Astronomy and Astrophysics – Astronomy
Scientific paper
May 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aas...190.2503l&link_type=abstract
American Astronomical Society, 190th AAS Meeting, #25.03; Bulletin of the American Astronomical Society, Vol. 29, p.806
Astronomy and Astrophysics
Astronomy
Scientific paper
We report on the first set of UV spectra taken of Mira stars under high dispersion with the Goddard High Resolution Spectrograph (GHRS) onboard the Hubble Space Telescope (HST). Two spectral regions were observed, 2320 Angstroms -- 2368 Angstroms to record the C II] (UV0.01) multiplet and 2785 Angstroms -- 2835 Angstroms to obtain the Mg II h & k lines, for two Mira variables stars: R Hya, taken on 9 July 1996 (phase 0.26), and R Leo, taken on 14 January 1997 (phase 0.12). The R Hya Mg II spectrum is very clean and shows overlying absorption from Fe I (UV3) and Mn I (UV1) over the k line. The fluoresced Fe I (UV44) feature at 2824 Angstroms is plainly visible in this spectrum, whereas past IUE observations at high dispersion were unable to record this feature. Remarkably, the newly identified fluoresced Fe I (UV45) feature near 2807 Angstroms feature is seen in this spectrum. Until now, this line has only been seen in cool carbon stars with HST/GHRS. It is remarkable in that it is pumped by the thin C II] (UV0.01) emission line at 2325.5 Angstroms in the carbon stars. This line is the likely pump in the oxygen-rich Miras in our sample as well. Two of the strongest C II] (UV0.01) near 2325 Angstroms are barely detectable in our spectrum. This region of the spectrum is dominated by weak Si II] (UV0.01) near 2335 Angstroms, opposite to what is observed in the carbon stars. Very weak Mg II lines are seen in the R Leo spectrum at phase 0.12. At this phase, these lines are typically absent in IUE spectra. This work is supported by NASA/STSCI grant GO-06620.01-95A. Ms. Mahar is an undergraduate student at East Tennessee State University who is assisting in the data analysis.
Luttermoser Donald G.
Mahar S.
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