Synthetic Doppler maps of gaseous flows in IP Peg

Details Synthetic Doppler maps of gaseous flows in IP Peg Synthetic Doppler maps of gaseous flows in IP Peg

2001-05-25

arxiv.org/abs/astro-ph/0105449v1

Astron. Zh. 2001, v.78, pp.997-1007 (Astron. Rep., v.45, pp.872-881)

Astronomy and Astrophysics

Astrophysics

LaTeX, 16 pages, to be published in Astron. Zh

Scientific paper

We present synthetic Doppler maps of gaseous flows in binary IP Peg based on the results of 3D gasdynamical simulations. Using of gasdynamical calculations alongside with the Doppler tomography technique permits us to identify the main features of the flow on the Doppler maps without solution of an ill-posed inverse problem. Comparison of synthetic tomograms with observations shows that in quiescence there are two zones of high emission: a shock wave on the edge of the stream from L_1 caused by the interaction of the gas of circumbinary envelope and the stream, and the dense region in a apoastron of quasi-elliptical accretion disk. A single arm of the spiral shock and the stream itself give a minor input to the total brightness. During outburst the accretion disk dominates, and the most emitive regions are the two arms of the spiral shock.

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