Solar wind disturbances caused by solar flares - Equatorial plane

Details Solar wind disturbances caused by solar flares - Equatorial plane Solar wind disturbances caused by solar flares - Equatorial plane

Dec 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983p%26ss...31.1435a&link_type=abstract

Planetary and Space Science (ISSN 0032-0633), vol. 31, Dec. 1983, p. 1435-1458.

Physics

11

Interplanetary Magnetic Fields, Solar Flares, Solar Wind Velocity, Flow Geometry, Heliosphere, Magnetic Field Configurations, Solar Physics, Velocity Distribution

Scientific paper

The propagation of solar wind disturbances caused by single, double and six successive flares in the dipolar and quadrupolar patterns of the interplanetary magnetic field (IMF) and the associated solar wind flow is studied. This study is based on a kinematic and empirical method developed by Hakamada and Akasofu (1982). Each flare is characterized by six parameters (such as the highest speed flow, its extent and duration). The successive IMF patterns in the equatorial plane of the heliosphere during a time span of 0.5-60 days after flares are presented for a variety of flares. The solar wind speed and IMF magnitude are given as a function of distance along a radial line fixed in space and also as a function of time at several points fixed in space (simulating approximately space probe observations). Some of the results are qualitatively compared with recent space probe observations, demonstrating fair similarity with the observed time profiles of solar wind speed variations over a wide range of both distances (0-10 AU) and time spans (60 days). The method provides a first-order construction, temporal and spatial, of flare-induced shocks and their multiple interactions with each other, as well as with the corotating interaction regions.

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