L-alpha intensity in coronal streamers

Details L-alpha intensity in coronal streamers L-alpha intensity in coronal streamers

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993soph..147...73n&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 147, no. 1, p. 73-96.

Mathematics

8

Luminous Intensity, Lyman Alpha Radiation, Relaxation Method (Mathematics), Solar Corona, Solar Radiation, Solar Wind, Two Dimensional Models, Magnetic Field Configurations, Solar Magnetic Field

Scientific paper

White-light images are presently the primary source of information on physical conditions in the solar corona at distances greater than a few tenths of a solar radius above the limb. As a consequence, we still only have an incomplete description of structures extending beyond the solar limb. In particular, streamers, although observed for decades, represent a poorly known phenomenon. SOHO, to be launched in 1995, will be able to make long-term observations of these features up to heights of a few solar radii, both in white light and UV. In this paper we present simulations of L-alpha intensity in coronal streamers, based on the two-dimensional (2D) model developed by Wang et at. (1992, 1993) via a time-dependent numerical relaxation approach. Because the model is 2D, we make an a priori hypothesis about the extension of streamers in the third dimension. L-alpha data, obtained from a rocket (Kohl et al., 1983), allowed us to identify a shape which fits the observations.

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