Computer Science
Scientific paper
Jun 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997phdt........21s&link_type=abstract
Thesis (PHD). THE COLLEGE OF WILLIAM AND MARY , Source DAI-B 58/08, p. 4279, Feb 1998, 103 pages.
Computer Science
Scientific paper
Solar data from the Halogen Occultation Experiment (HALOE) were analyzed to determine the center-to-limb relative intensity and the vertical temperature profile for the quiet and active Sun over wavelengths from 2.4 to 10 μm. An algorithm that incorporated a nonlinear least squares procedure was developed that modeled the HALOE instrument during data acquisition. Data obtained from limb-to-limb scans along the solar equator on days of very low activity in May 1994 were analyzed to obtain coefficients of a function describing the relative intensity from center to limb. The relative intensities produced were precise to 0.1% (2σ) from the center to 0.25 arc min from the limb. The brightness temperature from the flux and the temperature as a function of monochromatic optical depth were also calculated from the coefficients. These quantities were normalized using published central intensities and compared to a semiemperical model of the photosphere. In general, the calculated temperature quantities were in good agreement with the model predictions; however, differences occurring between 2.4 and 3 μm suggest that the central intensities used here are low. HALOE solar data were also investigated to obtain the intensity of a sunspot relative to the photosphere. A nonlinear least squares method was used to retrieve relative intensity information for a large sunspot on August 19, 1942. At each wavelength a one-component sunspot model proved sufficient to fit the measurements to the digitization level of the instrument. Sunspot/photosphere intensity ratios were calculated at each wavelength with an uncertainty of 2%. Compared with previous measurements at shorter wavelengths from 0.387 to 2.35 μm, the data exhibit the same general trend of larger ratios with increasing wavelengths; however, a larger than anticipated gap exists between the previous value at 2.35 μm and the HALOE ratio value at 2.45 μm. The photospheric and sunspot temperatures were calculated at each wavelength and show slight decreases with increasing wavelength. A steep drop exhibited by the previous measurements between 1.67 and 2.35 μm is not supported by HALOE values. Consideration of terrestrial atmospheric effects in the previous data could explain this discrepancy.
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