High-Eccentricity Migration with Disk-Induced Spin-Orbit Misalignment: a Preference for Perpendicular Hot Jupiters
Michelle Vick, Yubo Su, and Dong Lai

TL;DR
This paper investigates how disk-induced stellar obliquities influence high-eccentricity migration, revealing a preference for perpendicular hot Jupiters and explaining observed spin-orbit misalignments.
Contribution
It introduces a population synthesis model accounting for initial stellar obliquities from the protoplanetary disk phase, updating understanding of hot Jupiter misalignments.
Findings
Obliquity distribution peaks near 90 degrees.
Predominance of retrograde and perpendicular hot Jupiters.
Similarity to observed perpendicular planet systems.
Abstract
High-eccentricity migration is a likely formation mechanism for many observed hot Jupiters, particularly those with a large misalignment between the stellar spin axis and orbital angular momentum axis of the planet. In one version of high-eccentricity migration, an inclined stellar companion excites von Zeipel-Lidov-Kozai (ZLK) eccentricity oscillations of a cold Jupiter, and tidal dissipation causes the planet's orbit to shrink and circularize. Throughout this process, the stellar spin can evolve chaotically, resulting in highly misaligned hot Jupiters. Previous population studies of this migration mechanism have assumed that the stellar spin is aligned with the planetary orbital angular momentum when the companion begins to induce ZLK oscillations. However, in the presence of a binary companion, the star's obliquity may be significantly excited during the dissipation of its…
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