Informace o publikaci

Magnetorotational instability in decretion disks of critically rotating stars and the outer structure of Be and Be/X-ray disks

Název česky Magnetorotační nestabilita v dekrečních discích kriticky rotujících hvězd a vnější struktura disků hvězd typu Beas
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KRTIČKA Jiří KURFÜRST Petr KRTIČKOVÁ Iva

Rok publikování 2015
Druh Článek v odborném periodiku
Časopis / Zdroj Astronomy and Astrophysics
Fakulta / Pracoviště MU

Přírodovědecká fakulta

Citace
www http://www.aanda.org/articles/aa/abs/2015/01/aa24867-14/aa24867-14.html
Doi http://dx.doi.org/10.1051/0004-6361/201424867
Obor Astronomie a nebeská mechanika, astrofyzika
Klíčová slova stars: mass-loss; stars: evolution; stars: rotation; hydrodynamics; magnetohydrodynamics
Popis Evolutionary models of fast-rotating stars show that the stellar rotational velocity may approach the critical speed. Critically rotating stars cannot spin up more, therefore they lose their excess angular momentum through an equatorial outflowing disk. The radial extension of such disks is unknown, partly because we lack information about the radial variations of the viscosity. We study the magnetorotational instability, which is considered to be the origin of anomalous viscosity in outflowing disks. We used analytic calculations to study the stability of outflowing disks submerged in the magnetic field. The magnetorotational instability develops close to the star if the plasma parameter is large enough. At large radii the instability disappears in the region where the disk orbital velocity is roughly equal to the sound speed. The magnetorotational instability is a plausible source of anomalous viscosity in outflowing disks. This is also true in the region where the disk radial velocity approaches the sound speed. The disk sonic radius can therefore be roughly considered as an effective outer disk radius, although disk material may escape from the star to the insterstellar medium. The radial profile of the angular momentum-loss rate already flattens there, consequently, the disk mass-loss rate can be calculated with the sonic radius as the effective disk outer radius. We discuss a possible observation determination of the outer disk radius by using Be and Be/X-ray binaries.
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