Two Classes of Hot Jupiters [PDF]
The Astrophysical Journal, 2007 We identify two classes of transiting planet, based on their equilibrium temperatures and Safronov numbers. We examine various possible explanations for the dichotomy. It may reflect the influence of planet or planetesimal scattering in determining when planetary migration stops.
Brad M. S. Hansen, Travis Barman
openalex +6 more sources
Radiative equilibrium models of “hot Jupiters” [PDF]
Symposium - International Astronomical Union, 2004 We present an extension of our equilibrium model, initially applied to 51 Peg b (Goukenleuque et al. 2000), to other irradiated extrasolar planets with different orbital distances (up to 1 AU). The model yields the mean atmospheric thermal structure and predicts the reflected spectral flux as well as the thermal flux emerging from such planets, in the ...
C. Goukenleuque +2 more
openalex +3 more sources
Runaway Migration and the Formation of Hot Jupiters [PDF]
The Astrophysical Journal, 2003 Accepted for publication in ApJ.
F. Masset, J. C. B. Papaloizou
openalex +5 more sources
Hot Jupiters Have Giant Companions: Evidence for Coplanar High-eccentricity Migration [PDF]
Astrophysical Journal Letters, 2023 This study considers the characteristics of planetary systems with giant planets based on a population-level analysis of the California Legacy Survey planet catalog. We identified three characteristics common to hot Jupiters (HJs).
Jon K. Zink, A. Howard
semanticscholar +1 more source
Photochemical Hazes Dramatically Alter Temperature Structure and Atmospheric Circulation in 3D Simulations of Hot Jupiters [PDF]
Astrophysical Journal, 2023 Photochemical hazes are expected to form in hot Jupiter atmospheres and may explain the strong scattering slopes and muted spectral features observed in the transmission spectra of many hot Jupiters.
M. Steinrueck +7 more
semanticscholar +1 more source
Orbital Decay of Hot Jupiters due to Weakly Nonlinear Tidal Dissipation [PDF]
Astrophysical Journal, 2023 We study tidal dissipation in hot Jupiter host stars due to the nonlinear damping of tidally driven g-modes, extending the calculations of Essick & Weinberg to a wide variety of stellar host types.
N. Weinberg +5 more
semanticscholar +1 more source
TESS Transit Timing of Hundreds of Hot Jupiters [PDF]
Astrophysical Journal Supplement Series, 2022 We provide a database of transit times and updated ephemerides for 382 planets based on data from the NASA Transiting Exoplanet Survey Satellite (TESS) and previously reported transit times, which were scraped from the literature in a semiautomated ...
Ekaterina S. Ivshina, J. Winn
semanticscholar +1 more source
Origins of Hot Jupiters from the Stellar Obliquity Distribution [PDF]
Astrophysical Journal Letters, 2022 The obliquity of a star, or the angle between its spin axis and the average orbit normal of its companion planets, provides a unique constraint on that system’s evolutionary history. Unlike the solar system, where the Sun’s equator is nearly aligned with
M. Rice, Songhu Wang, G. Laughlin
semanticscholar +1 more source
Patchy Nightside Clouds on Ultra-hot Jupiters: General Circulation Model Simulations with Radiatively Active Cloud Tracers [PDF]
Astrophysical Journal, 2022 The atmospheres of ultra-hot Jupiters have been characterized in detail through recent phase curve and low- and high-resolution emission and transmission spectroscopic observations.
T. Komacek +3 more
semanticscholar +1 more source
Evidence for the Late Arrival of Hot Jupiters in Systems with High Host-star Obliquities [PDF]
Astronomical Journal, 2022 It has been shown that hot Jupiters systems with massive, hot stellar primaries exhibit a wide range of stellar obliquities. On the other hand, hot Jupiter systems with low-mass, cool primaries often have stellar obliquities close to zero.
J. Hamer, K. Schlaufman
semanticscholar +1 more source