Common envelope binary interaction simulations between a thermally pulsating AGB star and a low mass companion

Miguel González-Bolívar, Orsola De Marco*, Mike Y. M. Lau, Ryosuke Hirai, Daniel J. Price

*Corresponding author for this work

    Research output: Contribution to journalArticlepeer-review

    8 Citations (Scopus)
    69 Downloads (Pure)

    Abstract

    At least one in five of all planetary nebulae are the product of a common envelope (CE) interaction, where the companion in-spirals into the envelope of an asymptotic giant branch (AGB) star ejecting the nebula and leaving behind a compact binary. In this work we carry out 3D smoothed particle hydrodynamics simulations of the CE interaction between a 1.7 M AGB star and a 0.6 M companion. We model the AGB structure using a 1D stellar model taken at the seventh thermal pulse. The interaction takes place when the giant is on the expanding phase of the seventh thermal pulse and has a radius of 250 R. The post-CE orbital separations varies between 20 and 31 R, with the inclusion of recombination energy resulting in wider separations. Based on the observed short in-spiral time-scales, we suggest that thermal pulses can trigger CEs, extending the ability of AGB stars to capture companions into CEs, that would lead to the prediction of a larger population of post-AGB, post-CE binaries. Simulations that include a tabulated equation of state unbind a great deal more gas, likely unbinding the entire envelope on short time-scales. The shape of the CE after the in-spiral is more spherical for AGB than red giant branch stars, and even more so if recombination energy is included. We expect that the planetary nebula formed from this CE will have different features compared to those formed from red giant branch stars.

    Original languageEnglish
    Pages (from-to)3181-3199
    Number of pages19
    JournalMonthly Notices of the Royal Astronomical Society
    Volume517
    Issue number3
    DOIs
    Publication statusPublished - 1 Dec 2022

    Bibliographical note

    This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society, Volume 517, Issue 3, December 2022, Pages 3181–3199, https://doi.org/10.1093/mnras/stac2301. Copyright 2022 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

    Keywords

    • hydrodynamics
    • methods: numerical
    • stars: AGB

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