Unresolved binary systems with white dwarfs in open star clusters

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Аннотация

We invesigate unresolved binary systems with components of main sequence star (MS) and white dwarf (WD) in nine open clusters. These systems are located below and to the left of the main sequence at the colour-magnitude diagram. We compare the number of cluster stars, which have likely evolved into white dwarfs, with the number of candidates for unresolved binary systems with WD. The number of probable cluster members, lying below the main sequence, is generally less than the expected number of white dwarfs. The observations in the ultraviolet could detect WDs and unresolved binary WD+MS systems more confidently than the observations in the visible range.

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Авторлар туралы

V. Mikhnevich

Ural Federal University

Хат алмасуға жауапты Автор.
Email: varvara.mikhnevich@urfu.ru
Ресей, Еkaterinburg

A. Seleznev

Ural Federal University

Email: varvara.mikhnevich@urfu.ru
Ресей, Еkaterinburg

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2. Fig. 1. PARSEC isochrones with solar metal abundances and age logarithms in years from 7.3 to 9.5. The position of the turning point is indicated by a black dot on each isochrone. The mass of the star in solar mass units corresponding to the turning point is indicated by an arrow. The age is indicated by a halftone gradient.

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3. Fig. 2. CMD clusters of NGC 3532 in the Gaia photometric system. The solid black line shows the PARSEC isochrone [29], which best fits the cluster sequence. The dots show the cluster stars according to the data of [32]. The black stars indicate the selected MS stars. The open circles indicate the BCs associated with the cluster [18], and the squares indicate the simulated unresolved binary systems consisting of a BC and a MS star.

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4. Fig. 3. CMD clusters of NGC 3532 in the Gaia photometric system. The solid black line shows the PARSEC isochrone, the dashed line shows the boundary of the region occupied by white dwarfs, according to [15]. The dots show the cluster stars according to [32]. The squares indicate the supposedly unresolved BC + GP systems — the cluster members lying below the main sequence. The open circles indicate the BC stellar magnitude estimates obtained for all possible mGP values ​​in the BC + GP system. The triangles are the cluster members falling within the BC region.

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5. Fig. 4. On the left is the “stellar magnitude-color index” diagram of the NGC 3532 cluster sample in the Gaia photometric system [32]. On the right is the ratio of the abundance of objects evolved in the BD Nevol/Ntotal and the abundance of binary systems with a white dwarf NBD+GP/Ntotal; the gradient shows the age of the clusters under consideration.

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6. Fig. 5. CMD clusters of NGC 3532 in the UV bands of the Hubble Space Telescope photometric system. The PARSEC isochrone is shown by the solid black line. The black stars indicate selected MS stars. The open circles indicate selected BCs from [35]. The squares indicate simulated unresolved binary systems consisting of a BC and a MS star.

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