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High Resolution Observations of the Solar Corona

Published online by Cambridge University Press:  30 March 2016

D. Gomez  and
L. Golub
D. Gomez
Affiliation:
Harvard-Smithsonian Center for Astrophysics60 Garden St., Cambridge, MA 02138, USA
L. Golub
Affiliation:
Harvard-Smithsonian Center for Astrophysics60 Garden St., Cambridge, MA 02138, USA

Extract

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Soft X-ray images of the solar corona obtained during the last 20 years have systematically shown an intimate relationship between intense emitting structures and magnetic fields (Vaiana and Rosner 1978). The magnetic field confines a 106 K plasma, which is an intense source of soft X-ray photons. Therefore, it is natural to expect the bright X-ray structures to follow the field’s geometry. But this relationship does not seem to be just geometrical. It is generally believed that the energy necessary to heat the plasma comes from the dissipation of magnetic stresses, which are continually being re-generated by subphotospheric convective motions. However, there is still great uncertainty about the precise physical mechanisms involved in the production and release of the magnetic energy.

Type
Joint Commission Meetings
Information
Highlights of Astronomy , Volume 9: Highlights of Astronomy. As presented at the XXIst General Assembly of the IAU, 1991 , 1992 , pp. 659 - 660
Copyright
Copyright © Kluwer 1992

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