Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989nyasa.571..423m&link_type=abstract
(NASA, NSF, Texas Academy of Science, et al., Texas Symposium on Relativistic Astrophysics, 14th, Dallas, TX, Dec. 11-16, 1988)
Astronomy and Astrophysics
Astrophysics
Companion Stars, Pulsars, Stellar Magnetospheres, Stellar Occultation, Stellar Winds, Comet Heads, Eclipses, Pulsar Magnetospheres, Refractivity, Stellar Models
Scientific paper
Three existing eclipse models for the PSR 1957 + 20 pulsar are discussed in terms of their requirements and the information they yield about the pulsar wind: the interacting wind from a companion model, the magnetosphere model, and the occulting disk model. It is shown out that the wind model requires an 'MHD' wind from the pulsar, with enough particles that the Poynting flux of the wind can be thermalized; in this model, a large flux of energetic radiation from the pulsar is required to accompany the wind and drive the wind off the companion. The magnetosphere model requires an 'EM' wind, which is Poynting flux dominated; the advantage of this model over the wind model is that the plasma density inside the magnetosphere can be orders of magnitude larger than in a magnetospheric tail blown back by wind interaction. The occulting disk model also requires an 'EM' wind so that the interaction would be pushed down onto the companion surface, minimizing direct interaction of the wind with the orbiting macroscopic particles.
No associations
LandOfFree
Eclipse models 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 Eclipse models, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Eclipse models will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1575873