Post-dynamical inspiral phase of common envelope evolution Binary orbit evolution and angular momentum transport

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F23%3A10467333" target="_blank" >RIV/00216208:11320/23:10467333 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=8jkKl.f8jD" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=8jkKl.f8jD</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202346057" target="_blank" >10.1051/0004-6361/202346057</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Post-dynamical inspiral phase of common envelope evolution Binary orbit evolution and angular momentum transport

Popis výsledku v původním jazyce

After the companion dynamically plunges through the primary&apos;s envelope, the two cores remain surrounded by a common envelope and the decrease of the orbital period P-orb stalls. The subsequent evolution has never been systematically explored with multidimensional simulations. For this study, we performed 3D hydrodynamical simulations of an envelope evolving under the influence of a central binary star using an adaptively refined spherical grid. We followed the evolution over hundreds of orbits of the central binary to characterize the transport of angular momentum by advection, gravitational torques, turbulence, and viscosity. We find that local advective torques from the mean flow and Reynolds stresses associated with the turbulent flow dominate the angular momentum transport, which occurs outward in a disk-like structure about the orbital plane and inward along the polar axis. Turbulent transport is less efficient, but can locally significantly damp or enhance the net angular momentum radial transport and may even reverse its direction. Short-term variability in the envelope is remarkably similar to circumbinary disks, including the formation and destruction of lump-like overdensities, which enhance mass accretion and contribute to the outward transport of eccentricity generated in the vicinity of the binary. If the accretion onto the binary is allowed, the orbital decay timescale settles to a nearly constant value tau(b) similar to 10(3) to 10(4) P-orb, while preventing accretion leads to a slowly increasing tau(b) similar to 10(5) P-orb at the end of our simulations. Our results suggest that the post-dynamical orbital contraction and envelope ejection will slowly continue while the binary is surrounded by gas and that tau(b) is often much shorter than the thermal timescale of the envelope.

Název v anglickém jazyce

Post-dynamical inspiral phase of common envelope evolution Binary orbit evolution and angular momentum transport

Popis výsledku anglicky

After the companion dynamically plunges through the primary&apos;s envelope, the two cores remain surrounded by a common envelope and the decrease of the orbital period P-orb stalls. The subsequent evolution has never been systematically explored with multidimensional simulations. For this study, we performed 3D hydrodynamical simulations of an envelope evolving under the influence of a central binary star using an adaptively refined spherical grid. We followed the evolution over hundreds of orbits of the central binary to characterize the transport of angular momentum by advection, gravitational torques, turbulence, and viscosity. We find that local advective torques from the mean flow and Reynolds stresses associated with the turbulent flow dominate the angular momentum transport, which occurs outward in a disk-like structure about the orbital plane and inward along the polar axis. Turbulent transport is less efficient, but can locally significantly damp or enhance the net angular momentum radial transport and may even reverse its direction. Short-term variability in the envelope is remarkably similar to circumbinary disks, including the formation and destruction of lump-like overdensities, which enhance mass accretion and contribute to the outward transport of eccentricity generated in the vicinity of the binary. If the accretion onto the binary is allowed, the orbital decay timescale settles to a nearly constant value tau(b) similar to 10(3) to 10(4) P-orb, while preventing accretion leads to a slowly increasing tau(b) similar to 10(5) P-orb at the end of our simulations. Our results suggest that the post-dynamical orbital contraction and envelope ejection will slowly continue while the binary is surrounded by gas and that tau(b) is often much shorter than the thermal timescale of the envelope.

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

2023

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

674

Číslo periodika v rámci svazku

June

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

26

Strana od-do

A121

Kód UT WoS článku

001007989800005

EID výsledku v databázi Scopus

2-s2.0-85163170086