An SRG/eROSITA Study of Be X-ray binaries in Quiescence
Abstract
Be X-ray binaries (BeXRBs) are mostly transient X-ray binaries with usually a neutron star as the compact object and a Be star as their optical companion. We performed a comprehensive analysis of BeXRBs in quiescence with the extended ROentgen Survey with an Imaging Telescope Array (eROSITA), the soft X-ray instrument on board the Spectrum-Roentgen-Gamma satellite, using its first all-sky survey (eRASS1) data. The transient BeXRBs spend majority of time in their quiescent state, but are often studied during their outbursts. A quiescence study is useful to probe the emission mechanism of BeXRBs at low mass accretion rates. The spectra of BeXRBs detected in the eRASS1 main catalogue could be well fitted with a powerlaw as well as a blackbody model. In the absence of detection of a BeXRB, we report the luminosity upper limit for its position in the sky. The X-ray luminosity for the quiescent BeXRBs detected with eROSITA have LX∼1033−36 erg s−1 for both absorbed powerlaw and blackbody models in most cases. For the absorbed blackbody model, the emission seems to come from a fraction of the neutron star's surface. The quiescence luminosity of BeXRBs are used to distinguish between different accretion models at low mass accretion rates, like accretion in the propeller regime or from a cold accretion disc. The detection space of BeXRBs in quiescence for the eRASS1 data is compared against previously reported luminosities across multiple X-ray observatories.
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BibTeX
@misc{balu2026srgerosita,
title = {{An SRG/eROSITA Study of Be X-ray binaries in Quiescence}},
author = {Ajith Balu and Kinjal Roy and Biswajit Paul},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.37277},
eprint = {2610.37277},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.37277},
note = {CC BY-NC-ND 4.0},
}
RIS
TY - UNPB
TI - An SRG/eROSITA Study of Be X-ray binaries in Quiescence
AU - Ajith Balu
AU - Kinjal Roy
AU - Biswajit Paul
PY - 2026
DA - 2026/10/27
PB - arXiv
DO - 10.48550/arxiv.2610.37277
UR - https://arxiv.org/abs/2610.37277
AB - Be X-ray binaries (BeXRBs) are mostly transient X-ray binaries with usually a neutron star as the compact object and a Be star as their optical companion. We performed a comprehensive analysis of BeXRBs in quiescence with the extended ROentgen Survey with an Imaging Telescope Array (eROSITA), the soft X-ray instrument on board the Spectrum-Roentgen-Gamma satellite, using its first all-sky survey (eRASS1) data. The transient BeXRBs spend majority of time in their quiescent state, but are often studied during their outbursts. A quiescence study is useful to probe the emission mechanism of BeXRBs at low mass accretion rates. The spectra of BeXRBs detected in the eRASS1 main catalogue could be well fitted with a powerlaw as well as a blackbody model. In the absence of detection of a BeXRB, we report the luminosity upper limit for its position in the sky. The X-ray luminosity for the quiescent BeXRBs detected with eROSITA have L_X∼10^33−36 erg s^−1 for both absorbed powerlaw and blackbody models in most cases. For the absorbed blackbody model, the emission seems to come from a fraction of the neutron star's surface. The quiescence luminosity of BeXRBs are used to distinguish between different accretion models at low mass accretion rates, like accretion in the propeller regime or from a cold accretion disc. The detection space of BeXRBs in quiescence for the eRASS1 data is compared against previously reported luminosities across multiple X-ray observatories.
ER -