Statistics – Computation
Scientific paper
Oct 1952
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1952aj.....57t.160h&link_type=abstract
Astronomical Journal, Vol. 57, p. 160
Statistics
Computation
1
Scientific paper
New photoelectric observations in two colors have been made with the ~3-inch Cassegrain telescope of the McDonald Observatory of the University of Texas, using photoelectric equipment belonging to the Washburn Observatory. These observations, combined with others made in Madison, are more accurate than any obtained formerly. A new and better solution for the elements of this star than that published in 1951 is therefore possible. It is apparent from the light-curves that the minima in the two colors are shallower than before. The secondary eclipse, which is total, permits an accurate determination of the phases of second and third contacts and hence a new determination of the darkening coefficients. Assuming one solution with ~ = 0.2, K = 0.455 + 0.003, the ratio of the radii of the two components, is smaller than before, with a probable error +0.003 compared to +0.008. There are corresponding changes of the other elements, but these changes are small. The ratio of surface brightness of the two stars is 1.64 in yellow light and 1.74 in blue light. The difference in magni- tudes is 2.3 in both colors, thus accounting for the fact that only one spectrum is visible. Computations are not yet entirely finished, but are sufficiently in hand to indicate a darkening coefficient ~ between 0.2 and 0.6 for the larger, brighter star and 0.6 for the smaller, fainter star. The small coefficient for a B2 star was predicted by Professor Russell in 1946. It was at first believed and hoped that in this case the coefficient would be somewhat larger, and could be attributed to electron scattering. It is possible that there is an abrupt change in the stellar atmospheric absorption detectable near the middle of the primary eclipse, since computed curves using different coefficients cross the observed curve. Further computations will be necessary before this puzzling question can be definitely answered. Washburn Observatory, Madison, Wis., and University of Manchester, England.
Huffer C. M.
Kopal Zdenek
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