The dawn of a new era for dustless HdC stars withGaiaeDR3

Autor: P. Tisserand, C. L. Crawford, G. C. Clayton, A. J. Ruiter, V. Karambelkar, M. S. Bessell, I. R. Seitenzahl, M. M. Kasliwal, J. Soon, T. Travouillon
Rok vydání: 2022
Předmět:
Zdroj: Astronomy & Astrophysics. 667:A83
ISSN: 1432-0746
0004-6361
DOI: 10.1051/0004-6361/202142916
Popis: Decades after their discovery, only four hydrogen-deficient carbon (HdC) stars were known to have no circumstellar dust shell. This is in complete contrast to the $\sim$130 known Galactic HdC stars that are notorious for being heavy dust producers, i.e. the R Coronae Borealis (RCB) stars. Together they form a rare class of supergiant stars that are thought to originate from the merger of CO/He white dwarf binary systems, otherwise known as the double-degenerate scenario. We searched for new dustless HdC (dLHdC) stars. We used primarily the 2MASS and GAIA eDR3 catalogues to select candidates that were followed-up spectroscopically. We discovered 27 new dLHdC stars, one new RCB star and two new EHe stars. Surprisingly, 20 of the new dLHdC stars share a characteristic of the known dLHdC star HD 148839, having lower atmospheric hydrogen deficiencies. The uncovered population of dLHdC stars exhibit a Bulge-like distribution, like the RCB stars, but show multiple differences from those that indicate they are a different population of HdC stars following its own evolutionary sequence with a fainter luminosity and also a narrow range of effective temperature. We found indication of a current low dust production activity for four of the new dLHdC stars which could be typical RCB stars passing through a transition time. We have evidence for the first time of a large range of absolute magnitudes in the overall population of HdC stars, spanning over 3 mag. In the favoured formation framework, this is explained by a large range in the initial total WD binary mass which leads to a series of evolutionary sequences with distinct maximum brightness and initial temperature. The cold Galactic RCB stars are also noticeably fainter than the Magellanic ones, possibly due to a difference in metallicity resulting in different WD mass ratio. In our Galaxy, there could be as many dLHdC stars as RCB stars.
22 pages, 18 figures, accepted in A&A. V3: minor corrections on Table 2 and 3 related to HD stars names and (V-I)0 colours (Fig.10 changed accordingly). V4: changed the colour to light blue for the two new EHe stars indicated in Fig.10, page 13
Databáze: OpenAIRE
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