Fen Edebiyat Fakültesi / Faculty of Letters and Sciences

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Browsing Fen Edebiyat Fakültesi / Faculty of Letters and Sciences by Author "Adelman, S. J."

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    A spectroscopic atlas of Deneb (A2 lae) lambda lambda 3826-5212
    (E D P SCIENCES, 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS CEDEXA, FRANCE, 2003-03) Albayrak, B.; Gulliver, A. E.; Adelman, S. J.; Aydin, C.; Koçer, Dursun
    We present a spectroscopic atlas of Deneb (A2 Iae) obtained with the long camera of the 1.22-m telescope of the Dominion Astrophysical Observatory using Reticon and CCD detectors. Forlambdalambda3826-5212 the inverse dispersion is 2.4 Angstrom mm(-1) with a resolution of 0.072 Angstrom. At the continuum the mean signal-to-noise ratio is 1030. The wavelengths in the laboratory frame, the equivalent widths, and the identifications of the various spectral features are given. This atlas should provide useful guidance for studies of other stars with similar spectral types. The stellar and synthetic spectra with their corresponding line identifications can be examined at ht tp://www.brandonu.ca/physics/gulliver/atlases.html.
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    Elemental Abundance Analyses with DAO Spectrograms - XXIX. The Mercury-Manganese Stars 53 Tau, beta Tau, Gamma Crv, and Upsilon Her
    (EDP SCIENCES S A, 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE, 2006-02) Adelman, S. J.; Çalışkan, H.; Gulliver, A. F.; Teker, Ayşegül; TR142309
    We performed elemental abundances analyses of the mercury-manganese (HgMn) stars 53 Tau, beta Tau, and gamma Crv consistent with previous studies of similar stars in this series. The derived v sin i values for the last two stars are 59 and 32 km s(-1), respectively, both of which are greater than those of HgMn stars previously Studied. For 53 Tau this analysis using Selected wavelength regions replaces one performed with coadded photographic spectra. A stricter upper limit is placed on any Hg II lambda 3984 line. The abundances of beta Tau are usually greater than those of gamma Crv. But the later star has a Hg II lambda 3984 line which the former lacks. Our analysis of v Her, which was performed with spectrograms obtained with CCD detectors, is extended by using additional spectrograms to increase the range of wavelengths covered longward of lambda 4800. Minor changes in the derived abundances result.