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Science 10 March 1995:
Vol. 267. no. 5203, pp. 1470 - 1473
DOI: 10.1126/science.267.5203.1470
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Articles

The Elemental Composition of the Corona of Procyon: Evidence for the Absence of the FIP Effect

Jeremy J. Drake 1, J. Martin Laming 2, Kenneth G. Widing 3, Jürgen H. M. M. Schmitt 4, Bernhard Haisch 5, and Stuart Bowyer 1

1 Center for Extreme Ultraviolet Astrophysics, University of California, 2150 Kittredge Street, Berkeley, CA 94720, USA.
2 Sachs Freeman Associates, Landover, MD 20785, USA, and E. O. Hulburt Center for Space Research, Naval Research Laboratory, Code 7674L, Washington, DC 20375, USA.
3 E. O. Hulburt Center for Space Research, Naval Research Laboratory, Code 7674W, Washington, DC 20375, USA.
4 Max-Planck-Institut fur Extraterrestrische Physik, 85740 Garching, Germany
5 Lockheed Solar and Astrophysics Laboratory, Department 91-30, Building 252, 3251 Hanover Street, Palo Alto, CA 94304, USA, and Center for Extreme Ultraviolet Astrophysics, University of California, 2150 Kittredge Street, Berkeley, CA 94720, USA.

The chemical composition of the solar corona is not the same as that of the underlying photosphere. In the corona, elements with a first ionization potential (FIP) of le10 electron volts (for example, iron, magnesium, silicon, and calcium) are overabundant relative to those with an FIP of ge10 electron volts (for example, oxygen, neon, and sulfur) by factors of 3 to 10 with respect to the photosphere. The origin of this FIP effect is unknown. The launch of the Extreme Ultraviolet Explorer Satellite (EUVE) opened up the spectroscopic capability required to determine elemental abundances in the coronae of other stars. Spectroscopic observations of the corona of the nearby F5 IV star Procyon obtained with EUVE have yielded estimates of the relative abundances of high- and low-FIP species. The results provide evidence that Procyon, unlike the sun, does not exhibit the FIP effect. Whether the sun or Procyon is more typical of the general late-type stellar population is of fundamental interest to the physics of stellar outer atmospheres and has a bearing on the origin of cosmic rays.

Submitted on August 18, 1994
Accepted on December 28, 1994

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Science. ISSN 0036-8075 (print), 1095-9203 (online)