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Probing the size of a magnetosphere of a young solar-like star

Published online by Cambridge University Press:  01 November 2008

Catrina M. Hamilton ,
C. M. Johns-Krull ,
R. Mundt ,
W. Herbst  and
J. N. Winn
Catrina M. Hamilton
Affiliation:
Department of Physics and Astronomy, Dickinson College, Carlisle, PA 17013, USA email: hamiltoc@dickinson.edu
C. M. Johns-Krull
Affiliation:
Department of Physics and Astronomy, Rice University, Houston, TX 77005, USA email: cmj@rice.edu
R. Mundt
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany email: mundt@mpia.de
W. Herbst
Affiliation:
Astronomy Department, Wesleyan University, Middletown, CT 06459, USA email: wherbst@wesleyan.edu
J. N. Winn
Affiliation:
Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA email: jwinn@space.mit.edu
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Abstract

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We have obtained high resolution spectra of the pre-main sequence binary system KH 15D (V582 Mon) while the star is fully visible, fully occulted, and during several ingress and egress events over the course of five contiguous observing seasons. The Hα line profile is a standard probe of the magnetospheric accretion flows on young stars such as KH 15D. We use these time series data to map out the size of the magnetosphere and find that it changes size from one observing season to the next.

Keywords

Line: profiles – stars: individual (KH 15D, V582 Mon) – stars: pre-main-sequence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S259: Cosmic Magnetic Fields: From Planets, to Stars and Galaxies , November 2008 , pp. 413 - 414
Copyright
Copyright © International Astronomical Union 2009

References

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Hamilton, C. M., et al. 2003, ApJ 591, L45Google Scholar
Hamilton, C. M., et al. 2005, AJ 130, 1896Google Scholar
Winn, J. N., et al. 2004, ApJ 603, L45Google Scholar