Abstract:The magma ocean concept was first conceived to explain the geology of the Moon, but hemispherical or global oceans of silicate melt could be a widespread "lava world" phase of rocky planet accretion, and could persist on planets on short-period orbits around other stars. The formation and crystallization of magma oceans could be a defining stage in the assembly of a core, origin of a crust, initiation of tectonics, and formation of an atmosphere. The last decade has seen significant advances in our understandi… Show more
“…WASP-47 e, Kepler-78 b, Kepler-10 b, CoRot-7 b, and Kepler-36 b: These planets have been the focus of several theoretical studies that conjecture -in agreement with our analysisthat they should either have secondary atmospheres (and magma oceans) or/and low density interiors (e.g. Schaefer & Fegley 2009;Ito et al 2015;Dorn et al 2017b;Dai et al 2019;Chao et al 2020). Unfortunately, their host stars are much dimmer than 55 Cnc with V ∼ 11 to 12 mag (Léger et al 2009;Queloz et al 2009;Howard et al 2013;Becker et al 2015;Batalha et al 2011).…”
Section: Planet Candidates That Are Best Modeled With Secondary Atmos...supporting
Past studies have demonstrated that atmospheric escape by the core-powered mass-loss mechanism can explain a multitude of observations associated with the radius valley that separates the super-Earth and sub-Neptune planet populations. Complementing such studies, in this work, we present a shortlist of planets that could be losing their atmospheres today if their evolution is indeed primarily dictated by core-powered mass-loss. We use Bayesian inference analysis on our planet evolution and mass-loss model to estimate the posteriors of the parameters that encapsulate the current state of a given planet, given their published masses, radii and host star properties. Our models predict that the following planets could be losing their atmospheres today at a rate 10 7 g/s at 50% confidence level: pi Men c, Kepler-60 d, Kepler-60 b, HD 86226 c, EPIC 249893012 b, Kepler-107 c, HD 219134 b, Kepler-80 e, Kepler-138 d and GJ 9827 d. As a by-product of our Bayesian inference analysis, we were also able to identify planets that most-likely harbor either secondary atmospheres abundant with high mean-molecular weight species, low-density interiors abundant with ices, or both. The planets belonging to this second category are WASP-47 e, Kepler-78 b, Kepler-10 b, CoRoT-7 b, HD 80653 b, 55 Cnc e and Kepler-36 b. While the aforementioned lists are by no means exhaustive, we believe that candidates presented here can serve as useful input for target selection for future surveys and for testing the importance of core-powered mass-loss in individual planetary systems.
“…WASP-47 e, Kepler-78 b, Kepler-10 b, CoRot-7 b, and Kepler-36 b: These planets have been the focus of several theoretical studies that conjecture -in agreement with our analysisthat they should either have secondary atmospheres (and magma oceans) or/and low density interiors (e.g. Schaefer & Fegley 2009;Ito et al 2015;Dorn et al 2017b;Dai et al 2019;Chao et al 2020). Unfortunately, their host stars are much dimmer than 55 Cnc with V ∼ 11 to 12 mag (Léger et al 2009;Queloz et al 2009;Howard et al 2013;Becker et al 2015;Batalha et al 2011).…”
Section: Planet Candidates That Are Best Modeled With Secondary Atmos...supporting
Past studies have demonstrated that atmospheric escape by the core-powered mass-loss mechanism can explain a multitude of observations associated with the radius valley that separates the super-Earth and sub-Neptune planet populations. Complementing such studies, in this work, we present a shortlist of planets that could be losing their atmospheres today if their evolution is indeed primarily dictated by core-powered mass-loss. We use Bayesian inference analysis on our planet evolution and mass-loss model to estimate the posteriors of the parameters that encapsulate the current state of a given planet, given their published masses, radii and host star properties. Our models predict that the following planets could be losing their atmospheres today at a rate 10 7 g/s at 50% confidence level: pi Men c, Kepler-60 d, Kepler-60 b, HD 86226 c, EPIC 249893012 b, Kepler-107 c, HD 219134 b, Kepler-80 e, Kepler-138 d and GJ 9827 d. As a by-product of our Bayesian inference analysis, we were also able to identify planets that most-likely harbor either secondary atmospheres abundant with high mean-molecular weight species, low-density interiors abundant with ices, or both. The planets belonging to this second category are WASP-47 e, Kepler-78 b, Kepler-10 b, CoRoT-7 b, HD 80653 b, 55 Cnc e and Kepler-36 b. While the aforementioned lists are by no means exhaustive, we believe that candidates presented here can serve as useful input for target selection for future surveys and for testing the importance of core-powered mass-loss in individual planetary systems.
“…Thus, a mixture of these gases should be considered to study the thermal structure of planets with secondary atmospheres. Planets b and c in the TRAPPIST-1 system could present magma oceans due to their high surface temperatures (T ≥ 1300 K) (Barr et al 2018;Chao et al 2020), and the maximum surface pressure we have obtained here can be used to assess the current outgassing rate in magma ocean studies (Noack et al (2017), Baumeister et al submitted) and better constrain the WMF for the interior magma ocean models (e.g Katyal et al (2020)) in the future.…”
Section: Discussionmentioning
confidence: 75%
“…The integrated model should also include a description escape processes, such as hydrodynamic or Jeans escapes, which is particularly interesting to explore the lifetime of secondary atmospheres. Close-in, low-mass planets are likely to outgas atmospheric species, such as CO 2 , and form O 2 via photodissociation of outgased H 2 O, during their magma ocean stage or due to plate tectonics (Chao et al 2020). Thus, a mixture of these gases should be considered to study the thermal structure of planets with secondary atmospheres.…”
Context. Planetary mass and radius data are showing a wide variety in densities of low-mass exoplanets. This includes sub-Neptunes, whose low densities can be explained with the presence of a volatile-rich layer. Water is one of the most abundant volatiles, which can be in the form of different phases depending on the planetary surface conditions. To constrain their composition and interior structure, it is required to develop models that calculate accurately the properties of water at its different phases. Aims. We present an interior structure model that includes a multiphase water layer with steam, supercritical and condensed phases. We derive the constraints for planetary compositional parameters and their uncertainties, focusing on the multiplanetary system TRAPPIST-1, which presents both warm and temperate planets. Methods. We use a 1D steam atmosphere in radiative-convective equilibrium with an interior whose water layer is in supercritical phase self-consistently. For temperate surface conditions, we implement liquid and ice Ih to ice VII phases in the hydrosphere. We adopt a MCMC inversion scheme to derive the probability distributions of core and water compositional parameters Results. We refine the composition of all planets and derive atmospheric parameters for planets b and c. The latter would be in a post-runaway greenhouse state and could be extended enough to be probed by space mission such as JWST. Planets d to h present condensed ice phases, with maximum water mass fractions below 20%. Conclusions. The derived amounts of water for TRAPPIST-1 planets show a general increase with semi-major axis, with the exception of planet d. This deviation from the trend could be due to formation mechanisms, such as migration and an enrichment of water in the region where planet d formed, or an extended CO 2 -rich atmosphere.
“…The youth of TOI-1807 b makes it an even more compelling target for secondary eclipse spectroscopy, as the luminosity of the planet's cooling core may be an order of magnitude higher than it would be at older (> 1 Gyr) ages (Linder et al 2019). Finally, as a candidate "lava world" (Chao et al 2020), TOI-1807 b presents an opportunity to study the early evolution of these poorly-understood objects.…”
We report the discovery of two planetary systems around comoving stars; TOI-2076 (TIC 27491137) and TOI-1807 (TIC 180695581). TOI-2076 is a nearby (41.9 pc) multi-planetary system orbiting a young (204 ± 50 Myr), bright (K = 7.115 in TIC v8.1). TOI-1807 hosts a single transiting planet, and is similarly nearby (42.58 pc), similarly young (180 ± 40 Myr), and bright. Both targets exhibit significant, periodic variability due to star spots, characteristic of their young ages. Using photometric data collected by TESS we identify three transiting planets around TOI-2076 with radii of R b =3.3±0.04 R ⊕ , R c =4.4±0.05 R ⊕ , and R d =4.1±0.07 R ⊕ . Planet TOI-2076b has a period of P b =10.356 d. For both TOI 2076c and d, TESS observed only two transits, separated by a 2-year interval in which no data were collected, preventing a unique period determination. A range of long periods (>17d) are consistent with the data. We identify a short-period planet around TOI-1807 with a radius of R b =1.8±0.04 R ⊕ and a period of P b =0.549 d. Their close proximity, and bright, cool host stars, and young ages, make these planets excellent candidates for follow-up. TOI-1807b is one of the best known small (R < 2 R ⊕ ) planets for characterization via eclipse spectroscopy and phase curves with JWST. TOI-1807b is the youngest ultra-short period planet discovered to date, providing valuable constraints on formation time-scales of short period planets. Given the rarity of young planets, particularly in multiple planet systems, these planets present an unprecedented opportunity to study and compare exoplanet formation, and young planet atmospheres, at a crucial transition age for formation theory.
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