Abstract
A co-rotating interaction region (CIR) forms in a stellar wind when a fast stream from a rotating star overtakes a slow stream. CIR’s have been studied in detail in the solar wind over the past decade primarily because they are efficient sources of particle acceleration. Here, we point out the usefulness of CIR’s in OB star winds to explain two properties of such winds: deposition of non-radiative energy in the wind far from the stellar surfaces and acceleration of non-thermal particles.
This is a preview of subscription content, log in via an institution to check access.
Access this chapter
Tax calculation will be finalised at checkout
Purchases are for personal use only
Preview
Unable to display preview. Download preview PDF.
References
Abbott, D. 1985 (this conference).
Fisk, L. A. and Lee, M A. 1980, Ap. J. 237, 620.
Holzer, T. 1979, in Solar System Plasma Physics (eds. E. Parker et al) (North Holland), p. 101.
Hundhausen, A. 1973, J. Geophys. Res. 78, 1528.
Lamers, H. et al, 1982, Ap. J. 158, 186.
Mullan, D. J. 1984. Ap. J. 283, 303.
Smith, E. J. and Wolfe, J. H. 1977 in Study of Travelling Interplanetary Phenomena (eds. M. Shea, et al) (Reidel), p.227.
White, R. E. and Becker, R. 1983, Ap. J. (Lett.) 272, L19.
Author information
Authors and Affiliations
Editor information
Editors and Affiliations
Rights and permissions
Copyright information
© 1985 D. Reidel Publishing Company
About this paper
Cite this paper
Mullan, D.J. (1985). Co-Rotating Interaction Regions in Stellar Winds: Particle Acceleration and Non-Thermal Radio Emission in Hot Stars. In: Hjellming, R.M., Gibson, D.M. (eds) Radio Stars. Astrophysics and Space Science Library, vol 116. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-5420-5_4
Download citation
DOI: https://doi.org/10.1007/978-94-009-5420-5_4
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-8892-3
Online ISBN: 978-94-009-5420-5
eBook Packages: Springer Book Archive