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Short time-scale periodicity in H-alpha emission from the main-sequence star H II 1883
Marcy, G. W.; Duncan, D. K.; Cohen, R. D.
AA(Mount Wilson and Las Campanas Observatoires, Pasadena, CA), AB(Mount Wilson and Las Campanas Observatoires, Pasadena, CA), AC(California, University, La Jolla, CA)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 288, Jan. 1, 1985, p. 259-265. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
H Alpha Line, Late Stars, Main Sequence Stars, Stellar Spectra, Variable Stars, Corotation, Emission Spectra, Luminosity, Radial Velocity, Star Clusters, Stellar Mass Ejection, Stellar Rotation, Stellar Winds
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H-alpha emission having a full width at its base of 700 km/s is observed in the main-sequence K star, H II 1883, confirming the report by Stauffer et al. (1984). Both the centroid and the width of the H-alpha emission vary synchronously with the 0.24 day rotation period of this Pleiades star. Based on the ratio H-alpha/H-beta, the absence of forbidden lines, and the inferred gas kinematics, this star must have an extended emission region of order one stellar radius in size. The periodic Doppler shifts of H-alpha probably arise from a wind with oppositely directed streams. If a significant fraction of the high-velocity material escapes from the star it will spin down in less than about 10 myr. This suggests that its remarkable properties may represent a natural, though transient stage in the evolution of late-type stars.

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