EDP Sciences
Free access
Volume 438, Number 2, August I 2005
Page(s) L13 - L16
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:200500118

A&A 438, L13-L16 (2005)
DOI: 10.1051/0004-6361:200500118


The cool Galactic R Coronae Borealis variable DY Persei

L. Zacs1, W. P. Chen2, O. Alksnis1, D. Kinoshita2, F. A. Musaev3, 4, 5, T. Brice6, K. Sanchawala2, H. T. Lee2 and C. W. Chen2

1  Institute of Atomic Physics and Spectroscopy, University of Latvia, Raina bulvaris 19, 1586 Riga, Latvia
    e-mail: zacs@latnet.lv
2  Graduate Institute of Astronomy, National Central University, Chung-Li 32054, ROC, Taiwan
    e-mail: wchen@astro.ncu.edu.tw
3  Special Astrophysical Observatory and Isaac Newton Institute of Chile, SAO Branch, Nizhnij Arkhyz 369167, Russia
    e-mail: faig@sao.ru
4  ICAMER, National Academy of Sciences of Ukraine, 361605 Peak Terskol, Kabardino-Balkaria, Russia
5  Shamakhy Astrophysical Observatory, National Academy of Sciences of Azerbaijan, Azerbaijan
6  1.State Gimnazium of Riga, Raina bulvaris 8, 1050 Riga, Latvia
    e-mail: tamara@r1g.edu.lv

(Received 1 March 2005 / Accepted 28 April 2005)

Results of first CCD photometry during the recent deep light decline, and high-resolution spectroscopy, are presented for DY Persei. The spectra show variable blueshifted features in the sodium D lines. The C I lines are strong whereas neutron-capture elements are not enhanced. The isotopic 13CN(2, 0) lines relative to 12CN are of similar strength with those for the carbon star U Hya. All these confirm the RCB nature of DY Per and the existence of ejected clouds. At least two clouds are revealed at -197.3 and -143.0 km s-1. A star was detected about 0$\farcs$4 to the west and 2$\farcs$5 to the north from DY Per. This anonymous companion, with observed colour indices (B-V) = 0.68 and  $(V-R) \simeq 1.1$, may be a foreground star.

Key words: stars: carbon -- stars: winds, outflows -- stars: fundamental parameters -- stars: circumstellar matter -- stars: individual: DY Per

SIMBAD Objects

© ESO 2005