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Astrotomography

Published online by Cambridge University Press:  20 April 2012

Keith Horne ,
Raymundo Baptista ,
Misty C. Bentz  and
Danny Steeghs
Keith Horne
Affiliation:
SUPA Physics & Astronomy, University of St Andrews, St Andrews KY16 9SS, Scotland email: kdh1@st-and.ac.uk
Raymundo Baptista
Affiliation:
Departmento de Fisica, Universidade Federal de Santa Catarina, Campus Trinidade, 88040-900 Florianopolis, SC, Brazil
Misty C. Bentz
Affiliation:
Department of Physics and Astronomy, Georgia State University, Atlanta, GA, 30303USA
Danny Steeghs
Affiliation:
Department of Physics, University of Warwick, Coventry CV4 7AL, UK
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Abstract

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Astrotomography refers to a suite of indirect imaging techniques that achieve micro-arcsecond angular resolution by measuring projections obtained from time-resolved spectroscopic observations. The projections arise from Doppler shifts, eclipses or time delays, combined with rotation of the star or binary system being imaged. At our workshop we reviewed and discussed state-of-the-art methods for imaging the surfaces and magnetic fields of rapidly rotating stars, the accretion flows in compact binary star systems and the broad emission-line regions in active galactic nuclei.

Keywords

accretionaccretion disksblack hole physicsmethods: data analysistechniques: high angular resolutionstars: binaries: eclipsinggalaxies: Seyfert
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S285: New Horizons in Time-Domain Astronomy , September 2011 , pp. 227 - 234
Copyright
Copyright © International Astronomical Union 2012

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