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HST GHRS Observations of the Herbig Ae Star HD104237: First UV Observations of a Hot Disk Wind from a Pre-Main Sequence Star

Published online by Cambridge University Press:  12 April 2016

Alexander Brown ,
H.R.E. Tjin A Djie ,
P.F.C. Blondel ,
G.M. Harper ,
P.D. Bennett  and
S.L. Skinner
Alexander Brown
Affiliation:
Center for Astrophysics and Space Astronomy, Campus Box 389, University of Colorado, Boulder, Colorado 80309–0389, USA
H.R.E. Tjin A Djie
Affiliation:
Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
P.F.C. Blondel
Affiliation:
Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
G.M. Harper
Affiliation:
Center for Astrophysics and Space Astronomy, Campus Box 389, University of Colorado, Boulder, Colorado 80309–0389, USA
P.D. Bennett
Affiliation:
Center for Astrophysics and Space Astronomy, Campus Box 389, University of Colorado, Boulder, Colorado 80309–0389, USA
S.L. Skinner
Affiliation:
JILA, University of Colorado, Boulder, Colorado 80309–0440, USA

Abstract

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We have obtained ultraviolet spectra of the Herbig Ae star HD104237 using the Goddard High Resolution Spectrograph (GHRS) on HST. The high temperature emission and absorption lines show remarkable outflow absorption features, which have very similar profiles that are essentially independent of formation temperature. The profiles are not those expected from a spherically-symmetric stellar wind but have optically-thick absorption to −280 km s−1 and a high velocity plateau extending to −375 km s−1. The profile shape is a manifestation of the nonspherical geometry of the flow. The observed UV emission is too strong to be associated with the hot X–ray emitting plasma seen by ASCA and probably is generated by the interaction of the innermost part of an accretion disk with the corotating outermost magnetospheric field. The outflow is almost certainly the inner part of a biconical disk wind.

Type
Part 10. Accretion Disks and Outflows
Information
International Astronomical Union Colloquium , Volume 163: Accretion Phenomena and Related Outflows , 1997 , pp. 448 - 452
Copyright
Copyright © Astronomical Society of the Pacific 1997

References

Blondel, P.F.C., Talavera, A., & Tjin A Djie, H.R.E. 1993, A&A, 268, 624 Google Scholar
Grinin, V.P. & Rostopchina, A.N. 1996, Ast. Rep., 40, 194 Google Scholar
Palla, F. and Stahler, S.W. 1990, ApJ, 360, L47 CrossRefGoogle Scholar
Shu, F. et al. 1994, ApJ, 429, 781 Google Scholar
Skinner, S.L. & Yamauchi, S. 1996, ApJ, 471, in pressGoogle Scholar