From Warm Planets to Perpendicular Hot Planets. (arXiv:2108.09325v2 [astro-ph.EP] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Dawson_R/0/1/0/all/0/1">Rebekah I. Dawson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Albrecht_S/0/1/0/all/0/1">Simon H. Albrecht</a>
High eccentricity tidal migration (HEM) is a promising channel for the
origins of hot Jupiters and hot Neptunes. In the typical HEM scenario, a planet
forms beyond the ice line, but alternatively a planet can disk migrate or form
warm and undergo a short final stretch of HEM. At the warm origin point,
general relavistic precession can reduce the amplitude of Kozai-Lidov
oscillations driven by an outer companion. We show that warm planets that
achieve HEM under these conditions — and with common types of planetary and
stellar companions — tend to end up with near-polar spin-orbit alignments (psi
= 50-130 degrees) instead of concentrated at 40 and 140 degrees. Thus short
distance, GR-reduced HEM is a possible explanation for the observed population
of perpendicular planets.
High eccentricity tidal migration (HEM) is a promising channel for the
origins of hot Jupiters and hot Neptunes. In the typical HEM scenario, a planet
forms beyond the ice line, but alternatively a planet can disk migrate or form
warm and undergo a short final stretch of HEM. At the warm origin point,
general relavistic precession can reduce the amplitude of Kozai-Lidov
oscillations driven by an outer companion. We show that warm planets that
achieve HEM under these conditions — and with common types of planetary and
stellar companions — tend to end up with near-polar spin-orbit alignments (psi
= 50-130 degrees) instead of concentrated at 40 and 140 degrees. Thus short
distance, GR-reduced HEM is a possible explanation for the observed population
of perpendicular planets.
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