Gamma-ray binaries

Chernyakova, Maria; Malyshev, D.

doi:10.22323/1.362.0045

Cited by 12 publications

(8 citation statements)

References 118 publications

(163 reference statements)

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“…Ultraviolet emission from the hot star ionizes the disk, which re-emits photons at longer wavelengths. Be stars are also interesting because they are often found in high-mass X-ray binaries (HMXBs;Walter et al 2015) and γ-ray binaries (Chernyakova & Malyshev 2020). The end products of Be star (and Be binary) evolution are not fully understood (van den Heuvel 2019) and may include exotic compact objects (e.g., magnetars).…”

Section: Introductionmentioning

confidence: 99%

Catalog of X-Ray Detected Be Stars (XDBS)

et al. 2022

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We present a catalog of X-ray Detected Be Stars (XDBS) with 161 Be stars from the Be Star Spectra (BeSS) database having X-ray counterparts in the Chandra Source Catalog v2.0, XMM-Newton 4XMM-DR11 Catalog, or Swift 2SXPS Catalog. The multi-wavelength catalog includes accurate optical positions, X-ray properties (fluxes, photon indices and hardness ratios), optical, near-infrared and infrared photometry, source classifications (when available), and other properties including proper motions, effective temperatures, X-ray to optical flux ratios as well. We also provide a convenient https://home.gwu.edu/~kargaltsev/XDBS/graphical user interface which allows for easy visualization of the catalog content.

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Section: Introductionmentioning

confidence: 99%

Catalog of X-Ray Detected Be Stars (XDBS)

et al. 2022

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“…The γ ‐ray binaries are a recently established and rare subclass of the high‐mass X‐ray binaries with most of their luminosity output being radiated above 1 MeV (Chernyakova & Malyshev 2020; Dubus 2013). They are composed of an OBe donor star and a neutron star or a black hole (Mirabel 2012).…”

Section: Introductionmentioning

confidence: 99%

Radius, rotational period, and inclination of the Be stars in the Be/gamma‐ray binariesMWC148 andMWC656

et al. 2021

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Using TESS photometry and Rozhen spectra of the Be/γ-ray binaries MWC 148 and MWC 656, we estimate the projected rotational velocity (v sin i), rotational period (P rot ), radius (R 1 ), and inclination (i) of the mass donor. For MWC 148, we derive P rot = 1.10 ± 0.03 day, R 1 = 9.2 ± 0.05 R sun , i = 40 • ± 2 • , and v sin i = 272 ± 5 km s −1 . For MWC 656, we obtain P rot = 1.12 ± 0.03 day, R 1 = 8.8 ± 0.5 R sun , i = 52 • ± 3 • , and v sin i = 313 ± 3 km s −1 . For MWC 656, we also find that the rotation of the mass donor is coplanar with the orbital plane.

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“…According to a Bayesian analysis of the radio data, the orbital period of LS I +61 • 303 is 26.4960 ± 0.0028 d (Gregory 2002). The most peculiar feature of this system is its superorbital modulations with P sup ≃ 1628 ± 48 d as seen at all wavelengths, which has not been found for other γ-ray binaries (e.g., Li et al 2011;Chernyakova et al 2012Chernyakova et al , 2017Ackermann et al 2013;Ahnen et al 2016;Massi & Torricelli-Ciamponi 2016;Jaron et al 2018). The origin of its long-term modulations remains unknown, although several models have been proposed, including precession of the Be disc or the relativistic jet (Massi & Torricelli-Ciamponi 2014;Saha et al 2016;Xing et al 2017;Jaron 2021).…”

Section: Ls I +61 • 303mentioning

confidence: 95%

“…γ-ray binaries are a rare subclass of high-mass binary systems harbouring a compact object in orbit with a type O/B star and radiate luminous γ-rays with non-thermal energy spectra peaking beyond 1 MeV (see Dubus 2013Dubus , 2015Lamberts 2016;van Soelen 2017;Paredes & Bordas 2019;Chernyakova & Malyshev 2020 for reviews). So far, less than ten such binaries have been found, and only two of them with compact objects have been identified as pulsars.…”

Section: Introductionmentioning

confidence: 99%

Modelling the correlated keV/TeV light curves of Be/gamma-ray binaries

Chen,

Takata

2021

Preprint

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Be/γ-ray binaries comprise a confirmed or presumptive pulsar orbiting a Be star and emit luminous γ-rays. Nonthermal emissions are thought to arise from synchrotron radiation and inverse-Compton (IC) scattering in the shock where the pulsar wind is terminated by the stellar outflow. We study wind interactions and shock radiations from such systems and show that the bimodal structures observed in keV/TeV light curves are caused by enhanced synchrotron radiation and IC scattering during disc passages. We use a simple radiation model to reproduce orbital modulations of keV X-ray and TeV γ-ray flux and compare with two confirmed pulsar/Be star binaries (i.e. PSR B1259-63/LS 2883 and PSR J2032+4127/MT91 213), and two candidates (i.e. HESS J0632+057 and LS I +61 • 303). We find that the keV/TeV light curves of former two binaries can be well explained by the inclined disc model, while modelling the modulated emissions of latter two sources remains challenging with current orbital solutions. Therefore, we propose alternative orbital geometries for HESS J0632+057 and LS I +61 • 303. We estimate the positions and inclination angles of Be discs by fitting correlated keV/TeV light curves. Our results could be beneficial for future measurements of orbital parameters and searches for radio pulsations from presumed pulsars.

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Gamma-ray binaries

Cited by 12 publications

References 118 publications

Catalog of X-Ray Detected Be Stars (XDBS)

Catalog of X-Ray Detected Be Stars (XDBS)

Radius, rotational period, and inclination of the Be stars in the Be/gamma‐ray binariesMWC148 andMWC656

Modelling the correlated keV/TeV light curves of Be/gamma-ray binaries

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