Co-rotating Interaction Regions In Stellar Winds: Particle Acceleration and Non-Thermal Radio Emission in Hot Stars

Details Co-rotating Interaction Regions In Stellar Winds: Particle Acceleration and Non-Thermal Radio Emission in Hot Stars Co-rotating Interaction Regions In Stellar Winds: Particle Acceleration and Non-Thermal Radio Emission in Hot Stars

Jul 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985assl..116...39m&link_type=abstract

Radio Stars, edited by Robert M. Hjellming and David M. Gobson ISBN 90-277-2063-0; 1985 Astrophysics and Space Science Library V

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

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, the author points 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.

Affiliated with

Also associated with

No associations

Rating

Co-rotating Interaction Regions In Stellar Winds: Particle Acceleration and Non-Thermal Radio Emission in Hot Stars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Co-rotating Interaction Regions In Stellar Winds: Particle Acceleration and Non-Thermal Radio Emission in Hot Stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Co-rotating Interaction Regions In Stellar Winds: Particle Acceleration and Non-Thermal Radio Emission in Hot Stars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1231436