Maximum-entropy maps of the Be shell star zeta Tauri from optical long-baseline interferometry

Details Maximum-entropy maps of the Be shell star zeta Tauri from optical long-baseline interferometry Maximum-entropy maps of the Be shell star zeta Tauri from optical long-baseline interferometry

Mar 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...283l..13q&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 283, no. 2, p. L13-L16

Statistics

Computation

60

B Stars, Computer Aided Mapping, Emission Spectra, H Alpha Line, Maximum Entropy Method, Shell Stars, Stellar Mass, Stellar Models, Computational Astrophysics, Mathematical Models, Point Sources, Scattering Amplitude, Stellar Envelopes, Very Long Base Interferometry

Scientific paper

We present the first maximum-entropy maps reconstructed from visibility amplitudes obtained with an optical long-baseline interferometer. They show the Be shell star zeta Tauri. In the continuum at 550 nm the star is an unresolved point source, whereas in the light of the H-alpha line an extended, elongated structure is observed. The best-fit parameters of an elliptical Gaussian model are: major axis a = 3.55 +/- 0.33 mas, axial ratio r = 0.30 +/- 0.03, position angle phi = -59 deg +/- 4 deg. The morphology of the H-alpha emission region is most easily interpreted as a disk seen almost edge-on; if this disk is axially symmetric, a limit for the inclination i greater than or equal to 73 deg can be derived. Our observations provide further evidence for the equatorial disk model of Be stars.

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