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Stellar Rotation in the Young Cluster M17

Published online by Cambridge University Press:  26 May 2016

Wenjin Huang ,
Douglas Gies ,
Philip Massey  and
Peter S. Conti
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
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 67 - 68
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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