Abstract
The integrated soft X-ray (8–12 A) fluxes for solar flares, given by Thomas and Teske (1971), have been scaled to the equivalent EXOSAT (0.04–2.0 KeV) fluxes using spectra obtained from a variety of rocket-based experiments. A model by Me we for a 1.5 KeV plasma gives essentially similar results. The data show good agreement with the soft X-ray — Hγ correlation established earlier by Butler, Rodono and Foing (1988) for flares on dMe stars. Simultaneous GINGA and optical spectroscopy of a flare on the RS CVn star II Peg extends the correlation a further two orders of magnitude and confirms that a common, linear, relationship applies to all stellar and solar flares for which data are currently available (see figure 1).
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
