Journey to the center of the common envelope evolution: Inner dynamics of the post-dynamical inspiral

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F25%3A10505432" target="_blank" >RIV/00216208:11320/25:10505432 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=X7bZfjnUBP" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=X7bZfjnUBP</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202452616" target="_blank" >10.1051/0004-6361/202452616</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Journey to the center of the common envelope evolution: Inner dynamics of the post-dynamical inspiral

Popis výsledku v původním jazyce

Three-dimensional hydrodynamical simulations of common envelope evolution are often terminated soon after the initial dynamical plunge of the companion transitions into a long-lasting post-dynamical inspiral with a slowly varying semimajor axis, a(b). This premature termination is often due to insufficient numerical resolution and challenges associated with the softening of the gravitational potential of the two cores. In this work we used statically refined 3D hydrodynamical simulations to study non-accreting binaries orbiting inside a common envelope, exploring the effects of varying numerical resolution, delta, gravitational potential softening prescriptions, and the associated softening length scale, &amp; varepsilon;. We find that quantities such as the binary inspiral timescale or the volume-averaged shearing rate typically converge to asymptotic values only for &amp; varepsilon;&lt;= 0.1a(b) and delta &lt;= 6x10(-3)a(b), with smaller &amp; varepsilon; requiring correspondingly smaller delta. This suggests that many of the contemporary simulations could effectively be under-resolved. After a few tens of binary orbits, the two cores become surrounded by a corotating, nearly hydrostatic gas structure that resembles the shared envelope of a contact binary. We propose that this structure is responsible for the slowing of the dynamical inspiral, leading to an asymptotic inspiral timescale of approximately 10(5) orbital periods for a binary mass ratio q=1/3, and approximately 10(6) orbital periods for a binary mass ratio q=1. Even in the absence of magnetic fields, we observe intermittent polar outflows collimated by partially centrifugally evacuated polar funnels. We discuss the implications for the long-term evolution in the post-dynamical inspiral phase and the ultimate emergence of the post-common-envelope binary.

Název v anglickém jazyce

Journey to the center of the common envelope evolution: Inner dynamics of the post-dynamical inspiral

Popis výsledku anglicky

Three-dimensional hydrodynamical simulations of common envelope evolution are often terminated soon after the initial dynamical plunge of the companion transitions into a long-lasting post-dynamical inspiral with a slowly varying semimajor axis, a(b). This premature termination is often due to insufficient numerical resolution and challenges associated with the softening of the gravitational potential of the two cores. In this work we used statically refined 3D hydrodynamical simulations to study non-accreting binaries orbiting inside a common envelope, exploring the effects of varying numerical resolution, delta, gravitational potential softening prescriptions, and the associated softening length scale, &amp; varepsilon;. We find that quantities such as the binary inspiral timescale or the volume-averaged shearing rate typically converge to asymptotic values only for &amp; varepsilon;&lt;= 0.1a(b) and delta &lt;= 6x10(-3)a(b), with smaller &amp; varepsilon; requiring correspondingly smaller delta. This suggests that many of the contemporary simulations could effectively be under-resolved. After a few tens of binary orbits, the two cores become surrounded by a corotating, nearly hydrostatic gas structure that resembles the shared envelope of a contact binary. We propose that this structure is responsible for the slowing of the dynamical inspiral, leading to an asymptotic inspiral timescale of approximately 10(5) orbital periods for a binary mass ratio q=1/3, and approximately 10(6) orbital periods for a binary mass ratio q=1. Even in the absence of magnetic fields, we observe intermittent polar outflows collimated by partially centrifugally evacuated polar funnels. We discuss the implications for the long-term evolution in the post-dynamical inspiral phase and the ultimate emergence of the post-common-envelope binary.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

R - Projekt Ramcoveho programu EK

Rok uplatnění

2025

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astronomy &amp; Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Svazek periodika

697

Číslo periodika v rámci svazku

13 May 2025

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

22

Strana od-do

A68

Kód UT WoS článku

001487971400005

EID výsledku v databázi Scopus

2-s2.0-105005184678