2.5D magnetohydrodynamic models of circumstellar discs around FS CMa post-mergers - I. Non-stationary accretion stage

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F23%3A10475678" target="_blank" >RIV/00216208:11320/23:10475678 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=cb.PC8sFgb" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=cb.PC8sFgb</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stad1796" target="_blank" >10.1093/mnras/stad1796</a>

Jazyk výsledku

angličtina

Název v původním jazyce

2.5D magnetohydrodynamic models of circumstellar discs around FS CMa post-mergers - I. Non-stationary accretion stage

Popis výsledku v původním jazyce

We investigate the dynamic evolution of the gaseous regions around FS CMa post-mergers. Owing to the slow rotation of the central B-type star, the dynamics is driven mainly by the magnetic field of the central star. Recent observations have allowed us to set realistic initial conditions, such as the magnetic field value (B-* approximate to 6 x 10(3) G), the mass of the central star (M-* = 6 M-circle dot), and the initial disc density rho(d0) is an element of [10(-13) g cm(-3), 10(-1)1 g cm(-3)]. We use the PLUTO code to perform 2.5D magnetohydrodynamic simulations of thin and thick disc models. Especially relevant for the interpretation of the observed properties of FS CMa post-mergers are the results for low-density discs, in which we find a jet emerging from the inner edge of the disc, as well as the formation of the so-called &apos;hot plasmoid&apos; in the coronal region. Jets are probably detected as discrete absorption components in the resonance lines of FS CMa stars. Moreover, the magnetic field configuration in the low-density plasma region favours the appearance of magnetocentrifugal winds from the disc. The currents towards the star created by the magnetic field may explain accidentally observed material infall. The disc structure is significantly changed owing to the presence of the magnetic field. The magnetic field is also responsible for the formation of a hot corona, as observed in several FS CMa stars through the Raman lines. Our results are valid for all magnetic stars surrounded by a low-density plasma, that is, by some stars showing the B[e] phenomenon.

Název v anglickém jazyce

2.5D magnetohydrodynamic models of circumstellar discs around FS CMa post-mergers - I. Non-stationary accretion stage

Popis výsledku anglicky

We investigate the dynamic evolution of the gaseous regions around FS CMa post-mergers. Owing to the slow rotation of the central B-type star, the dynamics is driven mainly by the magnetic field of the central star. Recent observations have allowed us to set realistic initial conditions, such as the magnetic field value (B-* approximate to 6 x 10(3) G), the mass of the central star (M-* = 6 M-circle dot), and the initial disc density rho(d0) is an element of [10(-13) g cm(-3), 10(-1)1 g cm(-3)]. We use the PLUTO code to perform 2.5D magnetohydrodynamic simulations of thin and thick disc models. Especially relevant for the interpretation of the observed properties of FS CMa post-mergers are the results for low-density discs, in which we find a jet emerging from the inner edge of the disc, as well as the formation of the so-called &apos;hot plasmoid&apos; in the coronal region. Jets are probably detected as discrete absorption components in the resonance lines of FS CMa stars. Moreover, the magnetic field configuration in the low-density plasma region favours the appearance of magnetocentrifugal winds from the disc. The currents towards the star created by the magnetic field may explain accidentally observed material infall. The disc structure is significantly changed owing to the presence of the magnetic field. The magnetic field is also responsible for the formation of a hot corona, as observed in several FS CMa stars through the Raman lines. Our results are valid for all magnetic stars surrounded by a low-density plasma, that is, by some stars showing the B[e] phenomenon.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA17-00871S" target="_blank" >GA17-00871S: Vlastnosti circumstelární látky u B[e] hvězd</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2023

Kód důvěrnosti údajů

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

Název periodika

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

1365-2966

Svazek periodika

523

Číslo periodika v rámci svazku

4

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

11

Strana od-do

5554-5564

Kód UT WoS článku

001023895800045

EID výsledku v databázi Scopus

2-s2.0-85164296662