Obliquity Tides on Hot Jupiters

2005/06/20 by Joshua N. Winn, Matthew J. Holman · 2 citations
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Stellar, planetary, and galactic studies #astro-ph

paper · pdf · doi:10.1086/432834

To appear in ApJ Letters [9 pages, 2 figures]

arxiv created 2005/06/20 · openalex publication_date 2005/07/15 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/04

Abstract

Obliquity tides are a potentially important source of heat for extrasolar planets on close-in orbits. Although tidal dissipation will usually reduce the obliquity to zero, a nonzero obliquity can persist if the planet is in a Cassini state, a resonance between spin precession and orbital precession. Obliquity tides might be the cause of the anomalously large size of the transiting planet HD 209458b.

Citations

• A Jupiter-mass companion to a solar-type star
• Evolutionary models for cool brown dwarfs and extrasolar giant planets. The case of HD 209458
• Measuring the Oblateness and Rotation of Transiting Extrasolar Giant Planets
• The Changing Face of the Extrasolar Giant Planet HD 209458b
• TrES-1: The Transiting Planet of a Bright K0 V Star
• Orbital Perturbations of Transiting Planets: A Possible Method to Measure Stellar Quadrupoles and to Detect Earth‐Mass Planets
• Tilting Saturn. I. Analytic Model

Cited by

• Tidal Evolution of Close‐in Extrasolar Planets
• Planet [wikipedia]