EDP Sciences
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Volume 427, Number 3, December I 2004
Page(s) 937 - 944
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20041618

A&A 427, 937-944 (2004)
DOI: 10.1051/0004-6361:20041618

Fundamental parameters and evolutionary state of the Herbig Ae star candidate HD 35929

A. S. Miroshnichenko1, 2, 3, R. O. Gray4, V. G. Klochkova5, 6, K. S. Bjorkman2 and K. S. Kuratov7

1  Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
    e-mail: anatoly@physics.utoledo.edu
2  Ritter Observatory, Dept. of Physics & Astronomy, The University of Toledo, Toledo, OH 43606-3390, USA
3  Pulkovo Observatory, Saint-Petersburg, 196140, Russia
4  Dept. of Physics and Astronomy, Appalachian State University, Boone, NC 28608, USA
5  Special Astrophysical Observatory of the Russian Academy of Sciences, Karachai-Cirkassian Republic, Nizhnij Arkhyz, 369167, Russia
6  Isaac Newton Institute of Chile, SAO Branch, Russia
7  Fesenkov Astrophysical Institute, Almaty 480068, Kazakhstan

(Received 8 July 2004 / Accepted 27 July 2004)

HD 35929 is a pre-main-sequence Herbig Ae star candidate that exhibits emission in the H $\alpha$ line and a weak IR excess. Although its luminosity type was estimated as IV from low-resolution spectroscopy, the insignificant HIPPARCOS parallax ( $0.88\pm0.93$ mas) contradicted the low luminosity. To resolve this discrepancy, we took 3 high-resolution optical spectra of the star (region 5200-6915 Å, $R \sim60\,000$) and used an archival one (4000-6800 Å, $R \sim48\,000$). Our analysis of the spectral and photometric information shows that HD 35929 is an F2 III star with $T_{\rm eff}=6880\pm100$ K, $\log g = 3.3\pm0.1$, $\log \, L/L_{\odot}=1.7\pm0.2$, $v\,\sin i =70\pm5$ km s -1, $M=2.3\pm0.2~M_{\odot}$, a mild metal deficit $\rm [Fe/H]=-0.2\pm0.1$, and a weak interstellar reddening ( $A_{\rm V} \sim0.1$ mag) at a distance $D = 345\pm60$ pc. These results confirm an earlier suggestion by Marconi et al. (2000) that HD 35929 is located within the instability strip. At the same time, we argue that it is not a young object, but rather a post-main-sequence giant. The fundamental parameters and IR excess of HD 35929 are similar to those of HD 19993, an emission-line late A-type giant recently discovered by us (Miroshnichenko et al. 2003). These objects might represent a group of evolved intermediate-mass stars with an enhanced mass loss.

Key words: techniques: spectroscopic -- techniques: photometric -- stars: circumstellar matter -- stars: individual: HD 35929

SIMBAD Objects

© ESO 2004