Hostname: page-component-78c5997874-s2hrs Total loading time: 0 Render date: 2024-11-10T06:46:30.623Z Has data issue: false hasContentIssue false
  • English
  • Français

Abundances of Potassium, Argon, and Sulphur in Solar Flares

Published online by Cambridge University Press:  26 May 2016

K. J. H. Phillips ,
J. Sylwester ,
B. Sylwester  and
E. Landi
K. J. H. Phillips
Affiliation:
National Research Council Senior Research Associate, NASA Goddard Space Flight Center, Code 682, Greenbelt, MD 20771, USA
J. Sylwester
Affiliation:
Space Research Centre, Polish Academy of Sciences, ul. Kopernika 11, 51-622 Wroclaw, Poland
B. Sylwester
Affiliation:
Space Research Centre, Polish Academy of Sciences, ul. Kopernika 11, 51-622 Wroclaw, Poland
E. Landi
Affiliation:
Artep Inc., Ellicott City, MD 21042, USA and E. O. Hulburt Center for Space Research, US Naval Research Laboratory, Washington DC 20375, USA

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Observations of the 3.3—6.1 Â X-ray line and continuous spectrum during four long-duration flares with the RESIK crystal spectrometer on the Coronas-F spacecraft have been analyzed to get the absolute abundances of potassium, argon, and sulphur. A differential emission measure of the form DEM ∝ exp(—Te/T0) was found to give the most consistent results of three models including an isothermal model. We obtained K/H = (3.7 ± 1.0) x 10—7, a factor 3 times photospheric; Ar/H = (2.8 ± 0.2) x 10—6, slightly lower than photospheric; and S/H = (2.2±0.4) x 10—5, approximately equal to photospheric. These measurements are consistent with a pattern in which elements with low (< 10 eV) first ionization potential are enriched in the corona by a factor of about 3 and elements of high first ionization potential have abundances approximately equal to photospheric.

Type
Part 4: High Energy Phenomena in Sun and Stars
Information
Symposium - International Astronomical Union , Volume 219: Stars as Suns : Activity, Evolution and Planets , 2004 , pp. 176 - 180
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Dere, K. P., Landi, E., Mason, H. E., Monsignori Fossi, B. C., & Young, P. R. 1997, A&AS, 125, 149.Google Scholar
Doschek, G. A., Feldman, U., & Seely, J. F. 1985, MNRAS, 217, 317.CrossRefGoogle Scholar
Feldman, U., & Laming, J. M. 2000, Phys. Scr., 61, 222.Google Scholar
Grevesse, N., & Sauval, A. J. 1998, Space Sci. Rev., 85, 161.Google Scholar
Landi, E., Feldman, U., & Dere, K. P. 2002, ApJS, 139, 281.Google Scholar
Landi, E., Feldman, U., Innes, D. E., & Curdt, W. 2003, ApJ, 582, 506.CrossRefGoogle Scholar
Mazzotta, P., Mazzitelli, G., Colafranscesco, S., & Vittorio, N. 1998, A&AS, 133, 403.Google Scholar
Reames, D. V. 1998, Space Sci. Rev., 85, 327.Google Scholar
Takeda, Y., Kato, K.-I., Watanabe, Y., & Sadakane, K. 1996, PASJ, 48, 511.Google Scholar