Diagnostics of solar flare hard X-ray sources

The > 40-keV solar-flare electrons observed by the IMP III and Mariner IV satellites are shown to be closely correlated with solar radio and X-ray burst emission. In particular, intense type III radio bursts are observed to accompany solar electron-event flares. The energies of the electrons, the total number of electrons, and the size of the electron source at the sun can be inferred from radio observations. The characteristics of the electrons observed in interplanetary space are consistent with these radio observations. Therefore these electrons are identified as the exciting agents of the type III emission. It has been noted that the radio and X-ray bursts are part of the flash phase of flares. The observations indicate that a striking feature of the flash phase is the production of electrons of 10–100 keV energies.

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The influence of the energy emitted by solar flare soft X-ray bursts on the propagation of their associated interplanetary shock waves

Astrophysics and Space Science ◽

10.1007/bf00649273 ◽

1985 ◽

Vol 116 (1) ◽

pp. 51-60 ◽

Cited By ~ 4

Author(s):

S. Pinter ◽

M. Dryer

Keyword(s):

Solar Flare ◽

Shock Waves ◽

Interplanetary Shock ◽

X Ray

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X-ray magnitude of the 4 November 2003 solar flare inferred from the ionospheric attenuation of the galactic radio background

Journal of Geophysical Research Atmospheres ◽

10.1029/2004ja010960 ◽

2005 ◽

Vol 110 (A9) ◽

Cited By ~ 28

Author(s):

David Brodrick ◽

Steven Tingay ◽

Mark Wieringa

Keyword(s):

Solar Flare ◽

X Ray ◽

Radio Background ◽

Galactic Radio

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The frequency of stellar X-ray flares from a large-scale XMM-Newton sample

Proceedings of the International Astronomical Union ◽

10.1017/s1743921316008668 ◽

2015 ◽

Vol 11 (S320) ◽

pp. 134-137

Author(s):

John P. Pye ◽

Simon R. Rosen

Keyword(s):

Solar System ◽

Solar Flare ◽

Space Weather ◽

White Light ◽

Large Scale ◽

The Sun ◽

X Ray ◽

Cool Star ◽

Exoplanetary Systems ◽

Solar Type

AbstractWe present estimates of cool-star X-ray flare rates determined from the XMM-Tycho survey (Pyeet al. 2015, A&A, 581, A28), and compare them with previously published values for the Sun and for other stellar EUV and white-light samples. We demonstrate the importance of applying appropriate corrections, especially in regard to the total, effective size of the stellar sample. Our results are broadly consistent with rates reported in the literature for Kepler white-light flares from solar-type stars, and with extrapolations of solar flare rates, indicating the potential of stellar X-ray flare observations to address issues such as ‘space weather’ in exoplanetary systems and our own solar system.

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