Photometric and UV spectroscopic observations of 22 VUL at eclipse - Observational evidence for an extended chromosphere of a 'solar type' G supergiant

Details Photometric and UV spectroscopic observations of 22 VUL at eclipse - Observational evidence for an extended chromosphere of a 'solar type' G supergiant Photometric and UV spectroscopic observations of 22 VUL at eclipse - Observational evidence for an extended chromosphere of a 'solar type' G supergiant

Oct 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...151l...5s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 151, no. 2, Oct. 1985, p. L5, L6.

Astronomy and Astrophysics

Astronomy

7

Eclipsing Binary Stars, G Stars, Red Giant Stars, Stellar Atmospheres, Stellar Spectrophotometry, Supergiant Stars, Ultraviolet Spectroscopy, Chromosphere, Iue, Spaceborne Astronomy

Scientific paper

The solar spectral type supergiant (G3 Ib-II) of the 22 Vul binary has been observed photometrically and spectroscopically during its recent eclipse of the B9 V companion. From the new photometric observations the eclipse data given by Parsons and Ake (1984) can be slightly improved (period = 249.21 ± 0.2 days, mideclipse: JD 2446191.6 ± 0.2). The UV spectra obtained from IUE enable us to determine the extension and density of the chromosphere. The extension of the chromosphere is of the order of one giant radius (lRG). The column density of hydrogen at a projected distance of one eclipse radius from the photosphere is log NH = 21.6 ± 0.3, which is almost the same as the column density of the extended chromosphere of 32 Cyg (a K5 supergiant) at 1 RK.

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