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Lifetimes of Circumstellar Disks in Lynds 1641

Published online by Cambridge University Press:  12 April 2016

Lori E. Allen  and
Karen M. Strom
Lori E. Allen*
Affiliation:
School of Physics, University of New South Wales, Sydney, NSW, 2052, Australia
Karen M. Strom*
Affiliation:
Department of Physics and Astronomy, University of Massachusetts, Amherst, MA 01002
*
Visiting Astronomer, Kitt Peak National Observatory. KPNO is operated by AURA, Inc. under cooperative agreement with the National Science Foundation
Visiting Astronomer, Kitt Peak National Observatory. KPNO is operated by AURA, Inc. under cooperative agreement with the National Science Foundation

Abstract

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It is by now evident that most young stars have associated disks and/or envelopes, which may be active (accreting) or passive (reprocessing stellar photons), or both. Knowing how such disks evolve is crucial to our understanding of how stars form, and may be relevant to other questions, such as the time available for the formation of planets in solar nebulae. In this poster we discuss the properties of pre-main sequence circumstellar disks in Lynds 1641 in Orion, the nearest giant molecular cloud complex.

Type
Part 15. Poster Papers
Information
International Astronomical Union Colloquium , Volume 163: Accretion Phenomena and Related Outflows , 1997 , pp. 683 - 684
Copyright
Copyright © Astronomical Society of the Pacific 1997

References

D’Antona, F. & Mazzitelli, I. 1994, ApJS, 90, 467 CrossRefGoogle Scholar
Strom, K.M., Strom, S.E., & Merrill, K.M. 1993, ApJ, 412, 233 Google Scholar