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On the origin of continuum and line emission in CTTSs

Published online by Cambridge University Press:  01 May 2007

S. A. Lamzin ,
M. M. Romanova  and
A. S. Kravtsova
S. A. Lamzin
Affiliation:
Sternberg Astronomical Institute, Universitetskij prospect 13, Moscow, 119991, Russia email: [email protected], [email protected]
M. M. Romanova
Affiliation:
Department of Astronomy, Cornell University, Ithaca, NY 14853-6801, USA email: [email protected]
A. S. Kravtsova
Affiliation:
Sternberg Astronomical Institute, Universitetskij prospect 13, Moscow, 119991, Russia email: [email protected], [email protected]
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Abstract

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We calculated profiles of CIV, 1550Å, Si IV 1400Å, NV 1240Å and OVI 1035Å doublet lines using results of 3D MHD simulations of disc accretion onto young stars with a dipole magnetic field. It appeared that our calculations cannot reproduce the profiles of these lines observed (HST/GHRS-STIS and FUSE) in CTTSs spectra. We also found that the theory predicts much larger CIV 1550Å line flux than observed (up to two orders of magnitude in some cases) and argue that the main portion of accretion energy in CTTSs is liberated outside the accretion shock. We conclude that the reason of disagreement between the theory and observation is the strongly non-dipolar character of CTTS magnetic field near its surface.

Keywords

Stars: pre–main-sequenceshock wavesultraviolet: starsmagnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S243: Star-Disk Interaction in Young Stars , May 2007 , pp. 115 - 122
Copyright
Copyright © International Astronomical Union 2007

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