Can I read The structure and evolution of a solar flare as observed in 3.5–30 keV X-rays on EtoBox?

The structure and evolution of a solar flare as observed in 3.5–30 keV X-rays by R. A. Harrison; G. M. Simnett; P. Hoyng; H. LaFleur; H. F. Van Beek is a Physics and Astronomy article available to read on EtoBox.

What is The structure and evolution of a solar flare as observed in 3.5–30 keV X-rays about?

On July 5, 1980 the Hard X-Ray Imaging Spectrometer on board the Solar Maximum Mission observed a complex flare event starting at 22 : 32 UT from AR2559 (Hale 16955), then at N28 W29, which developed finally into a 2-ribbon flare. In this paper we compare the X-ray images with He photographs taken at the Big Bear Solar Observatory and identify the site of the most energetic flare phenomena. During the early phases of the event the hard X-rays (> 16 keV) came from a compact source located near one of the two bright He kernels; we believe the latter are at the footpoints of a compact magnetic loop. The kernel identified with the X-ray source is immediately adjacent to one of the principal sunspots and in fact appears to 'rotate' around the sunspot over 90 ~ in the early phase of the flare. Two intense X-ray bursts occur at the site of the rotating kernel, and following each burst the loop fills with hot, X-ray emitting plasma. If the first burst is interpreted as bremsstrahlung from a beam of electrons impinging on a collisionally dominated medium, the energy in such electrons, > 16 keV, is ~ 5 x 1030 erg. The altitude of the looptop is 7-10 • 103 kin. The temperature structure of th

Who reads The structure and evolution of a solar flare as observed in 3.5–30 keV X-rays?

Author

R. A. Harrison; G. M. Simnett; P. Hoyng; H. LaFleur; H. F. Van Beek

Publisher

Springer; Springer-Verlag; Kluwer Academic Publishers; Springer Science and Business Media LLC (ISSN 0038-0938)

Published

1983

Language

EN

Field

Physics and Astronomy (Physical Sciences)