Accretion Structure in AU Mon

Details Accretion Structure in AU Mon Accretion Structure in AU Mon

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21541923a&link_type=abstract

American Astronomical Society, AAS Meeting #215, #419.23; Bulletin of the American Astronomical Society, Vol. 42, p.280

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AU Mon is a long period (11.113 days) Algol binary system with a stable accretion disk that can be seen in the double-peaked emission in the H-alpha line. We present new modeling of the accretion structures in this system. We have reexamined archival UV data from the IUE telescope spanning 15 years and we have also analyzed H-alpha data from the KPNO 0.9m Coude Feed Telescope as well as high resolution echelle spectra from the Hobby-Eberly Telescope. We use these data to self-consistently model the temperature and structure of the accretion disk using the Shellspec program. The generated synthetic emission profiles are subtracted from the observed spectra for several lines of interest including H-alpha, H-beta, H-gamma, and the Si-IV doublet. The resulting difference profiles allow us to conduct tomography in order to characterize the gas stream and other accretion features of the system. The wide wavelength coverage of our data permits investigation of gas flows occurring at a variety of temperatures.

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