Hostname: page-component-cd9895bd7-7cvxr Total loading time: 0 Render date: 2024-12-23T19:39:38.745Z Has data issue: false hasContentIssue false
  • English
  • Français

Maxwellian Distributions for Stellar Rotations

Published online by Cambridge University Press:  12 April 2016

Armin J. Deutsch
Armin J. Deutsch*
Affiliation:
Hale Observatories, Carnegie Institution of Washington and California Institute of Technology, Pasadena, Calif, U.S.A.

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

For stars in the main-sequence band, the distributions of ‘line-widths’ Ksin; are rediscussed, with the inclusion of recent measurements by Walker and Hodge for B stars, and by Preston for Ap stars. The Ap stars are counted with normal stars of the same color-class. Over the whole range from B2 to A2, the observed incidence of sharp-line stars far exceeds the incidence predicted on the hypothesis that the true rotational velocities have a Maxwellian distribution. The ‘extra’ slow rotators are probably close binary remnants, in the sense of Van den Heuvel. However, it remains unclear how to distinguish individual members of this group of stars.

Type
Part III / Stellar Rotation in Binaries, Clusters, And Special Objects. Statistics of Stellar Rotation
Information
International Astronomical Union Colloquium , Volume 4: Stellar Rotation , 1970 , pp. 207 - 218
Copyright
Copyright © Reidel 1970

References

Allen, C. W.: 1963, Astrophysical Quantities, 2nd ed., Athlone Press, London, p. 243.Google Scholar
Conti, P. S.: 1965, Astrophys. J. 142, 1594.Google Scholar
Deutsch, A. J.: 1966, Astron. J. 71, 383.CrossRefGoogle Scholar
Deutsch, A. J.: 1967, The Magnetic and Related Stars, (ed. by Cameron, R. C.), Mono Book Corp., Baltimore, p. 181.Google Scholar
Deutsch, A. J.: 1969, reported by Babcock, H. W. in C.I.W. Yrbk. 68.Google Scholar
Eggen, O. J.: 1963, Astron. J. 68, 697.Google Scholar
Eggen, O. J.: 1964, Astron. J. 69, 570.Google Scholar
Huang, S.-S.: 1967, Astrophys. J. 150, 229.CrossRefGoogle Scholar
Huang, S.-S. and Struve, O.: 1960, in Stellar Atmospheres, (ed. by Greenstein, J. L.), Univ. of Chicago Press, p. 321.Google Scholar
Mestel, L.: 1969, Monthly Notices Roy. Astron. Soc. 140, 177.Google Scholar
Preston, G. W.: 1969a, private communication.Google Scholar
Preston, G. W.: 1969b, this volume, p. 254.Google Scholar
Rodgers, A. W.: 1968, Astrophys. J. 152, 109.Google Scholar
Sargent, W. L. W.: 1968, Astrophys. J. 152, 885.Google Scholar
Sargent, W. L. W.: 1969, private communication.Google Scholar
Slettebak, A.: 1954, Astrophys. J. 119, 146.Google Scholar
Slettebak, A.: 1955, Astrophys. J. 121, 653.CrossRefGoogle Scholar
Slettebak, A. and Howard, R. F.: 1955, Astrophys. J. 121, 102.Google Scholar
Van den Heuvel, E. P. J.: 1968, Bull. Astron. Inst. Neth. 19, 326.Google Scholar
Van den Heuvel, E. P. J.: 1969, Lick Obs. Bull., No. 603.Google Scholar
Walker, G. A. H. and Hodge, S. M.: 1966, Pub. Dominion Astrophys. Obs. 13, 2.Google Scholar