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Journal articles on the topic 'Planets'

Author: Grafiati

Published: 4 June 2021

Last updated: 25 July 2025

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1

Kokaia, Giorgi, Melvyn B. Davies, and Alexander J. Mustill. "Effects of capturing a wide-orbit planet on planetary systems: system stability and habitable zone bombardment rates." Monthly Notices of the Royal Astronomical Society 511, no. 2 (2021): 1685–93. http://dx.doi.org/10.1093/mnras/stab3659.

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ABSTRACT A large fraction of stars are formed in dense clusters. In the cluster, close encounters between stars at distances less than 100 au are common. It has been shown that during close encounters planets can transfer between stars. Such captured planets will be on different orbits compared to planets formed in the system, often on very wide, eccentric, and inclined orbits. We examine how these captured planets affect Kuiper belt-like planetesimal belts in their new systems by examining the effects on habitable planets in systems containing an outer gas giant. We show that these captured p

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2

Barr, Amy C., Vera Dobos, and László L. Kiss. "Interior structures and tidal heating in the TRAPPIST-1 planets." Astronomy & Astrophysics 613 (May 2018): A37. http://dx.doi.org/10.1051/0004-6361/201731992.

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Context. With seven planets, the TRAPPIST-1 system has among the largest number of exoplanets discovered in a single system so far. The system is of astrobiological interest, because three of its planets orbit in the habitable zone of the ultracool M dwarf. Aims. We aim to determine interior structures for each planet and estimate the temperatures of their rock mantles due to a balance between tidal heating and convective heat transport to assess their habitability. We also aim to determine the precision in mass and radius necessary to determine the planets’ compositions. Methods. Assuming the

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3

Jackson, Brian, Rory Barne, and Richard Greenberg. "Planetary Transits and Tidal Evolution." Proceedings of the International Astronomical Union 4, S253 (2008): 217–29. http://dx.doi.org/10.1017/s1743921308026434.

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AbstractTransiting planets are generally close enough to their host stars that tides may govern their orbital and thermal evolution. We present calculations of the tidal evolution of recently discovered transiting planets and discuss their implications. The tidal heating that accompanies this orbital evolution can be so great that it controls the planet's physical properties and may explain the large radii observed in several cases, including, for example, TrES-4. Also, since a planet's transit probability depends on its orbit, it evolves due to tides. Current values depend sensitively on the

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Franchini, Alessia, Rebecca G. Martin, and Stephen H. Lubow. "Multiplanet disc interactions in binary systems." Monthly Notices of the Royal Astronomical Society 491, no. 4 (2019): 5351–60. http://dx.doi.org/10.1093/mnras/stz3175.

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ABSTRACT We investigate the evolution of a multiplanet–disc system orbiting one component of a binary star system. The planet–disc system is initially coplanar but misaligned to the binary orbital plane. The planets are assumed to be giants that open gaps in the disc. We first study the role of the disc in shaping the mutual evolution of the two planets using a secular model for low initial tilt. In general, we find that the planets and the disc do not remain coplanar, in agreement with previous work on the single planet case. Instead, the planets and the disc undergo tilt oscillations. A high

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Schaefer, Laura K., and Vivien Parmentier. "The Air Over There: Exploring Exoplanet Atmospheres." Elements 17, no. 4 (2021): 257–63. http://dx.doi.org/10.2138/gselements.17.4.257.

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The atmospheric composition for a rocky exoplanet will depend strongly on the planet’s bulk composition and orbital position. Nontraditional gases may be present in the atmospheres of exceptionally hot planets. Atmospheres of more clement planets will depend on the abundance of volatiles acquired during planet formation and atmospheric removal processes, including escape, condensation, and reaction with the surface. To date, observations of exoplanet atmospheres have focused on giant planets, but future space-and ground-based observatories will revolutionize the precision and spectral resoluti

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6

Garrido-Deutelmoser, Juan, Cristobal Petrovich, Leonardo Krapp, Kaitlin M. Kratter, and Ruobing Dong. "Substructures in Protoplanetary Disks Imprinted by Compact Planetary Systems." Astrophysical Journal 932, no. 1 (2022): 41. http://dx.doi.org/10.3847/1538-4357/ac6bfd.

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Abstract The substructures observed in protoplanetary disks may be the signposts of embedded planets carving gaps or creating vortices. The inferred masses of these planets often fall in the Jovian regime despite their low abundance compared to lower-mass planets, partly because previous works often assume that a single substructure (a gap or vortex) is caused by a single planet. In this work, we study the possible imprints of compact systems composed of Neptune-like planets (∼10–30 M ⊕) and show that long-standing vortices are a prevalent outcome when their interplanetary separation (Δa) fall

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7

Howell, Steve B. "On the Value of High Precision Radial Velocity Observations and Astrometric Orbits for Binary Stars Hosting Exoplanets." Research Notes of the AAS 8, no. 9 (2024): 244. http://dx.doi.org/10.3847/2515-5172/ad7e23.

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Abstract Observations have concluded that exoplanet hosting binary stars appear to have wider mean separations than a definitive sample of “field binaries” as well as an apparent deficit of very close pairs. Many exoplanets orbit near their host stars equatorial plane, especially for close-in, small planets. Precision radial velocities of exoplanets in close binary stars are sparse but badly needed in order to provide statistical samples revealing the host stars spin axis and determinations of the masses and orbital planes of their planets. Astrometric orbits of the stars can provide precise b

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8

Kozhanov, T. S., and Nizyarov N. "Mathematical Theory of Motion of Revolving Axes on the Surface of Planets." International Astronomical Union Colloquium 178 (2000): 619–22. http://dx.doi.org/10.1017/s0252921100061790.

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Let a planet perform translational and rotational motions in the field of solar attraction. Let’s assume that the observer on the surface of the planet, knows (even approximately) an orbit and variations of orientation. It is necessary to clarify the motion of the instanteous rotation axis on the planet’s surface from the observer’s point of view on the planet’s surface.1. The coordinate system, to describe the translational and rotational motions of planets around the Sun we shall take into account the properties of orbits of solar system planets, namely: 1)All planets move in the same direct

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9

Maldonado, R. F., E. Villaver, A. J. Mustill, and M. Chávez. "Disentangling the parameter space: the role of planet multiplicity in triggering dynamical instabilities on planetary systems around white dwarfs." Monthly Notices of the Royal Astronomical Society 512, no. 1 (2022): 104–15. http://dx.doi.org/10.1093/mnras/stac481.

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ABSTRACT Planets orbiting intermediate- and low-mass stars are in jeopardy as their stellar hosts evolve to white dwarfs (WDs) because the dynamics of the planetary system changes due to the increase of the planet:star mass ratio after stellar mass-loss. In order to understand how the planet multiplicity affects the dynamical stability of post-main sequence (MS) systems, we perform thousands of N-body simulations involving planetary multiplicity as the variable and with a controlled physical and orbital parameter space:equal-mass planets; the same orbital spacing between adjacent planet’s pair

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10

Li, Gongjie. "Tilting Planets during Planet Scattering." Astrophysical Journal Letters 915, no. 1 (2021): L2. http://dx.doi.org/10.3847/2041-8213/ac0620.

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11

Fang, Julia, and Jean-Luc Margot. "PREDICTING PLANETS INKEPLERMULTI-PLANET SYSTEMS." Astrophysical Journal 751, no. 1 (2012): 23. http://dx.doi.org/10.1088/0004-637x/751/1/23.

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12

Rauer, Heike, and Artie Hatzes. "Extrasolar planets and planet formation." Planetary and Space Science 55, no. 5 (2007): 535. http://dx.doi.org/10.1016/j.pss.2006.09.001.

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13

Cloutier, R., N. Astudillo-Defru, X. Bonfils, et al. "Characterization of the L 98-59 multi-planetary system with HARPS." Astronomy & Astrophysics 629 (September 2019): A111. http://dx.doi.org/10.1051/0004-6361/201935957.

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Aims. L 98-59 (TIC 307210830, TOI-175) is a nearby M3 dwarf around which TESS revealed three small transiting planets (0.80, 1.35, 1.57 Earth radii) in a compact configuration with orbital periods shorter than 7.5 days. Here we aim to measure the masses of the known transiting planets in this system using precise radial velocity (RV) measurements taken with the HARPS spectrograph. Methods. We considered both trained and untrained Gaussian process regression models of stellar activity, which are modeled simultaneously with the planetary signals. Our RV analysis was then supplemented with dynami

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Gunell, Herbert, Romain Maggiolo, Hans Nilsson, et al. "Why an intrinsic magnetic field does not protect a planet against atmospheric escape." Astronomy & Astrophysics 614 (June 2018): L3. http://dx.doi.org/10.1051/0004-6361/201832934.

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The presence or absence of a magnetic field determines the nature of how a planet interacts with the solar wind and what paths are available for atmospheric escape. Magnetospheres form both around magnetised planets, such as Earth, and unmagnetised planets, like Mars and Venus, but it has been suggested that magnetised planets are better protected against atmospheric loss. However, the observed mass escape rates from these three planets are similar (in the approximate (0.5–2) kg s−1 range), putting this latter hypothesis into question. Modelling the effects of a planetary magnetic field on the

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15

Chen, Cheng, Rebecca G. Martin, Stephen H. Lubow, and C. J. Nixon. "Tilted Circumbinary Planetary Systems as Efficient Progenitors of Free-floating Planets." Astrophysical Journal Letters 961, no. 1 (2024): L5. http://dx.doi.org/10.3847/2041-8213/ad17c5.

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Abstract The dominant mechanism for generating free-floating planets has so far remained elusive. One suggested mechanism is that planets are ejected from planetary systems due to planet–planet interactions. Instability around a single star requires a very compactly spaced planetary system. We find that around binary star systems instability can occur even with widely separated planets that are on tilted orbits relative to the binary orbit due to combined effects of planet–binary and planet–planet interactions, especially if the binary is on an eccentric orbit. We investigate the orbital stabi

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16

Yu, Fangyuan, and Dong Lai. "Free-floating Planets, Survivor Planets, Captured Planets, and Binary Planets from Stellar Flybys." Astrophysical Journal 970, no. 1 (2024): 97. http://dx.doi.org/10.3847/1538-4357/ad4f81.

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Abstract In star clusters, close stellar encounters can strongly impact the architecture of a planetary system or even destroy it. We present a systematic study of the effects of stellar flybys on two-planet systems. When such a system experiences flybys, one or both planets can be ejected, forming free-floating planets (FFPs), captured planets (CPs) around the flyby star, and free-floating binary planets (BPs); the remaining single-surviving planets (SSPs) can have their orbital radii and eccentricities greatly changed. Through numerical experiments, we calculate the formation fractions (or b

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17

Marcy, Geoffrey W., R. Paul Butler, Steven S. Vogt, and Debra A. Fischer. "Extrasolar Planets and Prospects for Terrestrial Planets." Symposium - International Astronomical Union 213 (2004): 11–24. http://dx.doi.org/10.1017/s0074180900192903.

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Examination of ∼2000 sun–like stars has revealed 97 planets (as of 2002 Nov), all residing within our Milky Way Galaxy and within ∼200 light years of our Solar System. They have masses between 0.1 and 10 times that of Jupiter, and orbital sizes of 0.05–5 AU. Thus planets occupy the entire detectable domain of mass and orbits. News & summaries about extrasolar planets are provided at: http://exoplanets.org. These planets were all discovered by the wobble of the host stars, induced gravitationally by the planets, causing a periodicity in the measured Doppler effect of the starlight. Earth–ma

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18

Lee, Man Hoi, D. Fabrycky, and D. N. C. Lin. "Evidence for Solid Planets from Kepler's Near-Resonance Systems." Proceedings of the International Astronomical Union 8, S293 (2012): 100–105. http://dx.doi.org/10.1017/s1743921313012623.

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AbstractThe multiple-planet systems discovered by the Kepler mission show an excess of planet pairs with period ratios just wide of exact commensurability for first-order resonances like 2:1 and 3:2. In principle, these planet pairs could be in resonance if their orbital eccentricities are sufficiently small, because the width of first-order resonances diverges in the limit of vanishingly small eccentricity. We consider a widely-held scenario in which pairs of planets were captured into first-order resonances by migration due to planet-disk interactions, and subsequently became detached from t

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19

Marcy, Geoffrey W., and Andrew W. Howard. "The occurrence and the distribution of masses and radii of exoplanets." Proceedings of the International Astronomical Union 6, S276 (2010): 3–12. http://dx.doi.org/10.1017/s1743921311019867.

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AbstractWe analyze the statistics of Doppler-detected planets and Keplere-detected planet candidates of high integrity. We determine the number of planets per star as a function of planet mass, radius, and orbital period, and the occurrence of planets as a function of stellar mass. We consider only orbital periods less than 50 days around Solar-type (GK) stars, for which both Doppler and Kepler offer good completeness. We account for observational detection effects to determine the actual number of planets per star. From Doppler-detected planets discovered in a survey of 166 nearby G and K mai

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20

Bhatnagar, Alpana, Ramakant Marde, Gitika ., and Sudhendu Shekhar. "A RELATION BETWEEN ASTROLOGY AND AYURVEDA THROUGH NAVGRAH PLANTS: A REVIEW." International Journal of Research in Ayurveda and Pharmacy 16, no. 2 (2025): 169–71. https://doi.org/10.7897/2277-4343.16266.

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Yat Pinde Tat Bramhande this quotation states that all that is outside us is within us. The universe constitutes of various heavenly bodies which greatly affect humans. Stars and planets may it be individually or in association with themselves greatly impact the incidences in a human’s life, its intellect and health. The congregation of stars called Nakshatra, and the nine planets called navgraha that include the sun, Rahu and Ketu are studied for their effects on humans. As Ayurveda focuses on health and diseases, efforts should have been made to use it to neutralize the negative effects of t

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21

Nagasawa, Makiko, Shigeru Ida, and Taisuke Bessho. "The formation of close-in planets by the slingshot model." Proceedings of the International Astronomical Union 3, S249 (2007): 279–84. http://dx.doi.org/10.1017/s1743921308016700.

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AbstractWe investigated the efficiency of planet scatterings in producing close-in planets by a direct inclusion of the dynamical tide effect into the simulations. We considered a system consists of three Jovian planets. Through a planet-planet scattering, one of the planets is sent into shorter orbit. If the eccentricity of the scattered planet is enough high, the tidal dissipation from the star makes the planetary orbit circular. We found that the short-period planets are formed at about 30% cases in our simulation and that Kozai mechanism plays an important role. In the Kozai mechanism, the

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22

Velgas, Lev Borisovich, and Liia Lvovna Iavolinskaia. "Seven main discoveries, rigorously proven." Interactive science, no. 6 (40) (June 21, 2019): 103–5. http://dx.doi.org/10.21661/r-496981.

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We are striving to prove that all planets rotate around their axis due to their satellites. Rotation of the collateral gravitation is analogous for all the planets, for the Sun as well. The Sun, as well as every single planet, can have multiple satellites. Satellite and planet’s collateral gravitation, if it moves because of satellite’s movement around the orbit, rotates the planet or the Sun. The article proves that collateral gravitation of the Moon and the Earth, that moves around the Earth due to Moon’s movement around the Earth, rotates the Earth around it’s axis.

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23

Wilhelm, Caitlyn, Rory Barnes, Russell Deitrick, and Rachel Mellman. "The Ice Coverage of Earth-like Planets Orbiting FGK Stars." Planetary Science Journal 3, no. 1 (2022): 13. http://dx.doi.org/10.3847/psj/ac3b61.

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Abstract The photometric and spectroscopic signatures of habitable planets orbiting FGK stars may be modulated by surface ice coverage. To estimate its frequency and locations, we simulated the climates of hypothetical planets with a 1D energy balance model and assumed that the planets possess properties similar to modern Earth (mass, geography, atmosphere). We first simulated planets with fixed rotational axes and circular orbits, finding that the vast majority (≳ 90%) of planets with habitable surfaces are free of ice. For planets with partial ice coverage, the parameter space for ice caps (

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Sotiriadis, Sotiris, Anne-Sophie Libert, and Sean N. Raymond. "Formation of terrestrial planets in eccentric and inclined giant planet systems." Astronomy & Astrophysics 613 (May 2018): A59. http://dx.doi.org/10.1051/0004-6361/201731260.

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Aims. Evidence of mutually inclined planetary orbits has been reported for giant planets in recent years. Here we aim to study the impact of eccentric and inclined massive giant planets on the terrestrial planet formation process, and investigate whether it can possibly lead to the formation of inclined terrestrial planets. Methods. We performed 126 simulations of the late-stage planetary accretion in eccentric and inclined giant planet systems. The physical and orbital parameters of the giant planet systems result from n-body simulations of three giant planets in the late stage of the gas dis

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Fitzmaurice, Evan, David V. Martin, and Daniel C. Fabrycky. "Sculpting the circumbinary planet size distribution through resonant interactions with companion planets." Monthly Notices of the Royal Astronomical Society 512, no. 4 (2022): 5023–36. http://dx.doi.org/10.1093/mnras/stac741.

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ABSTRACT Resonant locking of two planets is an expected outcome of convergent disc migration. The planets subsequently migrate together as a resonant pair. In the context of circumbinary planets, the disc is truncated internally by the binary. If there were only a single planet, then this inner disc edge would provide a natural parking location. However, for two planets migrating together in resonance there will be a tension between the inner planet stopping at the disc edge and the outer planet continuing to be torqued inwards. In this paper, we study this effect, showing that the outcome is

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Navarro, Thomas, Timothy M. Merlis, Nicolas B. Cowan, and Natalya Gomez. "Atmospheric Gravitational Tides of Earth-like Planets Orbiting Low-mass Stars." Planetary Science Journal 3, no. 7 (2022): 162. http://dx.doi.org/10.3847/psj/ac76cd.

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Abstract Temperate terrestrial planets orbiting low-mass stars are subject to strong tidal forces. The effects of gravitational tides on the solid planet and that of atmospheric thermal tides have been studied, but the direct impact of gravitational tides on the atmosphere itself has so far been ignored. We first develop a simplified analytic theory of tides acting on the atmosphere of a planet. We then implement gravitational tides into a general circulation model of a static-ocean planet in a short-period orbit around a low-mass star—the results agree with our analytic theory. Because atmosp

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Kramm, Ulrike, Nadine Nettelmann, and Ronald Redmer. "Constraining planetary interiors with the Love number k2." Proceedings of the International Astronomical Union 6, S276 (2010): 482–84. http://dx.doi.org/10.1017/s1743921311020898.

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AbstractFor the solar sytem giant planets the measurement of the gravitational moments J2 and J4 provided valuable information about the interior structure. However, for extrasolar planets the gravitational moments are not accessible. Nevertheless, an additional constraint for extrasolar planets can be obtained from the tidal Love number k2, which, to first order, is equivalent to J2. k2 quantifies the quadrupolic gravity field deformation at the surface of the planet in response to an external perturbing body and depends solely on the planet's internal density distribution. On the other hand,

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Jackson, Brian, Richard Greenberg, and Rory Barnes. "Tidal evolution of close-in extra-solar planets." Proceedings of the International Astronomical Union 3, S249 (2007): 187–96. http://dx.doi.org/10.1017/s1743921308016591.

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AbstractThe distribution of eccentricities e of extra-solar planets with semi-major axes a > 0.2 AU is very uniform, and values for e are generally large. For a < 0.2 AU, eccentricities are much smaller (most e < 0.2), a characteristic widely attributed to damping by tides after the planets formed and the protoplanetary gas disk dissipated. We have integrated the classical coupled tidal evolution equations for e and a backward in time over the estimated age of each planet, and confirmed that the distribution of initial e values of close-in planets matches that of the general populatio

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Ricard, Yanick, and Frédéric Chambat. "Mass–Radius Relationships and Contraction of Condensed Planets by Cooling or Despinning." Astrophysical Journal 967, no. 2 (2024): 163. http://dx.doi.org/10.3847/1538-4357/ad4113.

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Abstract Condensed planets contract or expand as their temperature changes. With the exception of the effect of phase changes, this phenomenon is generally interpreted as being solely related to the thermal expansivity of the planet’s components. However, changes in density affect pressure and gravity and, consequently, the planet’s compressibility. A planet’s radius is also linked to its rate of rotation. Here again, changes in pressure, gravity, and compressibility are coupled. In this article we clarify how the radius of a condensed planet changes with temperature and rotation, using a simp

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Sikora, James, Jason Rowe, Saugata Barat, et al. "Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X." Astronomical Journal 165, no. 6 (2023): 250. http://dx.doi.org/10.3847/1538-3881/acc865.

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Abstract The early K-type T-Tauri star, V1298 Tau (V = 10 mag, age ≈ 20–30 Myr) hosts four transiting planets with radii ranging from 4.9 to 9.6 R ⊕. The three inner planets have orbital periods of ≈8–24 days while the outer planet’s period is poorly constrained by single transits observed with K2 and the Transiting Exoplanet Survey Satellite (TESS). Planets b, c, and d are proto–sub-Neptunes that may be undergoing significant mass loss. Depending on the stellar activity and planet masses, they are expected to evolve into super-Earths/sub-Neptunes that bound the radius valley. Here we present

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Louden, Emma M., Gregory P. Laughlin, and Sarah C. Millholland. "Tidal Dissipation Regimes among the Short-period Exoplanets." Astrophysical Journal Letters 958, no. 2 (2023): L21. http://dx.doi.org/10.3847/2041-8213/ad0843.

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Abstract The efficiency of tidal dissipation provides a zeroth-order link to a planet’s physical properties. For super-Earth and sub-Neptune planets in the range R ⊕ ≲ R p ≲ 4R ⊕, particularly efficient dissipation (i.e., low tidal quality factors) may signify terrestrial-like planets capable of maintaining rigid crustal features. Here, we explore global constraints on planetary tidal quality factors using a population of planets in multiple-planet systems whose orbital and physical properties indicate susceptibility to capture into secular spin–orbit resonances. Planets participating in secul

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Lazzoni, C., S. Desidera, F. Marzari, et al. "Dynamical models to explain observations with SPHERE in planetary systems with double debris belts." Astronomy & Astrophysics 611 (March 2018): A43. http://dx.doi.org/10.1051/0004-6361/201731426.

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Context. A large number of systems harboring a debris disk show evidence for a double belt architecture. One hypothesis for explaining the gap between the debris belts in these disks is the presence of one or more planets dynamically carving it. For this reason these disks represent prime targets for searching planets using direct imaging instruments, like the Spectro-Polarimetric High-constrast Exoplanet Research (SPHERE) at the Very Large Telescope.Aim. The goal of this work is to investigate this scenario in systems harboring debris disks divided into two components, placed, respectively, i

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Banik, Deepayan. "Planetary Rhythms: Synchronous Circulation on Variably Irradiated Asynchronous Planets." Astrophysical Journal 980, no. 2 (2025): 246. https://doi.org/10.3847/1538-4357/adabc4.

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Abstract Tidal locking of planets to their host stars results in an atmospheric circulation with a hotspot fixed to the frame of reference of the planet. On the other hand, asynchronously rotating planets feature moving hotspots either lagging or leading the corresponding substellar point as it translates along the surface. We show that a planet falling in the latter category could mimic the circulation of tidally synchronous planets under the influence of time-varying instellation, possibly provided by pulsating or multiple star systems. This happens when the planet’s diurnal period is in res

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Veras, Dimitri, Michael Efroimsky, Valeri V. Makarov, et al. "Orbital relaxation and excitation of planets tidally interacting with white dwarfs." Monthly Notices of the Royal Astronomical Society 486, no. 3 (2019): 3831–48. http://dx.doi.org/10.1093/mnras/stz965.

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Abstract Observational evidence of white dwarf planetary systems is dominated by the remains of exo-asteroids through accreted metals, debris discs, and orbiting planetesimals. However, exo-planets in these systems play crucial roles as perturbing agents, and can themselves be perturbed close to the white dwarf Roche radius. Here, we illustrate a procedure for computing the tidal interaction between a white dwarf and a near-spherical solid planet. This method determines the planet’s inward and/or outward drift, and whether the planet will reach the Roche radius and be destroyed. We avoid const

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35

Walsh, Kevin J. "Forming terrestrial planets and delivering water." Proceedings of the International Astronomical Union 11, A29B (2015): 427–30. http://dx.doi.org/10.1017/s174392131600572x.

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AbstractBuilding models capable of successfully matching the Terrestrial Planet's basic orbital and physical properties has proven difficult. Meanwhile, improved estimates of the nature of water-rich material accreted by the Earth, along with the timing of its delivery, have added even more constraints for models to match. While the outer Asteroid Belt seemingly provides a source for water-rich planetesimals, models that delivered enough of them to the still-forming Terrestrial Planets typically failed on other basic constraints - such as the mass of Mars.Recent models of Terrestrial Planet Fo

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Brasser, R., A. C. Barr, and V. Dobos. "The tidal parameters of TRAPPIST-1b and c." Monthly Notices of the Royal Astronomical Society 487, no. 1 (2019): 34–47. http://dx.doi.org/10.1093/mnras/stz1231.

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Abstract The TRAPPIST-1 planetary system consists of seven planets within 0.05 au of each other, five of which are in a multiresonant chain. These resonances suggest the system formed via planet migration; subsequent tidal evolution has damped away most of the initial eccentricities. We used dynamical N-body simulations to estimate how long it takes for the multiresonant configuration that arises during planet formation to break. From there we use secular theory to pose limits on the tidal parameters of planets b and c. We calibrate our results against multilayered interior models constructed

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S. GuimarÃ£es, Eduardo. "The Beginning of The Nuclear Universe and The Theory of Orbital Superconductivity of The Celestial Bodies." JOURNAL OF ADVANCES IN PHYSICS 14, no. 2 (2018): 5442–48. http://dx.doi.org/10.24297/jap.v14i2.7406.

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 This article is a logical and rational analysis of the original nuclear matter, and of the structure that gave rise to the space architecture of the universe with galaxies, stars, the system of planets and moons, and arrives to original and inedited conclusions. After the so-called Big Bang of the universe arose the space, a new time count and the nuclear universe, governed by the actions of the physical properties of nuclear superconductivity space. The actions of the physical properties of superconductivity nuclear matter generate the spatial phenomenon of orbital supercon

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Lissauer, Jack J. "Formation, Frequency and Spacing of Habitable Planets." International Astronomical Union Colloquium 161 (January 1997): 289–97. http://dx.doi.org/10.1017/s0252921100014809.

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AbstractModels of planet formation and of the orbital stability of planetary systems are described and used to discuss estimates of the abundance of habitable planets which may orbit stars within our galaxy. Modern theories of star and planet formation, which are based upon observations of the Solar System and of young stars and their environments, predict that most single stars should have rocky planets in orbit about them. Terrestrial planets are believed to grow via pairwise accretion until the spacing of planetary orbits becomes large enough that the configuration is stable for the age of

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Salazar, Andrea M., and Robin Wordsworth. "The Feasibility of Asynchronous Rotation via Thermal Tides for Diverse Atmospheric Compositions." Planetary Science Journal 5, no. 10 (2024): 218. http://dx.doi.org/10.3847/psj/ad74ef.

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Abstract The equilibrium rotation rate of a planet is determined by the sum of torques acting on its solid body. For planets with atmospheres, the dominant torques are usually the gravitational tide, which acts to slow the planet’s rotation rate, and the atmospheric thermal tide, which acts to spin up the planet. Previous work demonstrated that rocky planets with thick atmospheres may produce strong enough thermal tides to avoid tidal locking, but a study of how the strength of the thermal tide depends on atmospheric properties has not been done. In this work, we use a combination of simulatio

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Fabrycky, Daniel C. "What to Expect from Transiting Multiplanet Systems." Proceedings of the International Astronomical Union 4, S253 (2008): 173–79. http://dx.doi.org/10.1017/s1743921308026380.

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AbstractSo far radial velocity measurements have discovered ~25 stars to host multiple planets. The statistics imply that many of the known hosts of transiting planets should have additional planets, yet none have been solidly detected. They will be soon, via complementary search methods of RV, transit-time variations of the known planet, and transits of the additional planet. When they are found, what can transit measurements add to studies of multiplanet dynamical evolution? First, mutual inclinations become measurable, for comparison to the solar system's disk-like configuration. Such measu

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Dvorak, R., E. Pilat-Lohinger, E. Bois, B. Funk, F. Freistetter та L. Kiseleva-Eggleton. "Planets in Double Stars: The ϒ Cephei System". International Astronomical Union Colloquium 191 (серпень 2004): 222–26. http://dx.doi.org/10.1017/s0252921100008800.

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AbstractUp to now we have evidence for some 15 planets moving in double stars. They are all of the so-called S-type, which means that they are orbiting one of the primaries. Only two of the binaries have separations in the order of the distances where the planets in our Solar system orbit the Sun, namely Gliese 86 and ϒ Cep. In this study we investigate the stability of the recently discovered planet in ϒ Cep with respect to the orbital parameters of the binary and of the planet. Additionally we check the region inside and outside the planet’s orbit (a = 2.1 AU). Even when the mass of an addit

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Rosenthal, Lee J., Heather A. Knutson, Yayaati Chachan, et al. "The California Legacy Survey. III. On the Shoulders of (Some) Giants: The Relationship between Inner Small Planets and Outer Massive Planets." Astrophysical Journal Supplement Series 262, no. 1 (2022): 1. http://dx.doi.org/10.3847/1538-4365/ac7230.

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Abstract We use a high-precision radial velocity survey of FGKM stars to study the conditional occurrence of two classes of planets: close-in small planets (0.023–1 au, 2–30 M ⊕) and distant giant planets (0.23–10 au, 30–6000 M ⊕). We find that 41 − 13 + 15 % of systems with a close-in, small planet also host an outer giant, compared to 17.6 − 1.9 + 2.4 % for stars irrespective of small planet presence. This implies that small planet hosts may be enhanced in outer giant occurrences compared to all stars with 1.7σ significance. Conversely, we estimate that 42 − 13 + 17 % of cold giant hosts als

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Chen, Cheng, Rebecca G. Martin, and C. J. Nixon. "Can a binary star host three giant circumbinary planets?" Monthly Notices of the Royal Astronomical Society 525, no. 3 (2023): 3781–89. http://dx.doi.org/10.1093/mnras/stad2543.

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ABSTRACT We investigate the orbital stability of a tilted circumbinary planetary system with three giant planets. The planets are spaced by a constant number (Δ) of mutual Hill radii in the range Δ = 3.4–12.0 such that the period ratio of the inner pair is the same as that of the outer pair. A tilted circumbinary planetary system can be unstable even if the same system around a coplanar binary is stable. For an equal-mass binary, we find that the stability of a three-planet system is qualitatively similar to that of a two-planet system, but the three-planet system is more unstable in mean moti

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Taylor, Stuart F. "Flow of Planets Raises Short Period Fall-Off." Proceedings of the International Astronomical Union 8, S293 (2012): 241–43. http://dx.doi.org/10.1017/s174392131301291x.

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AbstractAfter finding more planets than expected at the shortest period, there has been an effort to explain their numbers by weak tidal friction. However, we find that the strength of tidal dissipation that would produce the occurence distribution found from Kepler planet candidates is different for giant versus medium radii planets. This discrepancy can be resolved if there is a “flow” of the largest planets regularly arriving such that they go through a “hot Jupiter” stage. We also show a correlation of higher stellar Fe/H with higher eccentricity of giant planets that may be from smaller p

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Lammers, Caleb, and Joshua N. Winn. "Discovery and Dynamics of the Nontransiting Planet Kepler-139f." Astrophysical Journal Letters 984, no. 2 (2025): L39. https://doi.org/10.3847/2041-8213/adce01.

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Abstract Among the ways that an outer giant planet can alter the architecture of an inner planetary system is by tilting the orbits of the inner planets and reducing their mutual transit probabilities. Here, we report on an example of this phenomenon: we show that the Kepler-139 system contains a nontransiting planet just exterior to three transiting planets and interior to a giant planet. This newly discovered planet, Kepler-139f, has an orbital period of 355 ± 2 days and a mass of 36 ± 10 M ⊕ based on transit-timing and radial-velocity data. Through dynamical simulations, we show that gravit

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Shin, In-Gu, Jennifer C. Yee, Weicheng Zang, et al. "Systematic KMTNet Planetary Anomaly Search. XI. Complete Sample of 2016 Subprime Field Planets." Astronomical Journal 167, no. 6 (2024): 269. http://dx.doi.org/10.3847/1538-3881/ad3ba3.

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Abstract Following Shin et al. (2023b), which is a part of the “Systematic KMTNet Planetary Anomaly Search” series (i.e., a search for planets in the 2016 KMTNet prime fields), we conduct a systematic search of the 2016 KMTNet subprime fields using a semi-machine-based algorithm to identify hidden anomalous events missed by the conventional by-eye search. We find four new planets and seven planet candidates that were buried in the KMTNet archive. The new planets are OGLE-2016-BLG-1598Lb, OGLE-2016-BLG-1800Lb, MOA-2016-BLG-526Lb, and KMT-2016-BLG-2321Lb, which show typical properties of microle

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Nixon, Matthew C., and Nikku Madhusudhan. "How deep is the ocean? Exploring the phase structure of water-rich sub-Neptunes." Monthly Notices of the Royal Astronomical Society 505, no. 3 (2021): 3414–32. http://dx.doi.org/10.1093/mnras/stab1500.

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ABSTRACT Understanding the internal structures of planets with a large H2O component is important for the characterization of sub-Neptune planets. The finding that the mini-Neptune K2-18b could host a liquid water ocean beneath a mostly hydrogen envelope motivates a detailed examination of the phase structures of water-rich planets. To this end, we present new internal structure models for super-Earths and mini-Neptunes that enable detailed characterization of a planet’s water component. We use our models to explore the possible phase structures of water worlds and find that a diverse range of

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Franson, Kyle, William O. Balmer, Brendan P. Bowler та ін. "JWST/NIRCam 4–5 μm Imaging of the Giant Planet AF Lep b". Astrophysical Journal Letters 974, № 1 (2024): L11. http://dx.doi.org/10.3847/2041-8213/ad736a.

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Abstract With a dynamical mass of 3 M Jup, the recently discovered giant planet AF Lep b is the lowest-mass imaged planet with a direct mass measurement. Its youth and spectral type near the L/T transition make it a promising target to study the impact of clouds and atmospheric chemistry at low surface gravities. In this work, we present JWST/NIRCam imaging of AF Lep b. Across two epochs, we detect AF Lep b in F444W (4.4 μm) with signal-to-noise ratios of 9.6 and 8.7, respectively. At the planet’s separation of 320 mas during the observations, the coronagraphic throughput is ≈7%, demonstrating

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Ford, Eric B., and Knicole D. Colón. "Characterizing the Eccentricities of Transiting Extrasolar Planets with Kepler and CoRoT." Proceedings of the International Astronomical Union 4, S253 (2008): 111–19. http://dx.doi.org/10.1017/s1743921308026306.

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AbstractRadial velocity planet searches have revealed that many giant planets have large eccentricities, in striking contrast with the giant planets in the solar system and prior theories of planet formation. The realization that many giant planets have large eccentricities raises a fundamental question: Do terrestrial-size planets of other stars typically have significantly eccentric orbits or nearly circular orbits like the Earth? While space-based missions such as CoRoT and Kepler will be capable of detecting nearly Earth-sized planets, it will be extremely challenging to measure their ecce

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Rogers, Leslie A. "Glimpsing the Compositions of Sub-Neptune-Size Exoplanets." Proceedings of the International Astronomical Union 8, S299 (2013): 247–51. http://dx.doi.org/10.1017/s1743921313008491.

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AbstractThe growing number of transiting planets with mass constraints opens the possibility of applying a statistical approach to learn about the underlying population of planet compositions. We focus on the intriguing transition between rocky exoplanets and planets with voluminous gas layers, and explore how the current census of sub-Neptune-size exoplanets constrains the maximum radii of rocky planets. We outline a hierarchical Bayesian model approach to infer the fraction of planets that are dense enough to be rocky (as a function of planet radius). A preliminary analysis of the current sa

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