GHRS Spectra of alpha Tau

Details GHRS Spectra of alpha Tau GHRS Spectra of alpha Tau

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...185.4509c&link_type=abstract

American Astronomical Society, 185th AAS Meeting, #45.09; Bulletin of the American Astronomical Society, Vol. 26, p.1380

Astronomy and Astrophysics

Astronomy

9

Scientific paper

Goddard High Resolution Spectrograph (GHRS) observations of the K5 giant alpha Tau were obtained on 8 April 1994. Spectra of approximately 40 Angstroms-wide regions centered near 1300, 1550, 1660, 1995, 2340, 2760, and 2800 Angstroms were obtained through the Small Science Aperture (SSA) with medium resolution (R=20,000) gratings. These data provide high-precision profiles of a variety of lines formed in the stellar chromosphere and transition region, including O I, Fe II, C I, C II], Si II], Mg II, and C IV. Self-reversed emission from O I, Fe II, and Mg II provide information on the wind flow velocities, with all three ions showing both red and blue-shifted absorption components, as seen previously in the Fe II emission from the later-type giants gamma Cru and mu Gem. The first evidence for hot plasma in the outer atmosphere of alpha Tau is seen in the G160M spectrum centered near 1550 Angstroms@. This spectrum shows very broad, but distinct features due to the C IV (UV 1) doublet, as well as a myriad of much narrower emissions formed at cooler temperatures, such as (fluorescent) Fe II and perhaps Ni II and C I. C I (UV 2) is seen in emission and a comparison of its flux with that in C I (UV 32) will allow an estimation of the C I chromospheric column density. Multiple observations of the C II] (UV 0.01) intercombination multiplet were obtained to search for evidence of shocks and/or propagating waves. Results of that search will be presented. Finally, very high-resolution (R=85,000) echelle spectra were obtained of the Mg II resonance doublet near 2800 Angstroms@. These emission features show strong interstellar, stellar, and circumstellar absorption components at, above, and below the stellar rest velocity.

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