Physics
Scientific paper
Jan 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985nascp2358..130m&link_type=abstract
In NASA. Goddard Space Flight Center The Origin of Nonradiative Heating/Momentum in Hot Stars p 130-135 (SEE N85-17755 08-88)
Physics
Hot Stars, Momentum Transfer, Nonthermal Radiation, Particle Acceleration, Rotating Fluids, Solar Wind, Stellar Rotation, Stellar Winds, Charged Particles, Flow Velocity, Magnetohydrodynamic Turbulence, Nonlinearity, Temperature Profiles
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. The CIR's were studied in detail in the solar wind over the past decade primarily because they are efficient sources of particle acceleration. Here, CIR's in OB star winds are used 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.
No associations
LandOfFree
Corotating 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 Corotating 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 Corotating interaction regions in stellar winds: Particle acceleration and non-thermal radio emission in hot stars will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-927320