Recent results on the solar diameter

Details Recent results on the solar diameter Recent results on the solar diameter

Oct 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991soph..135..243w&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 135, Oct. 1991, p. 243-248.

Physics

10

Astrometry, Diameters, Sun, Angular Resolution, Telescopes

Scientific paper

Using optically identical telescopes at different sites, the solar diameter is measured with a drift-scan technique. In order to investigate the cause of the observed fluctuations, observations made simultaneously by different observers at the same telescope are compared as are observations made simultaneously at two different sites. It is found that the mean error of a single drift time measurement is +/-0.08 s (or +/- 1.1 arcsec) at Izana and +/-0.11 s (or +/- 1.7 arcsec) at Locarno; this closely corresponds to the angular resolution at those two sites under normal seeing conditions. No correlation is found between observations at different sites; a significant correlation exists, however, between observations made simultaneously by different observers at the same site. This indicates that most of the observed fluctuations are due to atmospheric effects rather than personality effects. The mean solar semidiameter derived from a total of 1122 observations made in 1990 is R = (960.56 +/-0.03) arcsec; this may be compared with R = (960.32 +/-0.02) arcsec which is obtained from a reanalysis of 1773 observations made in 1981. Although a small residual increase of the solar diameter during the last 10 years seems to be indicated, most - if not all - of the observed varitions are due to variable seeing conditions, and there is still no conclusive evidence for a genuine solar variation with amplitudes in excess of about +/-0.3 arcsec.

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