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

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

Abstract

HD 35929 is a pre-main-sequence Herbig Ae star candidate that exhibits emission in the Hα line and a weak IR excess. Although its luminosity type was estimated as iv from low-resolution spectroscopy, the insignificant HIPPARCOS parallax ( mas) contradicted the low luminosity. To resolve this discrepancy, we took 3 high-resolution optical spectra of the star (region 5200–6915 Å, ) and used an archival one (4000–6800 Å, ). Our analysis of the spectral and photometric information shows that HD 35929 is an F2 iii star with K, , ,  km s^-1, , a mild metal deficit , and a weak interstellar reddening ( mag) at a distance  pc. These results confirm an earlier suggestion by Marconi et al. ([CITE]) 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. [CITE]). These objects might represent a group of evolved intermediate-mass stars with an enhanced mass loss.