A model for relativistic disk emission, flow and variability

dc.contributor.author	Mohan, Prashanth
dc.contributor.author	Mangalam, A
dc.date.accessioned	2020-11-27T01:25:07Z
dc.date.available	2020-11-27T01:25:07Z
dc.date.issued	2015-04
dc.identifier.citation	ASI Conference Series, Vol. 12, pp. 111-112	en_US
dc.identifier.uri	http://prints.iiap.res.in/handle/2248/7474
dc.description	Open Access © Astronomical Society of India http://www.astron-soc.in/bulletin/asics_vol012/pdfs/prashanth.pdf	en_US
dc.description.abstract	Orbiting features near a black hole can cause variability in optical/UV and X-ray bands with quasi-periodic signatures. The variable flux is derived in Kerr geometry including the following relativistic effects: light bending, time delay, Doppler and gravitational shifts and aberration. The model can be used as a distinguishing timing signature to identify types of accretion disks in active galactic nuclei and X-ray binaries and to constrain the black hole mass and spin.	en_US
dc.language.iso	en	en_US
dc.publisher	Astronomical Society of India	en_US
dc.subject	accretion, accretion disks	en_US
dc.subject	black hole physics	en_US
dc.subject	gravitation	en_US
dc.subject	relativity	en_US
dc.subject	galaxies: active	en_US
dc.subject	X-rays: binaries	en_US
dc.title	A model for relativistic disk emission, flow and variability	en_US
dc.type	Article	en_US