Generation of a magnetic barrier around a type I cometary tail

Details Generation of a magnetic barrier around a type I cometary tail Generation of a magnetic barrier around a type I cometary tail

Feb 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984azh....61..121i&link_type=abstract

(Astronomicheskii Zhurnal, vol. 61, Jan.-Feb. 1984, p. 121-123) Soviet Astronomy (ISSN 0038-5301), vol. 28, Jan.-Feb. 1984, p. 7

Physics

1

Comet Tails, Magnetohydrodynamics, Magnetomechanics (Physics), Kinematics, Magnetic Fields, Magnetic Induction, Solar Wind, Space Plasmas

Scientific paper

The theory of magnetokinematics is applied to characterize the magnetic field near a cometary tail, extending the results of Perez de Tejada et al. (1980) as proposed by Ioffe (1973). It is found that a magnetic barrier comprising a region of enhanced field extending parallel to the tail is generated at the velocity shear point at the base of the tail. The maximum value of the ratio of magnetic to kinematic energy density (beta) is calculated as 0.2 for a comet with tail initial velocity 30-50 km/s and tail matter density 5 x 10 to the -21st g/cu cm; the tail field in the central regions does not exceed 10 gamma.

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