Observational Appearance and Spectrum of Black-Hole Winds

Details Observational Appearance and Spectrum of Black-Hole Winds Observational Appearance and Spectrum of Black-Hole Winds

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010pasj...62.1399f&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.62, No.6, pp.1399--1405

Physics

Accretion, Accretion Disks, Black Hole Physics, Radiative Transfer, Relativity, Winds

Scientific paper

We examine the observational appearance of an optically thick, spherically symmetric, relativistic wind (a black-hole wind), focusing our attention on the emerging spectrum. In a relativistic flow, the apparent optical depth becomes small (large) in the downstream (upstream) direction due to the Lorentz-Fitzgerald contraction. As a result, the location of the apparent photosphere of the wind is remarkably modified, and there appears a relativistic limb-darkening (center-brightening) effect, where the comoving temperature distribution of the apparent photosphere is enhanced (reduced) at the center (in the limb). In addition, due to the usual Doppler boost, the observed temperature distribution is greatly changed. These relativistic effects modify the expected spectrum. When the wind speed is subrelativistic, the observed temperature distribution is almost uniform, and the spectra of the black-hole wind are blackbody-like. When the wind speed becomes relativistic, on the other hand, the observed temperature distribution, Tobs, exhibits a power-law nature of Tobs ∝ r-1, where r is the distance from the disk center, and the observed spectra Sν become a modified blackbody, which has a power-law part of Sν ∝ ν, where ν is the frequency. We briefly examine the effects of the spatial variation of the wind speed and the mass-loss rate.

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