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Stellar Rotation in the Young Cluster M17

Published online by Cambridge University Press:  26 May 2016

Wenjin Huang
Affiliation:
Georgia State Univ., Physics & Astronomy, Atlanta, GA 30303 U.S.A.
Douglas Gies
Affiliation:
Georgia State Univ., Physics & Astronomy, Atlanta, GA 30303 U.S.A.
Philip Massey
Affiliation:
Lowell Observatory, 1400 W. Mars Hill, Flagstaff, AZ 86001, U.S.A.
Peter S. Conti
Affiliation:
University of Colorado, JILA, Box 440, Boulder, CO 80309 U.S.A.

Abstract

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We constructed line profile models for young OB stars in M17 using TLUSTY and SYNSPEC, including the effects of rotational flattening and gravitational darkening. The values of v sin i for 8 member stars (with spectral classifications O4.5 V to O9 V) range from 7 km s–1 to 168 km s–1. The mean value of v sin i (102 km s–1) is lower than expected for very young clusters.

Type
Session 1 Observations of Rotating Stars
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Bumgardner, T. E. 1992, , Ohio State University Google Scholar
Hanson, M. M., Conti, P. S., & Rieke, M. J. 1996, ApJS 107, 281 CrossRefGoogle Scholar
Hanson, M. M., Howarth, I. D., & Conti, P. S. 1997, ApJ 489, 698 CrossRefGoogle Scholar
Howarth, I. D., Siebert, K. W., Hussain, G. J., & Prinja, R. K. 1997, MNRAS 284, 265 CrossRefGoogle Scholar
Hubeny, I., & Lanz, T. 1995, ApJ 439, 875 CrossRefGoogle Scholar