The solar-flare infrared continuum - Observational techniques and upper limits

Details The solar-flare infrared continuum - Observational techniques and upper limits The solar-flare infrared continuum - Observational techniques and upper limits

Nov 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975soph...45...69h&link_type=abstract

Solar Physics, vol. 45, Nov. 1975, p. 69-78.

Physics

12

Infrared Spectra, Solar Flares, Solar Spectra, Atmospheric Windows, H Alpha Line, Solar Radio Bursts, Submillimeter Waves

Scientific paper

Exploratory observations at 20 microns and 350 microns have determined detection thresholds for solar flares in these wavelengths. In the 20-micron range, solar atmospheric fluctuations (the 'temperature field') set the basic limits on flare detectability at about 5 K; at 350 microns, extinction in the earth's atmosphere provides the basic limitation of about 30 K. These thresholds are low enough for the successful detection of several infrared-emitting components of large flares. The upper limits obtained for subflares indicate that the thickness of the H-alpha flare region does not exceed approximately 10 km. This result confirms the conclusion of Suemoto and Hiei (1959) regarding the small effective thickness of the H-alpha-emitting regions in solar flares.

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