD 219134

Tags: Period = orbital period in days; a = semimajor axis in astronomical units (AU); Radius = radius in Earth units; Mass = mass in Earth units; Teq = equilibrium temperature in Kelvin. Data on planet e are based on those for planet h in Johnson et al. 2016. All other data are based on Gillon et al. 2017.

conflicts resolved?

We’ve now seen four successive studies of HD 219134 conducted by three different scientific teams. (I regard Gillon et al. 2017 as the same team as M15, since the two author groups overlap substantially and both report HARPS-N data.) Our picture of planet b is largely unchanged from the results of M15 and V15, except that we have a firmer understanding of its radius. With the new transit data and improved radial velocity data on planet c, we can also be confident of that planet’s mass, radius, and density, with no change in its estimated period. Even planet d retains virtually the same period reported by M15 and V15, although its mass falls between the values they provided.

Although planet f was not included in the analysis of M15, and a potential planet with a similar periodicity was rejected by J16, the object reported by Gillon & colleagues looks a lot like the planet f proposed by V15: its period is virtually the same, while its mass is a bit lower – a minimum of 7.3 Earth masses (7.3 Mea) instead of 8.9 Mea. Notably, the newly published period of planet f appears to place it just outside a 2:1 mean motion resonance with planet d. Similar period ratios have appeared in several compact low-mass systems discovered by the Kepler Telescope.

Consistent with M15 and J16, Gillon & colleagues implicitly reject V15’s proposed planet g at 94 days. They remain silent on the parameters of the system’s gas giant, to which J16 assign a period of almost 6 years and a semimajor axis of about 3 AU.

mass distribution

The new data suggest that HD 219134 harbors a substantial mass in refractory elements within a space much smaller than the region bounded by Mercury’s orbit in our system (see Table 1). Gillon & colleagues argue that the two innermost planets, b and c, have minimal volatile constituents, with radial velocity data indicating a combined refractory mass of about 9 Mea for this pair. Although we remain ignorant of the radii of the next two planets, f and d, most exoplanets with comparable masses (in the approximate range of 5 to 20 Mea) and comparable thermal environments (cooler than Venus) support substantial envelopes of hydrogen and helium. Existing studies suggest that the bulk mass composition of such planets is generally between 1% and 30% hydrogen/helium (see Lopez & Fortney 2014). Therefore, given their combined radial velocity masses of 23.5 Mea, we can estimate an aggregate mass of 16-22 Mea in refractory elements for this cooler, fatter pair, with hydrogen and other volatiles accounting for the remaining 1-7 Mea. That brings the total refractory mass of the four inner planets into the range of 25-31 Mea.

Altogether, the radial velocity data indicate a total mass of about 33 Mea for the inner system of HD 219134, placing it in roughly the same ballpark as the aggregate mass of the six-planet systems around Kepler-11 (about 30 Mea) and Kepler-20 (about 55 Mea). All these endowments are much richer than the aggregate mass of the four terrestrial planets in our Solar System, which collectively sum to 1.98 Mea. 

stingy spitzer scheduling

The late, lamented Kepler Mission demonstrated the need to collect continuous photometric data over a period of years in order to characterize the inner reaches of any planetary system. The longer the sequence of light curves, the more robust the resulting analysis of potential transits. In light of that history, I was surprised to learn that Gillon’s group was able to observe only two transits each for planets b and c. Their observing sessions with the Spitzer Space Telescope were confined to periods of 6.5 to 7.5 hours centered on the transit window predicted for each planet. As a result, we have no idea whether any of the other planets orbiting HD 219134 can be observed in transit. Definitive findings one way or the other would dramatically improve our understanding of this system’s distinctive architecture and constrain the degree of coplanarity among the orbits of the inner planets

Notably, Spitzer had to monitor TRAPPIST-1 for 20 consecutive days in order to untangle the orbits of its seven known planets, and even that allotment was too brief to obtain a clear picture of the outermost planet, which has a period just shy of 19 days. To illuminate the inner system of HD 219134 would require an observing run in excess of 200 days – evidently an impossibility at present. What we humans need is a whole array of space-based observatories staring year after year at all the most interesting stars in our neighborhood.

architecture and habitability

As I discussed in an earlier post on HD 219134, this system can be characterized as a “rich mixed-mass system,” defined as a planetary system with at least two low-mass planets plus at least one gas giant on a wider orbit. Including our Solar System, about a dozen such configurations are known. They share important similarities. In most of them – including HD 219134 – two or more low-mass planets are observed in transit, while the gas giant tends to be the outermost of the known planets. (The exceptions to the latter generalization are Kepler-87, Kepler-89, and the Solar System, each of which includes a gas giant with a low-mass planet on an exterior orbit.)

In more than half of the known systems –Kepler-48, Kepler-68, Kepler-87, Kepler-167, HD 219134, HD 10180, and our Solar System – we note a gap between the inner system of low-mass planets and the outer gas giant. Except for our own system, we can’t be sure whether any of these apparent gaps is truly empty. Some might be occupied by one or more planets that are misaligned with the others, and thus not visible in transit, or hiding a planet or planets that are too lightweight for radial velocity observations to detect.

In any case, such gaps are significant, because in HD 219134 and several other systems, they correspond to the classical habitable zone. That’s why I’d like to see lots of follow-up observations of HD 219134, accompanied by analyses of the orbital stability of potential Earth-mass planets occupying the space between 0.5 and 1 AU. Three such analyses have already been conducted for the habitable zone of HD 10180, with conflicting results (as blogged here).

beware of outsiders

Equally significant is the mechanism responsible for creating and maintaining these orbital gaps. The difficulty of identifying such a mechanism is underscored by the case of our Solar System, where we still have no widely endorsed scenario to explain why mass is severely depleted between the orbits of Earth and Jupiter, and altogether absent between the orbits of Mars and the Main Belt asteroids. Jupiter is probably involved, but the details are elusive (see Batygin & Laughlin 2015, Raymond et al. 2016). 

The question of orbital gaps and missing mass in this subset of system architectures is subsumed by a more general concern regarding the role of longer-period gas giants in systems with multiple low-mass planets on hot or warm orbits. Several recent studies have addressed the stability of compact multiplanet systems in the presence of an outer giant, whether seen or unseen (Hands & Alexander 2016, Hansen 2017, Becker & Adams 2017, Huang et al. 2017, Jontof-Hutter et al. 2017, Read et al. 2017). The results suggest that “friendly” giants, meaning those permitting the survival of several small, closely spaced planets, need to be cool in more ways than one. Not only must they follow orbits well-separated from the inner planets, in regions where insolation and equilibrium temperatures are lower; they must also be dynamically cool, with minimal eccentricities (deviations from circularity) and inclinations (deviations from coplanarity).

The most delicately balanced configuration – and thus the one most easily upset – contains several planets continually observable in transit. This balance can be maintained only a) if no gas giant is present or b) if the giant is either precisely aligned with the inner ensemble or very widely separated from it. Higher values of eccentricity, inclination, and mass, as well as lower values of semimajor axis, will lead to perturbations of the inner planets. In a perturbed regime, their inclinations might oscillate, such that transits periodically cease for certain planets and then resume after an interval, or become permanently misaligned, such that only one planet, or none at all, is observed in transit. In cases of extreme excitation of inclinations and eccentricities, some or all of the inner planets would be lost altogether.

For example, Becker & Adams found that, among 18 Kepler systems with at least 4 transiting planets each, potential gas giant companions would have to maintain semimajor axes of 10 AU or more to avoid perturbing the inner planets. They also made more specific predictions for several interesting systems featured in previous blog posts: WASP-47, Kepler-11, Kepler-62, Kepler-90, and Kepler-20.

The inner system of WASP-47 consists of a gas giant flanked by two low-mass planets inside a semimajor axis of 0.10 AU; the outer system contains another gas giant at 1.36 AU. Becker & Adams concluded that the orbit of the outer giant must be approximately coplanar with those of the inner tranets, or else they would become mutually misaligned and no longer be observable in transit. For Kepler-11, Kepler-62, and Kepler-20, their conclusions were even more restrictive: none of these systems could harbor an additional planet of 30 Mea or more between 1 and 30 AU without upsetting the clockwork orbits of the inner tranets. (Notably, Jontof-Hutter & colleagues reached a less restrictive conclusion for Kepler-11, ruling out any slightly inclined Jupiter-mass planets within 3 AU.) For Kepler-20, a total of six low-mass planets are known, but only five are observed in transit, given the misalignment of planet g. Becker & Adams propose that an undetected gas giant on a cool orbit might be responsible for this configuration.  

In an analogous study, Read & colleagues investigated the stability of systems containing short-period tranets and non-transiting giants at larger semimajor axes, including two rich mixed-mass systems, Kepler-48 and Kepler-68. For Kepler-48, they concluded that the outer giant must be closely aligned with the inner system, whereas for Kepler-68, available data provided no strong constraints on inclination.

The upshot of this group of studies is that compact inner systems of low-mass planets can typically tolerate cool giants only when the latter are well separated and well aligned. Accordingly, Brad Hansen included an evocative short title for his recent article on the stability problem: Beware of Outsiders. Once we have more data on HD 219134, comparable analyses should be able to constrain the alignment of planet e.

tranets in near space

HD 219134 now warrants a throng of superlatives: it’s the nearest star with a tranet of any description, the nearest Sun-like star with a tranet, the nearest with more than one tranet, the nearest with a terrestrial tranet, and the nearest with more than one terrestrial tranet. In order of increasing distance from the Sun, its closest rivals are Gliese 436 at 10.2 parsecs (one hot tranet more massive than Neptune), Gliese 1132 at 12 parsecs (one hot terrestrial tranet), TRAPPIST 1 at 12.1 parsecs (seven terrestrial tranets), 55 Cancri at 12.3 parsecs (one very hot, massive terrestrial tranet), LHS 1140 at 12.47 parsecs (one temperate terrestrial tranet), Gliese 1214 at 13 parsecs (one hot, puffy tranet about half the mass of Uranus), HD 189733 at 19.2 parsecs (one transiting Hot Jupiter), HD 97658 at 21 parsecs (one hot tranet more massive than Neptune), Gliese 3470 at 29 parsecs (one hot Uranus-mass tranet), HAT-P-11 at 38 parsecs (one hot tranet more massive than Neptune), and Kepler-42 at 39 parsecs (three warm terrestrial tranets in the nearest Kepler system). All the more distant tranets are either Hot Jupiters or low-mass planets discovered by space-based telescopes (Kepler and CoRoT).

Among the 12 transiting systems located within 40 parsecs (130 light years), only one includes a transiting gas giant on a hot orbit (HD 189733), a reminder that the well-known species of Hot Jupiters is actually quite rare. More than half of these nearby transiting systems center on M dwarfs, while only two systems with rocky tranets orbit Sun-like stars (HD 219134 and 55 Cancri). Coincidentally or not, these two are also the only mixed-mass systems in the group.

Given so many superlatives and distinctions, it’s safe to predict that we’ll be hearing more news from HD 219134 for years to come.

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