Catalogo Articoli (Spogli Riviste)
OPAC HELP
Titolo: Black hole X-ray transients: Mass accumulation in the disk - constraints for the viscosity
Autore: Meyer-Hofmeister, E; Meyer, F;
- Indirizzi:
- Max Planck Inst Astrophys, D-85740 Garching, Germany Max Planck Inst Astrophys Garching Germany D-85740 740 Garching, Germany
- Titolo Testata:
- ASTRONOMY & ASTROPHYSICS
fascicolo: 2,
volume: 372,
anno: 2001,
pagine: 508 - 515
- SICI:
- 1432-0746(200106)372:2<508:BHXTMA>2.0.ZU;2-E
- Fonte:
- ISI
- Lingua:
- ENG
- Soggetto:
- LOCAL SHEAR INSTABILITY; WEAKLY MAGNETIZED DISKS; ACCRETION DISK; DWARF NOVAE; MAGNETOHYDRODYNAMIC SIMULATIONS; WZ-SAGITTAE; BINARIES; EVAPORATION; QUIESCENCE; A0620-00;
- Keywords:
- accretion disks; black hole physics; X-rays : stars; stars : individual : A0620-00, Nova Vul 1988, Nova Mus 1991, 4U 1630-472;
- Tipo documento:
- Article
- Natura:
- Periodico
- Settore Disciplinare:
- Physical, Chemical & Earth Sciences
- Citazioni:
- 52
- Recensione:
- Indirizzi per estratti:
- Indirizzo: Meyer-Hofmeister, E Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany Max Planck Inst Astrophys Karl Schwarzschild Str 1Garching Germany D-85740
-
-
-
- Citazione:
- E. Meyer-Hofmeister e F. Meyer, "Black hole X-ray transients: Mass accumulation in the disk - constraints for the viscosity", ASTRON ASTR, 372(2), 2001, pp. 508-515
Abstract
The outburst cycles of black hole X-ray transients are now generally understood as caused by a thermal instability in the accretion disk, the same mechanism as in dwarf novae outbursts. During quiescence the accretion occursvia a cool disk in the outer region but changes to a coronal flow/ADAF in the inner region. The transition to the coronal ow is caused by evaporationof matter from the cool disk. This process is an important feature for thedisk evolution. We point out that if the disk is depleted during the outburst, e.g. by irradiation, its evolution during quiescence is independent ofthe detailed outburst luminosity decline. The mass accumulation during quiescence has to meet several constraints as the accretion rate, the recurrence time and the total outburst energy. We present a critical discussion of different ways to model X-ray transient outburst cycles and compare with the requirements from observations. For the case of only little mass left over after the outburst the observations indicate a frictional parameter in the cool disk of order alpha (cold) = 0.05, similar to that in dwarf nova disks during quiescence, with no need to resort to much lower alpha values of order 0.005.
ASDD Area Sistemi Dipartimentali e Documentali, Università di Bologna, Catalogo delle riviste ed altri periodici
Documento generato il 20/06/13 alle ore 05:45:45