2.5D magnetohydrodynamic models of circumstellar discs around FS CMa post-mergers - I. Non-stationary accretion stage
The result's identifiers
Result code in 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>
Result on the web
<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>
Alternative languages
Result language
angličtina
Original language name
2.5D magnetohydrodynamic models of circumstellar discs around FS CMa post-mergers - I. Non-stationary accretion stage
Original language description
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 'hot plasmoid' 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.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
<a href="/en/project/GA17-00871S" target="_blank" >GA17-00871S: Properties of the circumstellar matter around B[e] stars</a><br>
Continuities
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)
Others
Publication year
2023
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Monthly Notices of the Royal Astronomical Society
ISSN
0035-8711
e-ISSN
1365-2966
Volume of the periodical
523
Issue of the periodical within the volume
4
Country of publishing house
GB - UNITED KINGDOM
Number of pages
11
Pages from-to
5554-5564
UT code for WoS article
001023895800045
EID of the result in the Scopus database
2-s2.0-85164296662