Observations of the brightness structure of Alpha Orionis

Details Observations of the brightness structure of Alpha Orionis Observations of the brightness structure of Alpha Orionis

Jun 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....99..232r&link_type=abstract

Astronomy and Astrophysics, vol. 99, no. 2, June 1981, p. 232-238.

Astronomy and Astrophysics

Astrophysics

12

Speckle Patterns, Stellar Luminosity, Stellar Spectrophotometry, Stellar Structure, Supergiant Stars, Brightness, Electrophotometers, Orion Constellation, Power Spectra

Scientific paper

Photoelectric speckle interferometric measurements of Alpha Orionis were performed in October 1979 with the 193-cm telescope at the Haute-Provence Observatory. A radial cut of the two-dimensional power spectrum of the intensity distribution of Alpha Orionis was calculated; the lens atmosphere energy transfer function (ETF), determined from the unresolved Gamma Orionis, was used as a reference. The experimental lens atmosphere ETF was found to be in fair agreement with Korff's theoretical log-normal model (1973), computed for a Fried's parameter of about 6.4 cm. Interpretation of the Alpha Orionis power spectrum gives the following results: (1) the shape of the amplitude spectrum of the star cannot be represented by a uniform disk; (2) the observations are consistent with a core-halo model, the equivalent diameters being 35 plus or minus 10 and 100 plus or minus 40 milliarcseconds; and (3) the ratio of the flux emitted by these two structures is of the order of five, and the level of luminosity of the envelope, as compared to the core of the star, is only a few percent.

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