Correlation of He II Lyman alpha with He I 10830 A, and with chromospheric and EUV coronal emission

Details Correlation of He II Lyman alpha with He I 10830 A, and with chromospheric and EUV coronal emission Correlation of He II Lyman alpha with He I 10830 A, and with chromospheric and EUV coronal emission

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993soph..147...29t&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 147, no. 1, p. 29-46.

Physics

16

Chromosphere, Extreme Ultraviolet Radiation, Helium, Infrared Absorption, Lyman Alpha Radiation, Solar Radiation, Spectroheliographs, Calcium, Calibrating, Image Enhancement, Image Reconstruction, Point Spread Functions

Scientific paper

This paper describes the results of comparing Solar EUV Rocket Telescope and Spectrograph (SERTS-3) images obtained in the transition region line of He II 304 A with chromospheric He I 10830 A absorption; with strong coronal lines of Mg IX 368 A, Fe XV 284 A and 417 A, and Fe XVI 335 A and 31 A; with H-alpha; with Ca II 8542 A; and with magnetograms in Fe I 8688H-alpha. All of the images are illustrated, and the image reconstruction techniques used are described and evaluated. The high correlation of the He II 304 A and He I 10830 A images, originally found by Harvey and Sheeley (1977), is confirmed and is put on a quantitative basis. We find that the supergranulation network has greater contrast, and that filaments appear darker, in 10830 A than in 304 A. In active regions, the 304 A line follows more closely the behavior of H-alpha and Ca II 8542 A than the 10830 A line.

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