Stripped helium stars in UV
Abstract
The model of Galactic population of stripped helium stars, the remnants of 5 ≲ M/M⊙ ≲ 24 primary components of close binaries after RLOF is presented. These stars emit in the UV range of the spectrum and may be observed by detectors aboard planned "Spektr-UV" (WSO-UV) space telescope. For the current star formation rate in the Galaxy 2M⊙ yr−1, the estimate of the number of 1 to 7 M⊙ objects with Teff ≳25,000\,K ranges from 14700 to 28500. The number of 2 to 7 M⊙ objects is 3200 to 5500. The main evolutionary factor influencing the estimate is possible formation of common envelopes and merger of components in them. Detection of candidate stripped helium stars by UV-excess is hampered by the dominance of main-sequence companions to stripped helium stars in the combined spectra of binaries. This effect of observational selection may reduce the number of candidate stripped helium stars potentially detectable by photometry to ≲ 1000.
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BibTeX
@misc{yungelson2026stripped,
title = {{Stripped helium stars in UV}},
author = {L. R. Yungelson and A. G. Kuranov and A. V. Mishakina},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.14518},
eprint = {2609.14518},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.14518},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Stripped helium stars in UV
AU - L. R. Yungelson
AU - A. G. Kuranov
AU - A. V. Mishakina
PY - 2026
DA - 2026/09/13
PB - arXiv
DO - 10.48550/arxiv.2609.14518
UR - https://arxiv.org/abs/2609.14518
AB - The model of Galactic population of stripped helium stars, the remnants of 5 ≲ M/M_⊙ ≲ 24 primary components of close binaries after RLOF is presented. These stars emit in the UV range of the spectrum and may be observed by detectors aboard planned "Spektr-UV" (WSO-UV) space telescope. For the current star formation rate in the Galaxy 2M_⊙ yr^−1, the estimate of the number of 1 to 7 M_⊙ objects with T_eff ≳25,000\,K ranges from 14700 to 28500. The number of 2 to 7 M_⊙ objects is 3200 to 5500. The main evolutionary factor influencing the estimate is possible formation of common envelopes and merger of components in them. Detection of candidate stripped helium stars by UV-excess is hampered by the dominance of main-sequence companions to stripped helium stars in the combined spectra of binaries. This effect of observational selection may reduce the number of candidate stripped helium stars potentially detectable by photometry to ≲ 1000.
ER -