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Diagnostics of the Velocity Field in the Lower Atmosphere of Solar Flares

Published online by Cambridge University Press:  12 April 2016

Fang Cheng ,
Yin Su-Ying ,
Ding Ming-De  and
Eijiro Hiei
Fang Cheng
Affiliation:
Department of Astronomy, Nanjing University, Nanjing, China
Yin Su-Ying
Affiliation:
Department of Astronomy, Nanjing University, Nanjing, China
Ding Ming-De
Affiliation:
Department of Astronomy, Nanjing University, Nanjing, China
Eijiro Hiei
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, Japan

Abstract

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Based on the analyses of Call K line profiles of 12 solar flares, the characteristics of the red asymmetry of Call K line are summarized. Non-LTE calculations indicated that a downward motion of plasma above the temperature minimum region (TMR) as well as a contracting motion of plasma toward TMR can well explain the red asymmetry observed at the Ki positions. The typical velocity is 10-30 km s−1. This result is consistent with the observations of metallic lines of solar flares.

Type
Session 6. Flares and Transients
Information
International Astronomical Union Colloquium , Volume 141: The Magnetic and Velocity Fields of Solar Active Regions , 1993 , pp. 347 - 350
Copyright
Copyright © Astronomical Society of the Pacific 1993

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