Magnetic reconnection in large-scale cosmic plasmas

Details Magnetic reconnection in large-scale cosmic plasmas Magnetic reconnection in large-scale cosmic plasmas

Jun 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001ep%26s...53..677m&link_type=abstract

Earth, Planets and Space, Volume 53, p. 677-681.

Physics

1

Scientific paper

X-ray emitting hot plasmas of a temperature 2-12 keV, associated with galaxy clusters, constitute the most dominant form of baryons in the universe. The plasma is thought to be magnetized at least to 0.1-1 nT, although the b value is relatively high at 10-100. The plasma is confined by gravity of each cluster in a stable manner, but the member galaxies are moving through it with an approximately transonic speed. Therefore, the plasma must be in a magnetohydrodynamically turbulent condition, where frequent magnetic reconnection is expected to take place. Mainly based on observations with the ASCA X-ray Observatory, evidence for such magnetic reconnection is accumulating.

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