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Artículos de revistas sobre el tema "Giant gaseous planets"

Autor: Grafiati
Publicado: 20 de abril de 2024

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1

Veras, Dimitri, and Jim Fuller. "Tidal circularization of gaseous planets orbiting white dwarfs." Monthly Notices of the Royal Astronomical Society 489, no. 2 (2019): 2941–53. http://dx.doi.org/10.1093/mnras/stz2339.

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ABSTRACT A gas giant planet which survives the giant branch stages of evolution at a distance of many au and then is subsequently perturbed sufficiently close to a white dwarf will experience orbital shrinkage and circularization due to star–planet tides. The circularization time-scale, when combined with a known white dwarf cooling age, can place coupled constraints on the scattering epoch as well as the active tidal mechanisms. Here, we explore this coupling across the entire plausible parameter phase space by computing orbit shrinkage and potential self-disruption due to chaotic f-mode exci
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2

Boss, Alan P. "Metallicity and Planet Formation: Models." Proceedings of the International Astronomical Union 5, S265 (2009): 391–98. http://dx.doi.org/10.1017/s1743921310001067.

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AbstractPlanets typically are considerably more metal-rich than even the most metal-rich stars, one indication that planet formation must differ greatly from star formation. There is general agreement that terrestrial planets form by the collisional accumulation of solids composed of heavy elements in the inner regions of protoplanetary disks. Two competing mechanisms exist for the formation of giant planets, core accretion and disk instability, though hybrid combinations are possible as well. In core accretion, a higher metallicity in the protoplanetary disk leads directly to larger core mass
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3

Guenel, M., S. Mathis, and F. Remus. "Unravelling tidal dissipation in gaseous giant planets." Astronomy & Astrophysics 566 (June 2014): L9. http://dx.doi.org/10.1051/0004-6361/201424010.

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4

Carleo, Ilaria, Paolo Giacobbe, Gloria Guilluy, et al. "The GAPS Programme at TNG XXXIX. Multiple Molecular Species in the Atmosphere of the Warm Giant Planet WASP-80 b Unveiled at High Resolution with GIANO-B ∗." Astronomical Journal 164, no. 3 (2022): 101. http://dx.doi.org/10.3847/1538-3881/ac80bf.

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Abstract Detections of molecules in the atmosphere of gas giant exoplanets allow us to investigate the physico-chemical properties of the atmospheres. Their inferred chemical composition is used as tracer of planet formation and evolution mechanisms. Currently, an increasing number of detections is showing a possible rich chemistry of the hotter gaseous planets, but whether this extends to cooler giants is still unknown. We observed four transits of WASP-80 b, a warm transiting giant planet orbiting a late-K dwarf star with the near-infrared GIANO-B spectrograph installed at the Telescopio Naz
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5

Raymond, Sean N. "Terrestrial planet formation in extra-solar planetary systems." Proceedings of the International Astronomical Union 3, S249 (2007): 233–50. http://dx.doi.org/10.1017/s1743921308016645.

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AbstractTerrestrial planets form in a series of dynamical steps from the solid component of circumstellar disks. First, km-sized planetesimals form likely via a combination of sticky collisions, turbulent concentration of solids, and gravitational collapse from micron-sized dust grains in the thin disk midplane. Second, planetesimals coalesce to form Moon- to Mars-sized protoplanets, also called “planetary embryos”. Finally, full-sized terrestrial planets accrete from protoplanets and planetesimals. This final stage of accretion lasts about 10-100 Myr and is strongly affected by gravitational
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6

Boss, Alan P. "Modes of Gaseous Planet Formation." Symposium - International Astronomical Union 202 (2004): 141–48. http://dx.doi.org/10.1017/s0074180900217725.

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The discovery of gas giant planets around nearby stars has launched a new era in our understanding of the formation and evolution of planetary systems. However, none of the over four dozen companions detected to date strongly resembles Jupiter or Saturn: their inferred masses range from sub-Saturn-mass to 10 Jupiter-masses or more, while their orbits extend from periods of a few days to a few years. Given this situation, it seems prudent to re-examine mechanisms for gas giant planet formation. The two extreme cases are top-down or bottom-up. The latter is the core accretion mechanism, long fav
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7

Mayor, M., D. Naef, F. Pepe, et al. "HD 83443: a system with two Saturns." Symposium - International Astronomical Union 202 (2004): 84–86. http://dx.doi.org/10.1017/s0074180900217543.

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We report the discovery of an extrasolar planetary system with two Saturnian planets around the star HD 83443. The new planetary system is unusual by more than one aspect, as it contains two very low–mass gaseous giant planets, both on very tight orbits. Among the planets detected so far, the inner planet has the smallest semi–major axis (0.038 AU) and period (2.985 days) whereas the outer planet is the lightest one with m2 sin i = 0.53 MSat. A preliminary dynamical study confirms the stability of the system.
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8

Masset, Frédéric S. "Planetary migration in gaseous protoplanetary disks." Proceedings of the International Astronomical Union 3, S249 (2007): 331–46. http://dx.doi.org/10.1017/s1743921308016797.

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AbstractTides come from the fact that different parts of a system do not fall in exactly the same way in a non-uniform gravity field. In the case of a protoplanetary disk perturbed by an orbiting, prograde protoplanet, the protoplanet tides raise a wake in the disk which causes the orbital elements of the planet to change over time. The most spectacular result of this process is a change in the protoplanet's semi-major axis, which can decrease by orders of magnitude on timescales shorter than the disk lifetime. This drift in the semi-major axis is called planetary migration. In a first part, w
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9

Bitsch, Bertram, Andre Izidoro, Anders Johansen, et al. "Formation of planetary systems by pebble accretion and migration: growth of gas giants." Astronomy & Astrophysics 623 (March 2019): A88. http://dx.doi.org/10.1051/0004-6361/201834489.

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Giant planets migrate though the protoplanetary disc as they grow their solid core and attract their gaseous envelope. Previously, we have studied the growth and migration of an isolated planet in an evolving disc. Here, we generalise such models to include the mutual gravitational interaction between a high number of growing planetary bodies. We have investigated how the formation of planetary systems depends on the radial flux of pebbles through the protoplanetary disc and on the planet migration rate. Our N-body simulations confirm previous findings that Jupiter-like planets in orbits outsi
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10

Hansen, Bradley M. S. "Formation of exoplanetary satellites by pull-down capture." Science Advances 5, no. 10 (2019): eaaw8665. http://dx.doi.org/10.1126/sciadv.aaw8665.

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The large size and wide orbit of the recently announced exomoon candidate Kepler-1625b-i are hard to explain within traditional theories of satellite formation. We show that these properties can be reproduced if the satellite began as a circumstellar co-orbital body with the original core of the giant planet Kepler-1625b. This body was then drawn down into a circumplanetary orbit during the rapid accretion of the giant planet gaseous envelope, a process termed “pull-down capture.” Our numerical integrations demonstrate the stability of the original configuration and the capture process. In thi
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11

Guilera, O. M., D. Swoboda, Y. Alibert, G. C. de Elía, P. J. Santamaría, and A. Brunini. "Planetesimal fragmentation and giant planet formation: the role of planet migration." Proceedings of the International Astronomical Union 9, S310 (2014): 204–7. http://dx.doi.org/10.1017/s1743921314008266.

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AbstractIn the standard model of core accretion, the cores of the giant planets form by the accretion of planetesimals. In this scenario, the evolution of the planetesimal population plays an important role in the formation of massive cores. Recently, we studied the role of planetesimal fragmentation in the in situ formation of a giant planet. However, the exchange of angular momentum between the planet and the gaseous disk causes the migration of the planet in the disk. In this new work, we incorporate the migration of the planet and study the role of planet migration in the formation of a ma
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12

Zain, P. S., G. C. de Elía, M. P. Ronco, and O. M. Guilera. "Planetary formation and water delivery in the habitable zone around solar-type stars in different dynamical environments." Astronomy & Astrophysics 609 (January 2018): A76. http://dx.doi.org/10.1051/0004-6361/201730848.

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Context. Observational and theoretical studies suggest that there are many and various planetary systems in the Universe. Aims. We study the formation and water delivery of planets in the habitable zone (HZ) around solar-type stars. In particular, we study different dynamical environments that are defined by the most massive body in the system. Methods. First of all, a semi-analytical model was used to define the mass of the protoplanetary disks that produce each of the five dynamical scenarios of our research. Then, we made use of the same semi-analytical model to describe the evolution of em
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13

Raymond, Sean N., and Alessandro Morbidelli. "The Grand Tack model: a critical review." Proceedings of the International Astronomical Union 9, S310 (2014): 194–203. http://dx.doi.org/10.1017/s1743921314008254.

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AbstractThe “Grand Tack” model proposes that the inner Solar System was sculpted by the giant planets' orbital migration in the gaseous protoplanetary disk. Jupiter first migrated inward then Jupiter and Saturn migrated back outward together. If Jupiter's turnaround or “tack” point was at ~ 1.5 AU the inner disk of terrestrial building blocks would have been truncated at ~ 1 AU, naturally producing the terrestrial planets' masses and spacing. During the gas giants' migration the asteroid belt is severely depleted but repopulated by distinct planetesimal reservoirs that can be associated with t
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14

Valletta, Claudio, and Ravit Helled. "An approximation for the capture radius of gaseous protoplanets." Monthly Notices of the Royal Astronomical Society: Letters 507, no. 1 (2021): L62—L66. http://dx.doi.org/10.1093/mnrasl/slab089.

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ABSTRACT Determining the heavy-element accretion rate of growing giant planets is crucial for understanding their formation and bulk composition. The solid (heavy-element) accretion rate should be carefully modelled during the various stages of giant planet formation and therefore the planetary capture radius must be determined. In some simulations that model the heavy-element accretion rate, such as in N-body simulations, the presence of the gaseous envelope is either neglected or treated in an oversimplified manner. In this paper, we present an approximation for the capture radius that does
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15

Li, S. L., C. Agnor, and D. N. C. Lin. "Giant impact, planetary merger, and diversity of planetary-core mass." Proceedings of the International Astronomical Union 3, S249 (2007): 301–3. http://dx.doi.org/10.1017/s1743921308016736.

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AbstractTransit observations indicate a large dispersion in the internal structure among the known gas giants. This is a big challenge to the conventional sequential planetary formation scenario because the diversity is inconsistent with the expectation of some well defined critical condition for the onset of gas accretion in this scenario. We suggest that giant impacts may lead to the merger of planets or the accretion of planetary embryos and cause the diversity of the core mass. By using an SPH scheme, we show that direct parabolic collisions generally lead to the total coalescence of impin
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16

Cadman, James, Ken Rice, and Cassandra Hall. "AB Aurigae: possible evidence of planet formation through the gravitational instability." Monthly Notices of the Royal Astronomical Society 504, no. 2 (2021): 2877–88. http://dx.doi.org/10.1093/mnras/stab905.

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ABSTRACT Recent observations of the protoplanetary disc surrounding AB Aurigae have revealed the possible presence of two giant planets in the process of forming. The young measured age of 1–4 Myr for this system allows us to place strict time constraints on the formation histories of the observed planets. Hence, we may be able to make a crucial distinction between formation through core accretion (CA) or the gravitational instability (GI), as CA formation time-scales are typically Myr whilst formation through GI will occur within the first ≈104–105 yr of disc evolution. We focus our analysis
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17

Barge, P., and R. Pellat. "From Planetoids to Planets." Highlights of Astronomy 9 (1992): 367–74. http://dx.doi.org/10.1017/s1539299600009205.

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A common origin of the sun and the planets from the collapse of interstellar gas is now widely accepted. Regardless of how stars form, which is considered as the previous step of the whole story, the starting point is a flattened rotating cloud containing a mixture of dusts and gas (the so called Kant-Laplace Nebula). On the other hand the observations of young solar-mass stars show with increasing evidence that the gas is dispersed away on a time scale less than 107 years and this provides us with a clear time constraint for model building since the formation of the giant gaseous planets have
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18

Izidoro, Andre, and Laurette Piani. "Origin of Water in the Terrestrial Planets: Insights from Meteorite Data and Planet Formation Models." Elements 18, no. 3 (2022): 181–86. http://dx.doi.org/10.2138/gselements.18.3.181.

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Water condensed as ice beyond the water snowline, the location in the Sun’s natal gaseous disk where temperatures were below 170 K. As the disk evolved and cooled, the snowline moved inwards. A low temperature in the terrestrial planet-forming region is unlikely to be the origin of water on the planets, and the distinct isotopic compositions of planetary objects formed in the inner and outer disks suggest limited early mixing of inner and outer Solar System materials. Water in our terrestrial planets has rather been derived from H-bearing materials indigenous to the inner disk and delivered by
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19

Wang, Su, and D. N. C. Lin. "Dynamical Evolution of Closely Packed Multiple Planetary Systems Subject to Atmospheric Mass Loss." Astronomical Journal 165, no. 4 (2023): 174. http://dx.doi.org/10.3847/1538-3881/acc070.

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Abstract A gap in exoplanets’ radius distribution has been widely attributed to the photoevaporation threshold of their progenitors’ gaseous envelope. Giant impacts can also lead to substantial mass loss. The outflowing gas endures tidal torque from the planets and their host stars. Alongside the planet–star tidal and magnetic interaction, this effect leads to planets’ orbital evolution. In multiple super-Earth systems, especially in those that are closely spaced and/or contain planets locked in mean motion resonances, modest mass loss can lead to dynamical instabilities. In order to place som
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20

Brügger, N., R. Burn, G. A. L. Coleman, Y. Alibert, and W. Benz. "Pebbles versus planetesimals." Astronomy & Astrophysics 640 (August 2020): A21. http://dx.doi.org/10.1051/0004-6361/202038042.

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Context. In the core accretion scenario of giant planet formation, a massive core forms first and then accretes a gaseous envelope. In the discussion of how this core forms, some divergences appear. The first scenarios of planet formation predict the accretion of kilometre-sized bodies called planetesimals, while more recent works suggest growth by the accretion of pebbles, which are centimetre-sized objects. Aims. These two accretion models are often discussed separately and our aim here is to compare the outcomes of the two models with identical initial conditions. Methods. The comparison is
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21

Fortney, Jonathan J. "Two Classes of Hot Jupiter Atmospheres." Proceedings of the International Astronomical Union 4, S253 (2008): 247–53. http://dx.doi.org/10.1017/s174392130802646x.

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AbstractWe highlight the potential importance of gaseous TiO and VO opacity on the highly irradiated close-in giant planets. The day-side atmospheres of these planets may naturally fall into two classes that are somewhat analogous to the M- and L-type dwarfs. Those that are warm enough to have appreciable opacity due to TiO and VO gases we term the “pM Class” planets, and those that are cooler, such that Ti and V are predominantly in solid condensates, we term “pL Class” planets. The optical spectra of pL Class planets are dominated by neutral atomic Na and K absorption. We discuss a connectio
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22

Poon, Sanson T. S., Richard P. Nelson, Seth A. Jacobson, and Alessandro Morbidelli. "Formation of compact systems of super-Earths via dynamical instabilities and giant impacts." Monthly Notices of the Royal Astronomical Society 491, no. 4 (2019): 5595–620. http://dx.doi.org/10.1093/mnras/stz3296.

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ABSTRACT The NASA’s Kepler mission discovered ∼700 planets in multiplanet systems containing three or more transiting bodies, many of which are super-Earths and mini-Neptunes in compact configurations. Using N-body simulations, we examine the in situ, final stage assembly of multiplanet systems via the collisional accretion of protoplanets. Our initial conditions are constructed using a subset of the Kepler five-planet systems as templates. Two different prescriptions for treating planetary collisions are adopted. The simulations address numerous questions: Do the results depend on the accreti
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23

Lambrechts, M., E. Lega, R. P. Nelson, A. Crida, and A. Morbidelli. "Quasi-static contraction during runaway gas accretion onto giant planets." Astronomy & Astrophysics 630 (September 24, 2019): A82. http://dx.doi.org/10.1051/0004-6361/201834413.

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Gas-giant planets, like Jupiter and Saturn, acquire massive gaseous envelopes during the approximately 3 Myr-long lifetimes of protoplanetary discs. In the core accretion scenario, the formation of a solid core of around ten Earth masses triggers a phase of rapid gas accretion. Previous 3D grid-based hydrodynamical simulations found that runaway gas accretion rates correspond to approximately 10 to 100 Jupiter masses per Myr. Such high accretion rates would result in all planets with larger than ten Earth-mass cores to form Jupiter-like planets, which is in clear contrast to the ice giants in
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24

Zawadzki, Brianna, Daniel Carrera, and Eric B. Ford. "Rapid formation of super-Earths around low-mass stars." Monthly Notices of the Royal Astronomical Society 503, no. 1 (2021): 1390–406. http://dx.doi.org/10.1093/mnras/stab603.

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ABSTRACT NASA’s TESS mission is expected to discover hundreds of M dwarf planets. However, few studies focus on how planets form around low-mass stars. We aim to better characterize the formation process of M dwarf planets to fill this gap and aid in the interpretation of TESS results. We use ten sets of N-body planet formation simulations that vary in whether a gas disc is present, initial range of embryo semimajor axes, and initial solid surface density profile. Each simulation begins with 147 equal-mass embryos around a 0.2 solar mass star and runs for 100 Myr. We find that planets form rap
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25

Podolak, Morris, and Nader Haghighipour. "Planetesimal Capture by an Evolving Giant Gaseous Protoplanet." Proceedings of the International Astronomical Union 8, S293 (2012): 263–69. http://dx.doi.org/10.1017/s1743921313012957.

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AbstractBoth the core-accretion and disk-instability models suggest that at the last stage of the formation of a gas-giant, the core of this object is surrounded by an extended gaseous envelope. At this stage, while the envelope is contracting, planetesimals from the protoplanetary disk may be scattered into the protoplanets atmosphere and deposit some or all of their materials as they interact with the gas. We have carried out extensive simulations of approximately 104 planetesimals interacting with a envelope of a Jupiter-mass protoplanet including effects of gas drag, heating, and the effec
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26

Cortés, C. C., D. Minniti, and S. Villanova. "Search for exoplanetary transits in the Galactic bulge." Monthly Notices of the Royal Astronomical Society 485, no. 4 (2019): 4502–8. http://dx.doi.org/10.1093/mnras/sty3224.

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ABSTRACT A search for extrasolar planetary transits using extended Kepler mission (K2) campaigns 9 and 11 revealed five new candidates towards the Galactic bulge. The stars EPIC 224439122, 224560837, 227560005, 230778501 and 231635524 are found to have low-amplitude transits consistent with extrasolar planets, with periods P = 35.1695, 3.6390, 12.4224, 17.9856 and 5.8824 days, respectively. The K2 data and existing optical photometry are combined with multi-band near-IR photometry of the Vista Variables in the Via Lactea (VVV) survey and Two-Micron All-Sky Survey (2MASS) in order to measure ac
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27

Veras, Dimitri, Pier-Emmanuel Tremblay, J. J. Hermes, et al. "Constraining planet formation around 6–8 M⊙ stars." Monthly Notices of the Royal Astronomical Society 493, no. 1 (2020): 765–75. http://dx.doi.org/10.1093/mnras/staa241.

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ABSTRACT Identifying planets around O-type and B-type stars is inherently difficult; the most massive known planet host has a mass of only about $3\, \mathrm{M}_{\odot }$. However, planetary systems which survive the transformation of their host stars into white dwarfs can be detected via photospheric trace metals, circumstellar dusty and gaseous discs, and transits of planetary debris crossing our line of sight. These signatures offer the potential to explore the efficiency of planet formation for host stars with masses up to the core-collapse boundary at $\approx 8\, \mathrm{M}_{\odot }$, a
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28

Boley, Aaron C., and Richard H. Durisen. "On the possibility of enrichment and differentiation in gas giants during birth by disk instability." Proceedings of the International Astronomical Union 6, S276 (2010): 401–2. http://dx.doi.org/10.1017/s1743921311020527.

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AbstractWe investigate the coupling between solids and gas during the formation of gas giant planets by disk fragmentation in the outer regions of massive disks. We find that fragments can become differentiated at birth. Even if an entire clump does not survive, differentiation could create solids cores that survive to accrete gaseous envelopes later.
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29

Chametla, Raúl O., Gennaro D’Angelo, Mauricio Reyes-Ruiz, and F. Javier Sánchez-Salcedo. "Capture and migration of Jupiter and Saturn in mean motion resonance in a gaseous protoplanetary disc." Monthly Notices of the Royal Astronomical Society 492, no. 4 (2020): 6007–18. http://dx.doi.org/10.1093/mnras/staa260.

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ABSTRACT We study the dynamical evolution of Jupiter and Saturn embedded in a gaseous, solar nebula-type disc by means of hydrodynamics simulations with the fargo2d1d code. We study the evolution for different initial separations of the planets’ orbits, ΔaSJ, to investigate whether they become captured in mean motion resonance (MMR) and the direction of the subsequent migration of the planet (inwards or outwards). We also provide an assessment of the planet’s orbital dynamics at different epochs of Saturn’s growth. We find that the evolution of initially compact orbital configurations is depen
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30

Kretke, Katherine A., D. N. C. Lin, and Neal J. Turner. "Planet formation around intermediate mass stars." Proceedings of the International Astronomical Union 3, S249 (2007): 293–300. http://dx.doi.org/10.1017/s1743921308016724.

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AbstractWe present a mechanism by which gas giants form efficiently around intermediate mass stars. MRI-driven turbulence effectively drives angular momentum transport in regions of the disk with sufficiently high ionization fraction. In the inner regions of the disk, where the midplane temperature is above ∼1000K, thermal ionization effectively couples the disk to the magnetic field, providing a relatively large viscosity. A pressure maximum will develop outside of this region as the gaseous disk approaches a steady-state surface density profile, trapping migrating solid material. This rocky
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31

Dutrey, Anne. "Millimetre/Sub-millimetre Observations of Circumstellar Disks." Proceedings of the International Astronomical Union 7, S280 (2011): 103–13. http://dx.doi.org/10.1017/s1743921311024902.

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AbstractTTauri disks located in nearby star-forming regions (e.g. Taurus-Auriga at 140 pc) are thought to be the site of planet formation, since proto-planetary disks orbiting around active (still accreting) TTauri stars should contain, in many cases, enough gas to form giant gaseous planets. As such, circumstellar disks are ideal laboratories to study planet formation, provided the gas and dust observations have enough sensitivity and resolving power. I will focus in these proceedings, on recent results of molecular observations which unveil the physical conditions of gas disks and reveal the
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32

Brügger, N., Y. Alibert, S. Ataiee, and W. Benz. "Metallicity effect and planet mass function in pebble-based planet formation models." Astronomy & Astrophysics 619 (November 2018): A174. http://dx.doi.org/10.1051/0004-6361/201833347.

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Context. One of the main scenarios of planet formation is the core accretion model where a massive core forms first and then accretes a gaseous envelope. This core forms by accreting solids, either planetesimals or pebbles. A key constraint in this model is that the accretion of gas must proceed before the dissipation of the gas disc. Classical planetesimal accretion scenarios predict that the time needed to form a giant planet’s core is much longer than the time needed to dissipate the disc. This difficulty led to the development of another accretion scenario, in which cores grow by accretion
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33

Ronnet, T., and A. Johansen. "Formation of moon systems around giant planets." Astronomy & Astrophysics 633 (January 2020): A93. http://dx.doi.org/10.1051/0004-6361/201936804.

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The four major satellites of Jupiter, known as the Galilean moons, and Saturn’s most massive satellite, Titan, are believed to have formed in a predominantly gaseous circum-planetary disk during the last stages of formation of their parent planet. Pebbles from the protoplanetary disk are blocked from flowing into the circumplanetary disk by the positive pressure gradient at the outer edge of the planetary gap, so the gas drag assisted capture of planetesimals should be the main contributor to the delivery of solids onto circum-planetary disks. However, a consistent framework for the subsequent
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34

Nayakshin, S. "The paradox of youth for ALMA planet candidates." Monthly Notices of the Royal Astronomical Society 493, no. 2 (2020): 2910–25. http://dx.doi.org/10.1093/mnras/staa246.

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ABSTRACT Recent ALMA observations indicate that the majority of bright protoplanetary discs show signatures of young moderately massive planets. I show that this result is paradoxical. The planets should evolve away from their observed states by radial migration and gas accretion in about 1 per cent of the system age. These systems should then hatch tens of giant planets in their lifetime, and there should exist a very large population of bright planet-less discs; none of this is observationally supported. An alternative scenario, in which the population of bright ALMA discs is dominated by se
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35

Pontin, C. M., A. J. Barker, R. Hollerbach, Q. André, and S. Mathis. "Wave propagation in semiconvective regions of giant planets." Monthly Notices of the Royal Astronomical Society 493, no. 4 (2020): 5788–806. http://dx.doi.org/10.1093/mnras/staa664.

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ABSTRACT Recent observations of Jupiter and Saturn suggest that heavy elements may be diluted in the gaseous envelope, providing a compositional gradient that could stabilize ordinary convection and produce a stably stratified layer near the core of these planets. This region could consist of semiconvective layers with a staircase-like density profile, which have multiple convective zones separated by thin stably stratified interfaces, as a result of double-diffusive convection. These layers could have important effects on wave propagation and tidal dissipation that have not been fully explore
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36

Guenel, M., S. Mathis, and F. Remus. "Understanding tidal dissipation in gaseous giant planets from their core to their surface." EPJ Web of Conferences 101 (2015): 06029. http://dx.doi.org/10.1051/epjconf/201510106029.

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37

Humphries, J., and S. Nayakshin. "On the origin of wide-orbit ALMA planets: giant protoplanets disrupted by their cores." Monthly Notices of the Royal Astronomical Society 489, no. 4 (2019): 5187–201. http://dx.doi.org/10.1093/mnras/stz2497.

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ABSTRACT Recent ALMA observations may indicate a surprising abundance of sub-Jovian planets on very wide orbits in protoplanetary discs that are only a few million years old. These planets are too young and distant to have been formed via the core accretion (CA) scenario, and are much less massive than the gas clumps born in the classical gravitational instability (GI) theory. It was recently suggested that such planets may form by the partial destruction of GI protoplanets: energy output due to the growth of a massive core may unbind all or most of the surrounding pre-collapse protoplanet. He
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38

Pirani, S., A. Johansen, B. Bitsch, A. J. Mustill, and D. Turrini. "Consequences of planetary migration on the minor bodies of the early solar system." Astronomy & Astrophysics 623 (March 2019): A169. http://dx.doi.org/10.1051/0004-6361/201833713.

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Pebble accretion is an efficient mechanism that is able to build up the core of the giant planets within the lifetime of the protoplanetary disc gas-phase. The core grows via this process until the protoplanet reaches its pebble isolation mass and starts to accrete gas. During the growth, the protoplanet undergoes a rapid, large-scale, inward migration due to the interactions with the gaseous protoplanetary disc. In this work, we have investigated how this early migration would have affected the minor body populations in our solar system. In particular, we focus on the Jupiter Trojan asteroids
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39

Luque, A., D. Dubrovin, F. J. Gordillo-Vázquez, et al. "Coupling between atmospheric layers in gaseous giant planets due to lightning-generated electromagnetic pulses." Journal of Geophysical Research: Space Physics 119, no. 10 (2014): 8705–20. http://dx.doi.org/10.1002/2014ja020457.

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40

Clement, Matthew S., Sean N. Raymond, and John E. Chambers. "Mercury as the Relic of Earth and Venus Outward Migration." Astrophysical Journal Letters 923, no. 1 (2021): L16. http://dx.doi.org/10.3847/2041-8213/ac3e6d.

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Abstract In spite of substantial advancements in simulating planet formation, the planet Mercury’s diminutive mass and isolated orbit and the absence of planets with shorter orbital periods in the solar system continue to befuddle numerical accretion models. Recent studies have shown that if massive embryos (or even giant planet cores) formed early in the innermost parts of the Sun’s gaseous disk, they would have migrated outward. This migration may have reshaped the surface density profile of terrestrial planet-forming material and generated conditions favorable to the formation of Mercury-li
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41

Dobbs-Dixon, Ian, ShuLin Li, and Douglas N. C. Lin. "Tidal barrier and the asymptotic mass of proto gas-giant planets." Proceedings of the International Astronomical Union 3, S249 (2007): 263–66. http://dx.doi.org/10.1017/s1743921308016670.

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AbstractAlthough late stage gap formation reduces the surface density in the vicinity of protoplanets, simulations suggest gas may continue to leak through the protoplanets tidal barrier, replenishing the gas supply and allowing protoplanets to acquire masses comparable to or larger than that of Jupiter. Global gas depletion is a possible explanation for gaseous planets with lower masses in weak-line T-Tauri disks and ice giants in our own solar system, but it is unlikely to have stalled the growth of multiple systems around nearby stars that contain relatively low-mass, close-in planets along
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42

Vines, Jose I., James S. Jenkins, Jack S. Acton, et al. "NGTS-6b: an ultrashort period hot-Jupiter orbiting an old K dwarf." Monthly Notices of the Royal Astronomical Society 489, no. 3 (2019): 4125–34. http://dx.doi.org/10.1093/mnras/stz2349.

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ABSTRACT We report the discovery of a new ultrashort period hot Jupiter from the Next Generation Transit Survey. NGTS-6b orbits its star with a period of 21.17 h, and has a mass and radius of $1.330^{+0.024}_{-0.028}$MJ and $1.271^{+0.197}_{-0.188}$RJ, respectively, returning a planetary bulk density of $0.711^{+0.214}_{-0.136}$ g cm−3. Conforming to the currently known small population of ultrashort period hot Jupiters, the planet appears to orbit a metal-rich star ([Fe/H] = +0.11 ± 0.09 dex). Photoevaporation models suggest the planet should have lost 5 per cent of its gaseous atmosphere ove
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43

Tinetti, Giovanna, Jonathan Tennyson, Caitlin A. Griffith, and Ingo Waldmann. "Water in exoplanets." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 370, no. 1968 (2012): 2749–64. http://dx.doi.org/10.1098/rsta.2011.0338.

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Exoplanets—planets orbiting around stars other than our own Sun—appear to be common. Significant research effort is now focused on the observation and characterization of exoplanet atmospheres. Species such as water vapour, methane, carbon monoxide and carbon dioxide have been observed in a handful of hot, giant, gaseous planets, but cooler, smaller planets such as Gliese 1214b are now analysable with current telescopes. Water is the key chemical dictating habitability. The current observations of water in exoplanets from both space and the ground are reviewed. Controversies surrounding the in
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44

Alam, Munazza K., James Kirk, Courtney D. Dressing, et al. "The First Near-infrared Transmission Spectrum of HIP 41378 f, A Low-mass Temperate Jovian World in a Multiplanet System." Astrophysical Journal Letters 927, no. 1 (2022): L5. http://dx.doi.org/10.3847/2041-8213/ac559d.

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Abstract We present a near-infrared transmission spectrum of the long-period (P = 542 days), temperate (T eq = 294 K) giant planet HIP 41378 f obtained with the Wide-Field Camera 3 instrument aboard the Hubble Space Telescope (HST). With a measured mass of 12 ± 3 M ⊕ and a radius of 9.2 ± 0.1 R ⊕, HIP 41378 f has an extremely low bulk density (0.09 ± 0.02 g cm−3). We measure the transit depth with a median precision of 84 ppm in 30 spectrophotometric channels with uniformly sized widths of 0.018 μm. Within this level of precision, the spectrum shows no evidence of absorption from gaseous molec
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45

D’Angelo, Gennaro, and Francesco Marzari. "Second-generation dust in planetary systems: the case of HD 163296." Monthly Notices of the Royal Astronomical Society 509, no. 3 (2021): 3181–93. http://dx.doi.org/10.1093/mnras/stab3220.

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ABSTRACT Observations indicate that large, dust-laden protoplanetary discs are common. Some features, like gaps, rings, and spirals, suggest they may host young planets, which can excite the orbits of nearby leftover planetesimals. Energetic collisions among these bodies can lead to the production of second-generation dust. Grains produced by collisions may have a dynamical behaviour different from that of first-generation, primordial dust out of which planetesimals and planets formed. We aim to study these differences for the HD 163296 system and determine whether dynamical signatures in the
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46

Mathis, S. "Tidal dissipation in stars and giant planets: Jean-Paul Zahn's pioneering work and legacy." EAS Publications Series 82 (2019): 5–33. http://dx.doi.org/10.1051/eas/1982002.

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In this lecture opening the session focused on tides in stellar and planetary systems, I will review the Jean-Paul Zahn's key contributions to the theory of tidal dissipation in stars and fluid planetary layers. I will first recall the general principles of tidal friction in celestial bodies. Then, I will focus on the theories of the stellar equilibrium and dynamical tides founded by Jean-Paul and their predictions for the evolution of binary stars. I will underline their essential legacy for ongoing studies of tidal dissipation in stars hosting planets and in fluid planetary regions. I will a
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47

Webb, John K., and Imma Wormleaton. "Could We Detect O2 in the Atmosphere of a Transiting Extra-solar Earth-like Planet?" Publications of the Astronomical Society of Australia 18, no. 3 (2001): 252–58. http://dx.doi.org/10.1071/as01037.

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AbstractAlthough the extra-solar planets discovered so far are of the giant, gaseous type, the increased sensitivity of future surveys will result in the discovery of lower mass planets. The detection of O2 in the atmosphere of a rocky extra-solar planet would be a potential indicator of life. In this paper we address the specific issue of whether we would be able to detect the O2 A-band absorption feature in the atmosphere of a planet similar to the Earth, if it were in orbit around a nearby star. Our method is empirical, in that we use observations of the Earth's O2 A-band, with a simple geo
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48

Mosqueira, Ignacio, and Paul R. Estrada. "Formation of the regular satellites of giant planets in an extended gaseous nebula II: satellite migration and survival." Icarus 163, no. 1 (2003): 232–55. http://dx.doi.org/10.1016/s0019-1035(03)00077-0.

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49

Bergez-Casalou, C., B. Bitsch, A. Pierens, A. Crida, and S. N. Raymond. "Influence of planetary gas accretion on the shape and depth of gaps in protoplanetary discs." Astronomy & Astrophysics 643 (November 2020): A133. http://dx.doi.org/10.1051/0004-6361/202038304.

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It is widely known that giant planets have the capacity to open deep gaps in their natal gaseous protoplanetary discs. It is unclear, however, how gas accretion onto growing planets influences the shape and depth of their growing gaps. We performed isothermal hydrodynamical simulations with the Fargo-2D1D code, which assumes planets accreting gas within full discs that range from 0.1 to 260 AU. The gas accretion routine uses a sink cell approach, in which different accretion rates are used to cope with the broad range of gas accretion rates cited in the literature. We find that the planetary g
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50

André, Q., S. Mathis, and A. J. Barker. "Layered semi-convection and tides in giant planet interiors." Astronomy & Astrophysics 626 (June 2019): A82. http://dx.doi.org/10.1051/0004-6361/201833674.

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Context. Recent Juno observations have suggested that the heavy elements in Jupiter could be diluted throughout a large fraction of its gaseous envelope, providing a stabilising compositional gradient over an extended region of the planet. This could trigger layered semi-convection, which, in the context of giant planets more generally, may explain Saturn’s luminosity excess and play a role in causing the abnormally large radii of some hot Jupiters. In giant planet interiors, it could take the form of density staircases, which are convective layers separated by thin stably stratified interface
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