Hydrodynamics and Survivability during Post-main-sequence Planetary Engulfment

Yarza, Ricardo; Razo-López, Naela B.; Murguia-Berthier, Ariadna; Everson, Rosa Wallace; Antoni, Andrea; MacLeod, Morgan; Soares-Furtado, Melinda; Lee, Dongwook; Ramirez-Ruiz, Enrico

doi:10.3847/1538-4357/acbdfc

Title: Hydrodynamics and Survivability during Post-main-sequence Planetary Engulfment

Journal Article · 05 September 2023 · The Astrophysical Journal

DOI: https://doi.org/10.3847/1538-4357/acbdfc · OSTI ID:2425037

^[1]; Razo-López, Naela B. ^[2];

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Univ. of California, Santa Cruz, CA (United States); Texas Advanced Computing Center, Austin, TX (United States); Univ. of Texas, Austin, TX (United States)
Univ. of California, Santa Cruz, CA (United States)
Univ. of California, Santa Cruz, CA (United States); Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Evanston, IL (United States)
University of California, Berkeley, CA (United States)
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
Univ. of Wisconsin, Madison, WI (United States)

The engulfment of substellar bodies (SBs), such as brown dwarfs and planets, by giant stars is a possible explanation for rapidly rotating giants, lithium-rich giants, and the presence of SBs in close orbits around subdwarfs and white dwarfs. We perform three-dimensional hydrodynamical simulations of the flow in the vicinity of an engulfed SB. We model the SB as a rigid body with a reflective surface because it cannot accrete. This reflective boundary changes the flow morphology to resemble that of engulfed compact objects with outflows. We measure the drag coefficients for the ram-pressure and gravitational drag forces acting on the SB, and use them to integrate its trajectory inside the star. We find that engulfment can increase the luminosity of a 1 M_⊙ star by up to a few orders of magnitude. The time for the star to return to its original luminosity is up to a few thousand years when the star has evolved to ≈10 R_⊙ and up to a few decades at the tip of the red giant branch (RGB). No SBs can eject the envelope of a 1 M_⊙ star before it evolves to ≈10 R_⊙ if the orbit of the SB is the only energy source contributing to the ejection. In contrast, SBs as small as ≈10 MJup can eject the envelope at the tip of the RGB. The numerical framework we introduce here can be used to study planetary engulfment in a simplified setting that captures the physics of the flow at the scale of the SB.

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Research Organization:: Univ. of Chicago, IL (United States). DOE NNSA-ASC OASCR Flash Center

Sponsoring Organization:: USDOE National Nuclear Security Administration (NNSA); National Science Foundation (NSF); Gordon and Betty Moore Foundation; National Aeronautics and Space Administration (NASA)

OSTI ID:: 2425037

Journal Information:: The Astrophysical Journal, Journal Name: The Astrophysical Journal Journal Issue: 2 Vol. 954; ISSN 0004-637X

Publisher:: IOP PublishingCopyright Statement

Country of Publication:: United States

Language:: English

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