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The field of exoplanetary science has experienced a recent surge of new
systems that is largely due to the precision photometry provided by the Kepler
mission. The latest discoveries have included compact planetary systems in
which the orbits of the planets all lie relatively close to the host star,
which presents interesting challenges in terms of...
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Context 1
... right panel of Figure 1 is a zoom of this region which shows the radius- separation trend more clearly. Table 1 contains the com- plete list of moons which fall within 30 planet radii, along with their absolute and scaled semi-major axes and radii. We fit a power-law to these data of the form y = c 1 x c2 where c 1 = 0.00507, c 2 = 0.90777, and c 2 describes the slope of the fit. ...
Context 2
... estimate the masses of the planets using the mass-radius relation- ships of Weiss et al. (2013). We have calculated these timescales for each of the objects in the populations shown in Tables 1 and 2. For the moon population, the parameters for the star and planet in Equation 1 are replaced with the parameters of the planet and moon respectively. ...
Context 3
... compact Kepler systems have very small mutual inclinations by virtue of their transit detection, and it was shown by Lissauer et al. (2011b) that the inclination dispersion of these systems generally have a mean < 10 • . Of the Solar System moons shown in Table 1, only two have inclina- tions larger than 1.0 • with respect to the local Laplace plane. These are Miranda (4.338 • ) which has strong ev- idence of significant geological, tidal, and orbital evolu- tion (Tittemore & Wisdom 1990);and Triton (156.8 • ) which, as previously mentioned, was likely captured into its current retrograde orbit. ...
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Citations
... Madeira et al. (2021) note that the formation of the Galilean satellites may be similar to exoplanetary systems with close-in super-Earth's such as the TRAPPIST-1 system. The architecture of the Solar System's satellite systems can also be compared with exoplanetary systems (Kane et al. 2013). ...
The International Astronomical Union definitions for Planet and Dwarf Planet both require that a body has sufficient mass to overcome rigid body forces and self gravitate into a nearly round shape. However, quantitative standards for determining when a body is sufficiently round have been lacking. Previously published triaxial ellipsoid solutions for asteroids, satellites, and Dwarf Planets in the radius range 135 to 800 km are examined to identify a minimum mass above which the entire population, regardless of composition, is round. From this data, the minimum mass to meet the roundness criterion is 5.0 x 10E20 kg. The triaxial shape data suggests three radius ranges: (1) bodies with a radius less than 160 km are non-spheroidal, (2) bodies with a radius in the range 160 to 450 km are transitional in shape or nearly round, (3) bodies with a radius greater than 450 km are spheroidal. Bodies orbiting the Sun with a mass greater than 5.0 x 10E20 kg are Planets or Dwarf Planets. Arguments are presented for including the 16 spheroidal moons of the Solar System as a third dynamical class that can be identified as Satellite Planets. Definitions are proposed that expand upon the taxonomy started in 2006 with the International Astronomomical Union Planet and Dwarf Planet classes.
... Identifying exosatellites bridges the knowledge gap between the population demographics of low-mass stellar systems, such as TRAPPIST-1, and the moon systems of the Solar System giant planets. Previous comparisons between compact Kepler systems and the moons around giant planets in the Solar System by Kane et al. (2013) have revealed similarities in system architectures, despite the host masses varying by several orders of magnitudes. TEMPO will enable comparative studies of companion architecture extending down to the planetary-mass host regime, several orders of magnitude lower than previously explored. ...
The TEMPO (Transiting Exosatellites, Moons, and Planets in Orion) Survey is a proposed 30-day observational campaign using the Nancy Grace Roman Space Telescope. By providing deep, high-resolution, short-cadence infrared photometry of a dynamic star-forming region, TEMPO will investigate the demographics of exosatellites orbiting free-floating planets and brown dwarfs -- a largely unexplored discovery space. Here, we present the simulated detection yields of three populations: extrasolar moon analogs orbiting free-floating planets, exosatellites orbiting brown dwarfs, and exoplanets orbiting young stars. Additionally, we outline a comprehensive range of anticipated scientific outcomes accompanying such a survey. These science drivers include: obtaining observational constraints to test prevailing theories of moon, planet, and star formation; directly detecting widely separated exoplanets orbiting young stars; investigating the variability of young stars and brown dwarfs; constraining the low-mass end of the stellar initial mass function; constructing the distribution of dust in the Orion Nebula and mapping evolution in the near-infrared extinction law; mapping emission features that trace the shocked gas in the region; constructing a dynamical map of Orion members using proper motions; and searching for extragalactic sources and transients via deep extragalactic observations reaching a limiting magnitude of \,mag (F146 filter).
... A short while ago, exoplanetary science celebrated the milestone of 5,000 new worlds 1 , mainly owing to recent photometric space missions 2,3 . These discoveries reveal a remarkable planet zoo, with a large diversity of planetary system architectures 4,5 and physical parameters, including compact systems close to the hosting star 6,7 . This latter finding has inspired further studies into star-planet tidal interaction, as well as the search for relationships between stellar and planetary parameters, timescales and implications for the planetary systems [8][9][10][11][12][13] . ...
Star–planet interactions play, among other things, a crucial role in planetary orbital configurations by circularizing orbits, aligning the star and planet spin and synchronizing stellar rotation with orbital motions. This is especially true for innermost giant planets, which can be schematized as binary systems with a very large mass ratio. Despite a few examples where spin–orbit synchronization has been obtained, there is no demographic study on synchronous regimes in those systems yet. Here we use a sample of 1,055 stars with innermost planet companions to show the existence of three observational loci of star–planet synchronization regimes. Two of them have dominant fractions of subsynchronous and supersynchronous star–planet systems, and a third less populated regime of potentially synchronized systems. No synchronous star–planet system with a period higher than 40 days has been detected yet. This landscape is different from eclipsing binary systems, most of which are synchronized. We suggest that planets in a stable asynchronous spin state belonging to star–planet systems in a supersynchronized regime offer the most favourable conditions for habitability.
... Future detection and observational measurements will be biased toward short-period planets. As such, compact systems (e.g., multiple planets with P < 50 days) of planets close to the host star serve as blueprints for understanding the diversity of exoplanet system architectures (Kane et al. 2013;Tamayo et al. 2020). Owing to the proximity of planets in these systems, mutual gravitational interactions between neighboring planets can cause spin-axis dynamics that may be crucial from observational and habitability standpoints. ...
Climate modeling has shown that tidally influenced terrestrial exoplanets, particularly those orbiting M-dwarfs, have unique atmospheric dynamics and surface conditions that may enhance their likelihood to host viable habitats. However, sporadic libration and rotation induced by planetary interactions, such as those due to mean motion resonances (MMR) in compact planetary systems, may destabilize attendant exoplanets away from synchronized states (1:1 spin-orbit ratios). Here, we use a three-dimensional N-rigid-body integrator and an intermediately complex general circulation model to simulate the evolving climates of TRAPPIST-1 e and f with different orbital- and spin-evolution pathways. Planet f scenarios perturbed by MMR effects with chaotic spin variations are colder and dryer compared to their synchronized counterparts due to the zonal drift of the substellar point away from open ocean basins of their initial eyeball states. On the other hand, the differences between perturbed and synchronized planet e are minor due to higher instellation, warmer surfaces, and reduced climate hysteresis. This is the first study to incorporate the time-dependent outcomes of direct gravitational N-rigid-body simulations into 3D climate modeling of extrasolar planets, and our results show that planets at the outer edge of the habitable zones in compact multiplanet systems are vulnerable to rapid global glaciations. In the absence of external mechanisms such as orbital forcing or tidal heating, these planets could be trapped in permanent snowball states.
... The "deep dive" into the terrestrial regime of exoplanet detection was largely enabled by the Kepler mission [13]; a legacy that is now being continued with the Transiting Exoplanet Survey Satellite (TESS) [89]. Moreover, these discoveries have revealed the diversity of planetary system architectures [31,106] including compact systems of planets close to the host star [36,53]. The proximity of exoplanets to their host star has spurred further study into tidal locking scenarios, including the time scales and implications for the planets [6]. ...
The discovery and characterization of Earth-sized planets that are in, or near, a tidally-locked state are of crucial importance to understanding terrestrial planet evolution, and for which Venus is a clear analog. Exoplanetary science lies at the threshold of characterizing hundreds of terrestrial planetary atmospheres, thereby providing a statistical sample far greater than the limited inventory of terrestrial planetary atmospheres within the Solar System. However, the model-based approach for characterizing exoplanet atmospheres relies on Solar System data, resulting in our limited inventory being both foundational and critical atmospheric laboratories. Present terrestrial exoplanet demographics are heavily biased toward short-period planets, many of which are expected to be tidally locked, and also potentially runaway greenhouse candidates, similar to Venus. Here we describe the rise in the terrestrial exoplanet population and the study of tidal locking on climate simulations. These exoplanet studies are placed within the context of Venus, a local example of an Earth-sized, asynchronous rotator that is near the tidal locking limit. We describe the recent lessons learned regarding the dynamics of the Venusian atmosphere and how those lessons pertain to the evolution of our sibling planet. We discuss the implications of these lessons for exoplanet atmospheres, and outline the need for a full characterization of the Venusian climate in order to achieve a full and robust interpretation of terrestrial planetary atmospheres.
... While systems of short-period rocky planets strongly resemble scaled-up versions of the solar system's giant planet satellite systems (Kane et al. 2013;Miguel et al. 2020), it is likely that the varied configurations of moons around Jupiter, Saturn, Uranus, and Neptune also evince a complex and diverse range of formation and evolutionary histories (e.g., Canup & Ward 2002;Nesvorný et al. 2007;Ćuk et al. 2016;Batygin & Morbidelli 2020;Madeira et al. 2021). Nevertheless, it is generally accepted that short-period, rocky planets around lowmass stars must form through one of two possible avenues: (1) in situ via planetesimal impacts with potential contributions from pebbles (Raymond et al. 2007b;Hansen 2015) or (2) further out in the primordial nebular disk with more significant contributions from pebbles and subsequent implantation in the HZ via Type I migration (Ogihara & Ida 2009;Ormel et al. 2017). ...
In recent years, a paradigm shift has occurred in exoplanet science, wherein low-mass stars are increasingly viewed as a foundational pillar of the search for potentially habitable worlds in the solar neighborhood. However, the formation processes of this rapidly accumulating sample of planet systems are still poorly understood. Moreover, it is unclear whether tenuous primordial atmospheres around these Earth analogs could have survived the intense epoch of heightened stellar activity that is typical for low-mass stars. We present new simulations of in situ planet formation across the M-dwarf mass spectrum, and derive leftover debris populations of small bodies that might source delayed volatile delivery. We then follow the evolution of this debris with high-resolution models of real systems of habitable zone planets around low-mass stars such as TRAPPIST-1, Proxima Centauri, and TOI-700. While debris in the radial vicinity of the habitable zone planets is removed rapidly, thus making delayed volatile delivery highly unlikely, we find that material ubiquitously scattered into an exo-asteroid belt region during the planet-formation process represents a potentially lucrative reservoir of icy small bodies. Thus, the presence of external approximately Neptune–Saturn mass planets capable of dynamically perturbing these asteroids would be a sign that habitable zone worlds around low-mass stars might have avoided complete desiccation. However, we also find that such giant planets significantly limit the efficiency of asteroidal implantation during the planet-formation process. In the coming decade, long-baseline radial velocity studies and Roman Space Telescope microlensing observations will undoubtedly further constrain this process.
... Given the prevalence of satellites within the Solar System, substantial effort is being devoted to the search for moons orbiting exoplanets (e.g., Heller et al., 2014;Hill et al., 2018;Kipping et al., 2013). Furthermore, formation of regular moons, such as those in the Galilean system, may serve as analogs of compact exoplanetary systems in terms of their formation and architectures (Batygin & Morbidelli, 2020;Dobos et al., 2019;Kane, Hinkel, et al., 2013;Makarov et al., 2018). However, there are numerous questions that remain regarding the wide array of moons in the Solar System, including their geology and, in some cases, atmospheres. ...
Over the past several decades, thousands of planets have been discovered outside our Solar System. These planets exhibit enormous diversity, and their large numbers provide a statistical opportunity to place our Solar System within the broader context of planetary structure, atmospheres, architectures, formation, and evolution. Meanwhile, the field of exoplanetary science is rapidly forging onward toward a goal of atmospheric characterization, inferring surface conditions and interiors, and assessing the potential for habitability. However, the interpretation of exoplanet data requires the development and validation of exoplanet models that depend on in situ data that, in the foreseeable future, are only obtainable from our Solar System. Thus, planetary and exoplanetary science would both greatly benefit from a symbiotic relationship with a two‐way flow of information. Here, we describe the critical lessons and outstanding questions from planetary science, the study of which are essential for addressing fundamental aspects for a variety of exoplanetary topics. We outline these lessons and questions for the major categories of Solar System bodies, including the terrestrial planets, the giant planets, moons, and minor bodies. We provide a discussion of how many of these planetary science issues may be translated into exoplanet observables that will yield critical insight into current and future exoplanet discoveries.
... The advantage of this bias is that it has enabled a thorough exploration of multiple planet systems that exists in closely spaced orbits, often in extreme insolation flux environments, referred to as compact systems. The architecture and dynamics of compact planetary systems have been previously studied in detail (Ford 2014), including the dynamical connection to formation (Kane et al. 2013;Pu & Wu 2015) and the exclusion of moons (Kane 2017). Barnes & Quinn (2004) suggested that planetary systems may have quantifiable limits to the dynamically allowed number of planets. ...
Uncovering the occurrence rate of terrestrial planets within the habitable zone (HZ) of their host stars has been a particular focus of exoplanetary science in recent years. The statistics of these occurrence rates have largely been derived from transiting planet discoveries, and have uncovered numerous HZ planets in compact systems around M-dwarf host stars. Here we explore the width of the HZ as a function of spectral type, and the dynamical constraints on the number of stable orbits within the HZ for a given star. We show that, although the Hill radius for a given planetary mass increases with larger semimajor axis, the width of the HZ for earlier-type stars allows for more terrestrial planets in the HZ than late-type stars. In general, dynamical constraints allow ~6 HZ Earth-mass planets for stellar masses ≳0.7M⊙, depending on the presence of farther out giant planets. As an example, we consider the case of Beta CVn, a nearby bright solar-type star. We present 20 yr of radial velocities (RV) from the Keck/High Resolution Echelle Spectrometer (HIRES) and Automated Planet Finder (APF) instruments and conduct an injection-recovery analysis of planetary signatures in the data. Our analysis of these RV data rule out planets more massive than Saturn within 10 au of the star. These system properties are used to calculate the potential dynamical packing of terrestrial planets in the HZ and show that such nearby stellar targets could be particularly lucrative for HZ planet detection by direct imaging exoplanet missions.
... Even the intrasystem uniformity inherent to the demographics of sub-Jovian extrasolar planets (Millholland et al. 2017;Weiss et al. 2018) is aptly reproduced in the Galilean ensemble of moons. The ensuing possibility that this similarity may point to a deeper analogy between conglomeration pathways of solar system satellites and short-period exoplanets has not eluded the literature (Kane et al. 2013;Ronnet & Johansen 2020). Nevertheless, it is intriguing to notice that while the pursuit to quantify the formation of extrasolar super-Earths has received considerable attention over the course of the recent decades (see, e.g., the recent works of Bitsch 2019; Izidoro et al. 2019;Liu et al. 2019;Rosenthal & Murray-Clay 2019;Kuwahara & Kurokawa 2020;Poon et al. 2020 and the references therein), a complete understanding of the formation of the solar system's giant planet satellites themselves remains incomplete (Canup & Ward 2009;Miguel & Ida 2016;Ronnet & Johansen 2020). ...
Recent analyses have shown that the concluding stages of giant planet formation are accompanied by the development of a large-scale meridional flow of gas inside the planetary Hill sphere. This circulation feeds a circumplanetary disk that viscously expels gaseous material back into the parent nebula, maintaining the system in a quasi-steady state. Here, we investigate the formation of natural satellites of Jupiter and Saturn within the framework of this newly outlined picture. We begin by considering the long-term evolution of solid material, and demonstrate that the circumplanetary disk can act as a global dust trap, where s• ~ 0.1–10 mm grains achieve a hydrodynamical equilibrium, facilitated by a balance between radial updraft and aerodynamic drag. This process leads to a gradual increase in the system's metallicity, and eventually culminates in the gravitational fragmentation of the outer regions of the solid subdisk into R ~ 100 km satellitesimals. Subsequently, satellite conglomeration ensues via pair-wise collisions but is terminated when disk-driven orbital migration removes the growing objects from the satellitesimal feeding zone. The resulting satellite formation cycle can repeat multiple times, until it is brought to an end by photoevaporation of the parent nebula. Numerical simulations of the envisioned formation scenario yield satisfactory agreement between our model and the known properties of the Jovian and Saturnian moons.
... Data by Berta-Thompson et al. (2015) for GJ1132, Charbonneau et al. (2009) for GJ1214, for GJ3323, Dittmann et al. (2017) and Ment et al. (2019) for LHS1140, Bonfils et al. (2018) for Ross128, Anglada-Escudé et al. (2016) for Proxima Centauri, Gillon et al. (2016) for TRAPPIST-1, for YZ Cet and Zechmeister et al. (2019) for Teegarden's star system. be more similar to the formation of regular satellites than the one around solar-type stars (Chiang & Laughlin 2013;Kane, Hinkel & Raymond 2013). Some evidence of this can be seen in the observed population of planets around small stars. ...
The detection of Earth-size exoplanets around low-mass stars –in stars such as Proxima Centauri and TRAPPIST-1– provide an exceptional chance to improve our understanding of the formation of planets around M stars and brown dwarfs. We explore the formation of such planets with a population synthesis code based on a planetesimal-driven model previously used to study the formation of the Jovian satellites. Because the discs have low mass and the stars are cool, the formation is an inefficient process that happens at short periods, generating compact planetary systems. Planets can be trapped in resonances and we follow the evolution of the planets after the gas has dissipated and they undergo orbit crossings and possible mergers. We find that formation of planets above Mars mass and in the planetesimal accretion scenario, is only possible around stars with masses M⋆ ≥ 0.07Msun and discs of Mdisc ≥ 10−2 Msun. We find that planets above Earth-mass form around stars with masses larger than 0.15 Msun, while planets larger than 5 M⊕ do not form in our model, even not under the most optimal conditions (massive disc), showing that planets such as GJ 3512b form with another, more efficient mechanism. Our results show that the majority of planets form with a significant water fraction; that most of our synthetic planetary systems have 1, 2 or 3 planets, but planets with 4,5,6 and 7 planets are also common, confirming that compact planetary systems with many planets should be a relatively common outcome of planet formation around small stars.
