SIMBAD references

2007A&A...472..247Z - Astronomy and Astrophysics, volume 472, 247-256 (2007/9-2)

A comprehensive analysis of the cool RCB star DY Persei.

ZACS L., MONDAL S., CHEN W.P., PUGACH A.F., MUSAEV F.A. and ALKSNIS O.

Abstract (from CDS):

Theoretically, the number of cool Galactic R Coronae Borealis stars (RCBs) should be greater than the warm RCBs, however to date, only a few candidates have been detected. Observations of the extremely cool RCB candidate, DY Per, and the anonymous nearby star (the ``Taipei star'') are presented to specify its fundamental parameters and evolutionary status. CCD BVRI photometry and low-resolution spectroscopy at deep light decline was carried out in 2004. A high-resolution spectrum was gathered near the maximum light in 2002, and a qualitative analysis was made relative to the typical carbon stars of various types. Near the light maximums, the nearby anonymous star with a separation of ∼2.5" reported by Zacs et al. (2005A&A...438L..13Z) was outshined by DY Per. However, in the B and V band the components are resolved at deep light decline and the nearby star is somewhat brighter in B than DY Per itself. BV(R) individual magnitudes of the components were estimated using PSF photometry for the first time. The light decline in 2004 was the deepest ever observed for DY Per, B=18.16mag. The individual colour indices of DY Per at light decline, (B-V)=2.35 and (V-R)≃1.9, are not typical for carbon stars. In the spectrum, absorption features of C2 and CN molecules prevail, however, prominent C2 absorption bands are significantly veiled at deep-light decline and a broad (FWHM∼600km/s) emission feature of NaID12 is visible. Emissions are suspected in the C2 (1,0) bandhead and in Cai line at 4227Å. Analysis of DY Per relative to the sample of carbon stars, verifies the significant hydrogen deficiency, high carbon abundance, relatively high 12C/13C ratio and solar metallicity. Thus DY Per could be a prototype of cool extreme Galactic RCBs. The nearby star does not vary appreciably in the B and V bands, B=17.8mag. With the observed colour indices (B-V)=1.00 and (V-R)≃0.6, it may be a G0 dwarf not physically related to DY Per, although the distances to both stars are similar, d∼1.5kpc.

Abstract Copyright:

Journal keyword(s): stars: carbon - stars: winds, outflows - stars: fundamental parameters - stars: circumstellar matter - stars: individual: DY Per - stars: evolution

Nomenclature: Fig.1, Table 2: [ZMC2007] N (Nos 1-7).

Simbad objects: 18

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