dc.creatorBelloni, Tomaso
dc.creatorMéndez, Mariano R.
dc.creatorKing, Andrew J.
dc.creatorKlis, M. van der
dc.creatorParadijs, J. van
dc.date1999
dc.date2021-08-17T15:53:26Z
dc.date.accessioned2023-07-15T02:41:40Z
dc.date.available2023-07-15T02:41:40Z
dc.identifierhttp://sedici.unlp.edu.ar/handle/10915/122741
dc.identifierhttps://www.sciencedirect.com/science/article/abs/pii/S0920563298002345?via%3Dihub
dc.identifierissn:0920-5632
dc.identifier.urihttps://repositorioslatinoamericanos.uchile.cl/handle/2250/7462922
dc.descriptionGRS 1915+105, one of the two known galactic microquasars, shows an extremely complex variability in the X-ray band, comparable to no other X-ray source in the sky. Making use of RXTE/PCA data, we have analyzed the X-ray spectral distribution throughout the variability. We find that all variations can be attributed to the rapid appearance and disappearance of the inner region of an optically-thick accretion disk. Since the time scale for each event is related to the maximum radius of the disappearing region, the difference in time structure is due to the time distribution of such radii. The observed relation between the extent of the missing inner region of the disk and the duration of an event is in remarkable agreement with the expected radius dependence of the viscous time scale of the radiation-dominated region of an accretion disk.
dc.descriptionFacultad de Ciencias Astronómicas y Geofísicas
dc.formatapplication/pdf
dc.format330-335
dc.languageen
dc.rightshttp://creativecommons.org/licenses/by-nc-sa/4.0/
dc.rightsCreative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.subjectCiencias Astronómicas
dc.subjectThick disk
dc.subjectAstronomy
dc.subjectPhysics
dc.subjectAccretion disc
dc.subjectScale (ratio)
dc.subjectEvent (particle physics)
dc.subjectTime distribution
dc.subjectTime structure
dc.subjectAstrophysics
dc.subjectSky
dc.subjectRadius
dc.subjectSpectral power distribution
dc.titleThe viscous disk of GRS 1915-105
dc.typeArticulo
dc.typeArticulo


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