Orbital variability of the optical linear polarization of the <i>γ</i>-ray binary LS I +61° 303 and new constraints on the orbital parameters

Kravtsov, Vadim; Berdyugin, A.; Piirola, V.; Kosenkov, Ilia A.; Tsygankov, Sergey S.; Chernyakova, M.; Malyshev, D.; Sakanoi, Takeshi; Kagitani, Masato; Berdyugina, S. V.; Poutanen, Juri

doi:10.1051/0004-6361/202038745

Cited by 19 publications

(24 citation statements)

References 52 publications

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“…This may be caused by stellar activities on shorter/larger time scales, but the lack of data made it impossible to reach any conclusion. This sinusoidal variation of HOWPol light curve agreed with previous studies ( [12,14] for instance). Both HOWPol and HONIR light curves suggest a short, ∼0.1-0.2-mag brightening a few days after periastron (φ ∼ 0.3-0.35) in the optical bands.…”

Section: Lsi+61 303supporting

confidence: 93%

“…Orbital modulation is clearly seen in the V and R bands by HOWPol; the brightness increases from around periastron to apastron, then decreases from apastron to periastron. The binned light curve (shown in red) showed the amplitude of the variation is ∼0.05 mag, which is consistent with the previous study [14]. Although the phase coverage is not sufficient, the same sinusoidal feature is seen in the I band light curve.…”

Section: Lsi+61 303supporting

confidence: 91%

“…Line-profile variability in Hα indicates perturbations in the Be disk within one orbit, and a bright, high-speed (300-443 km s −1 ) component in the red side of the double-peaked profile before the apastron [13]. More recently, orbital variability in its optical photometry and polarization has been studied [14]. The polarization results showed a periodicity of 13.244 days-half of the orbital period.…”

Section: Introductionmentioning

confidence: 96%

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Optical and Near-Infrared Monitoring of Gamma-ray Binaries Hosting Be Stars

Moritani

Kawachi

2021

Universe

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Optical and near-infrared observations are compiled for the three gamma-ray binaries hosting Be stars: PSR B1259−63, LSI+61 303, and HESS J0632+057. The emissions from the Be disk are considered to vary according to the changes in its structure, some of which are caused by interactions with the compact object (e.g., tidal forces). Due to the high eccentricity and large orbit of these systems, the interactions—and, hence the resultant observables—depend on the orbital phase. To explore such variations, multi-band photometry and linear polarization were monitored for the three considered systems, using two 1.5 m-class telescopes: IRSF at the South African Astronomical Observatory and Kanata at the Higashi–Hiroshima Observatory.

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Section: Lsi+61 303supporting

confidence: 93%

Section: Lsi+61 303supporting

confidence: 91%

Section: Introductionmentioning

confidence: 96%

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Optical and Near-Infrared Monitoring of Gamma-ray Binaries Hosting Be Stars

Moritani

Kawachi

2021

Universe

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“…al provides the new constraints on the orbital parameter of the binary system [14]. The orbit is close to circular with a very small eccentricity ( < 0.15) [14]. The periastron passage is reported at 0.6 [14], significantly different from the previous assumptions but corresponds to the correlated peaks in radio, X-ray and TeV around 0.6.…”

Section: Introductionmentioning

confidence: 81%

“…However, the study by Kravtsov et. al provides the new constraints on the orbital parameter of the binary system [14]. The orbit is close to circular with a very small eccentricity ( < 0.15) [14].…”

Section: Introductionmentioning

confidence: 99%

Very High Energy Gamma-ray Emission from the Binary System LS I +61 303

Kieda¹,

Adams²,

Archer³

et al. 2021

Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)

257

200

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LS I +61°303 is one of around ten gamma-ray binaries detected so far which has a spectral energy distribution dominated by MeV-GeV photons. It is located at a distance of 2 kpc and consists of a compact object (black hole or neutron star) in an eccentric orbit around a 10-15Be star, with an orbital period of 26.496 days. The binary orbit modulates the emission ranging from radio to TeV energies. A second, longer, modulation period of 1667 days (the super-orbital period) has also been detected from radio to TeV observations. The VERITAS imaging atmospheric Cherenkov telescope array has been observing LS I +61°303 since 2006, and has accumulated a dataset that fully covers the entire orbit. Increased coverage of the source in the very-high-energy band is currently underway to provide more results on the modulation pattern, super-orbital period, and orbit-to-orbit variability at the highest energies. The spectral measurements at the highest energies will reveal more information about gamma-ray production/absorption mechanisms, the nature of the compact object, and the particle acceleration mechanism. Using >150 hrs of VERITAS data, we present a detailed study of the spectral energy distribution and periodic behavior of this rare gamma-ray source type at very-high energy.

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Optical spectroscopy of the Be/black hole binary MWC 656 ‐ interaction of a black hole with a circumstellar disc

et al. 2022

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We present new spectroscopic observations of the Be/black hole binary MWC 656 obtained during the period 2015–2021. We measure the equivalent width of Hα (EWα), Hβ (EWβ$$ {EW}_{\beta } $$), and the distance between the peaks of Hα (normalΔVα$$ \Delta {V}_{\alpha } $$), Hβ (normalΔVβ$$ \Delta {V}_{\beta } $$), and FeII (normalΔVFeII$$ \Delta {V}_{\mathrm{FeII}} $$) lines. Combining new and old data, we find that: (1) the density of the circumstellar disc of MWC 656 (normalΔVα$$ \Delta {V}_{\alpha } $$ versus EWα$$ {EW}_{\alpha } $$ diagram) is similar to the Be stars. For the Be stars, we find the relation normalΔVβ=0.999normalΔVα+62.4$$ \Delta {V}_{\beta }=0.999\Delta {V}_{\alpha }+62.4 $$ km s−1, and the position of MWC 656 corresponds to the average behavior of the Be stars. This means that the presence of the black hole does not change the overall structure of the circumstellar disc; (2) the periodogram analysis indicates modulation of EWα$$ {EW}_{\alpha } $$ with a period 60.4±0.4$$ 60.4\pm 0.4 $$ days, which is identical to the binary orbital period. The maxima of EWα$$ {EW}_{\alpha } $$ and EWβ$$ {EW}_{\beta } $$ are around periastron (phase zero); (3) around orbital phase zero, normalΔVβ$$ \Delta {V}_{\beta } $$ and normalΔVFeII$$ \Delta {V}_{FeII} $$ decrease by about 30$$ 30 $$ km s−1. This suggests that we observe an increase of the circumstellar disc size induced by the periastron passage of the black hole and that the entire circumstellar disc pulsates with the orbital period with relative amplitude of 10–20%. The observations also indicate, that the reason for the black hole in MWC 656 to be in deep quiescence is a very low efficiency of accretion (∼2×10−6$$ \sim 2\times {10}^{-6} $$).

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Orbital variability of the optical linear polarization of the γ-ray binary LS I +61° 303 and new constraints on the orbital parameters

Cited by 19 publications

References 52 publications

Optical and Near-Infrared Monitoring of Gamma-ray Binaries Hosting Be Stars

Optical and Near-Infrared Monitoring of Gamma-ray Binaries Hosting Be Stars

Very High Energy Gamma-ray Emission from the Binary System LS I +61 303

Optical spectroscopy of the Be/black hole binary MWC 656 ‐ interaction of a black hole with a circumstellar disc

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