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Spectral Line Shapes from Black Hole Accretion Disks

Spectral Line Shapes from Black Hole Accretion Disks. Tsing Wai Wong. Advisors: Dr. Drew Milsom Dr. David Ballantyne. (pictures from http://www.seasky.org/cosmic/sky7a09.html and http://www.nasa.gov ). Fitting with model including Relativistic Iron Line Emission.

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Spectral Line Shapes from Black Hole Accretion Disks

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  1. Spectral Line Shapes from Black Hole Accretion Disks Tsing Wai Wong Advisors: Dr. Drew Milsom Dr. David Ballantyne (pictures from http://www.seasky.org/cosmic/sky7a09.html and http://www.nasa.gov )

  2. Fitting with model including Relativistic Iron Line Emission • From Fabian et. al. 2002 Source: MCG-6-30-15 (Observed with XMM-Newton)

  3. Iron Line Profile Shown in (Fv) flux units, obtained from the ratio of the MOS data to best-fitting underlying continuum model. The crosses mark the data points and the solid line marks the line model • From Fabian et. al. 2002

  4. Steps in Calculation • Determine which photons escape and their observed frequencies • Determine which angle they are observed at • Determine the flux at the observation point • From Fanton et. al. 1997, Rauch and Blandford (1994) Image of XMM-Newton (from www.cnrs.fr )

  5. Number of Geodesics reaching Infinity vs. Red Shift

  6. Number of Geodesics Reaching Infinity at a certain Observation Angle

  7. Summary:What we can tell from the line shape? • Temperature Gradient • Spin of the Black Hole • Observation angle (picture from http://web1.pas.rochester.edu/~dmw/ast102/)

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