arXiv Open Access 2018

Dwarf carbon stars are likely metal-poor binaries and unlikely hosts to carbon planets

Lewis J. Whitehouse J. Farihi P. J. Green T. G. Wilson J. P. Subasavage

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Abstrak

Dwarf carbon stars make up the largest fraction of carbon stars in the Galaxy with around 1200 candidates known to date primarily from the Sloan Digital Sky Survey. They either possess primordial carbon-enhancements, or are polluted by mass transfer from an evolved companion such that C/O is enhanced beyond unity. To directly test the binary hypothesis, a radial velocity monitoring survey has been carried out on 28 dwarf carbon stars, resulting in the detection of variations in 21 targets. Using Monte Carlo simulations, this detection fraction is found to be consistent with a 100% binary population and orbital periods on the order of hundreds of days. This result supports the post-mass transfer nature of dwarf carbon stars, and implies they are not likely hosts to carbon planets.

Topik & Kata Kunci

astro-ph.SR astro-ph.EP

Penulis (5)

Lewis J. Whitehouse

J. Farihi

P. J. Green

T. G. Wilson

J. P. Subasavage

Format Sitasi

APA MLA BibTeX

Whitehouse, L.J., Farihi, J., Green, P.J., Wilson, T.G., Subasavage, J.P. (2018). Dwarf carbon stars are likely metal-poor binaries and unlikely hosts to carbon planets. https://arxiv.org/abs/1806.06074

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Informasi Jurnal

Tahun Terbit: 2018
Bahasa: en
Sumber Database: arXiv
Akses: Open Access ✓