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On mechanisms separating stars into normal and chemically peculiar

On mechanisms separating stars into normal and chemically peculiar The paper argues in favor of the assumption that magnetic and non-magnetic protostars, from which CP stars were formed, are the objects that had rotation velocities of the parent cloud V smaller than a critical value V c . At V greater than the critical value, differential rotation emerges in the collapsing protostellar cloud, which twists magnetic lines of force into an’ invisible’ toroidal shape and disturbs the stability of the atmosphere. In magnetic protostars, the loss of angular momentum is due to magnetic braking, while in metallic protostars, the loss of rotation momentum occurs due to tidal interactions with a close component. HgMn stars are most likely not affected by some braking mechanism, but originated from the slowest protostellar rotators. The boundary of V c where the differential rotation occurs is not sharp. The slower the protostar rotates, the greater the probability of suppressing the differential rotation and the more likely the possibility of CP star birth. http://www.deepdyve.com/assets/images/DeepDyve-Logo-lg.png Astrophysical Bulletin Springer Journals

On mechanisms separating stars into normal and chemically peculiar

Glagolevskij, Yu.
Astrophysical Bulletin , Volume 72 (4) – Nov 23, 2017
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29 pages

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Publisher
Springer Journals
Copyright
Copyright © 2017 by Pleiades Publishing, Ltd.
Subject
Physics; Astronomy, Astrophysics and Cosmology
ISSN
1990-3413
eISSN
1990-3421
DOI
10.1134/S199034131704006X
Publisher site
See Article on Publisher Site

Abstract

The paper argues in favor of the assumption that magnetic and non-magnetic protostars, from which CP stars were formed, are the objects that had rotation velocities of the parent cloud V smaller than a critical value V c . At V greater than the critical value, differential rotation emerges in the collapsing protostellar cloud, which twists magnetic lines of force into an’ invisible’ toroidal shape and disturbs the stability of the atmosphere. In magnetic protostars, the loss of angular momentum is due to magnetic braking, while in metallic protostars, the loss of rotation momentum occurs due to tidal interactions with a close component. HgMn stars are most likely not affected by some braking mechanism, but originated from the slowest protostellar rotators. The boundary of V c where the differential rotation occurs is not sharp. The slower the protostar rotates, the greater the probability of suppressing the differential rotation and the more likely the possibility of CP star birth.

Journal

Astrophysical Bulletin – Springer Journals

Published: Nov 23, 2017

References

  • Astrophysical Bulletin
    Glagolevskij, Y. V.; Nazarenko, A. F.
  • Proc. Intern. Conf on Magnetic Fields of Chemically Peculiar and Related Stars, Nizhnij Arkhyz, Russia, 1999
    Leushin, V. V.; Glagolevskij, Y. V.; North, P.