Radius, rotational period, and inclination of the Be stars in the Be/gamma‐ray binaries<scp>MWC</scp>148 and<scp>MWC</scp>656

Zamanov, R.; Stoyanov, K. A.; Martı́, Josep; Marchev, V. D.; Nikolov, Y.

doi:10.1002/asna.202123856

Cited by 10 publications

(15 citation statements)

References 41 publications

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“…The 2MASS colours (Phillips 2007) and the mean quiescent V − I c ∼ 4.2 (this paper) are consistent with M5 III (T eff = 3400 K; sec. 3.3) and the reddening E B−V = 0.7 ±0.1, which agrees with the total Galactic extinction E B−V < 0.80 ±0.04 (Schlafly & Finkbeiner 2011) and is consistent with E B−V = 0.81 ±0.10 (Zamanov et al 2021), as well as marginally consistent with E B−V ∼ 1 ±0.3 estimated by Mikołajewska et al (1997). We adopt the distance d = 6.9 kpc and E B−V = 0.7 for the rest of the paper.…”

Section: Red Giant and Distancesupporting

confidence: 91%

The symbiotic binary St 2-22: Orbital and stellar parameters and jet evolution following its 2019 outburst

Galan,

Mikolajewska,

Ilkiewicz

et al. 2021

Preprint

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Context. St 2-22 is a relatively poorly studied S-type symbiotic system that belongs to a small group of jet-producing systems as a result of disc accretion onto a white dwarf fed by its red giant companion. Aims. The goal of this paper is to analyse the nature and derive the basic parameters of St 2-22, and to follow the jet evolution. Methods. Photometric monitoring for over 16 yrs and high-quality spectroscopic data enabled us to shed new light on its nature. The high-resolution SALT spectra and V I C photometry obtained during and between the last two outbursts have been used to search for periodic changes, to derive spectroscopic orbits of both system components, and to study the outburst and jet evolution. Results. We present the orbital and stellar parameters of the system components. The orbital period is P orb = 918 ±6 d . The doubleline spectroscopic orbits indicate the mass ratio q = M g M −1 h = 3.50 ±0.53, and the components masses M g sin 3 i ∼ 2.35 M and M h sin 3 i ∼ 0.67 M . The orbit shows significant eccentricity, e = 0.16 ±0.07. The orbital inclination is close to 70 • . During outbursts, accelerating and decelerating jets are observed with changes in their radial velocity component in a range from ∼ 1500 up to nearly 1800 km s −1 . St 2-22 turned out to be a classical symbiotic system very similar to the precursor of the group -Z And.

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Section: Red Giant and Distancesupporting

confidence: 91%

The symbiotic binary St 2-22: Orbital and stellar parameters and jet evolution following its 2019 outburst

Galan,

Mikolajewska,

Ilkiewicz

et al. 2021

Preprint

Self Cite

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“…Using Eq. 5, Zamanov et al, 2021), and from the measurements of , we estimate the size of the circumstellar disc in MWC 656 to be in the range 123 ≤ ≤ 174 R ⊙ , with average value = 141 ± 8 R ⊙ . The distance between the peaks of H is in the range 214 ≤ Δ ≤ 282 km s −1 , with average value 255 ± 14 km s −1 .…”

Section: Figurementioning

confidence: 89%

“…The points lie close to and slightly above the average line. For the projected rotational velocity of the primary component of MWC 656 we used sin = 313 km s −1 (R. K. Zamanov, Stoyanov, Mart, Marchev, & Nikolov, 2021). The use of sin = 330 km s −1 (Casares et al, 2014), will move the points slightly down and they will be even closer to the average line.…”

Section: Disc Structurementioning

confidence: 99%

Optical spectroscopy of the Be/black hole binary MWC656 -- interaction of a black hole with a circumstellar disc

Zamanov,

Stoyanov,

Marchev

et al. 2022

Preprint

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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 H (EW ), H ( ), and the distance between the peaks of H (Δ ), H (Δ ), and FeII (Δ ) lines. Combining new and old data, we find that:-the density of the circumstellar disc of MWC 656 (Δ versus diagram) is similar to the Be stars. For the Be stars we find the relation Δ = 0.999Δ + 62.4 km s −1 , and the position of MWC 656 corresponds to the average behaviour of the Be stars. This means that the presence of the black hole does not change the overall structure of the circumstellar disc.-the periodogram analysis indicates modulation of with a period 60.4 ± 0.4 days, which is identical to the binary orbital period. The maxima of and are around periastron (phase zero). -around orbital phase zero, Δ and Δ decrease by about 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 ).

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“…9. Among the two possible scenarios, we first consider the one based on rotation because of the 0.6 d period persistency over several month scales, its proposed detection in a few gammaray binaries (Zamanov et al 2021), and the abundant rotation evidences found by the TESS observatory, not only in A-type stars, but also in B-type ones such as ours (Balona et al 2019). The fraction of rotational variables reported appears to be similar in both spectral types (about 40%).…”

Section: Parametermentioning

confidence: 99%

Orbital and sub-orbital period determination of the candidate high-mass X-ray binary HD 3191

Martı́

Luque-Escamilla

Sánchez-Ayaso

et al. 2021

A&A

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Aims. The final aim of this paper is to expand the sparse group of X-ray binaries with gamma-ray counterparts as laboratories to study high-energy processes under physical conditions that periodically repeat. Methods. A follow-up of a candidate system has been carried out. We applied both photometric and spectroscopic techniques in the optical domain together with a period analysis using the phase dispersion minimisation and CLEAN methods. A tentative period search was also conducted in the gamma-ray domain. Results. Our main result is having established the binary nature of the optical star and X-ray emitter HD 3191 towards the Fermi gamma-ray source 4FGL J0035.8+6131, the last one proposed to be associated with a blazar of an unknown type. An orbital period close to 16 d is reported for HD 3191 together with a likely rotation, or pulsation, period of about 0.6 d. Although no convincing evidence for the orbital cycle has been found in the Fermi light curve up to now, the confirmed presence of a high-mass X-ray binary towards 4FGL J0035.8+6131 now strengthens the need for caution about its true nature.

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

Cited by 10 publications

References 41 publications

The symbiotic binary St 2-22: Orbital and stellar parameters and jet evolution following its 2019 outburst

The symbiotic binary St 2-22: Orbital and stellar parameters and jet evolution following its 2019 outburst

Optical spectroscopy of the Be/black hole binary MWC656 -- interaction of a black hole with a circumstellar disc

Orbital and sub-orbital period determination of the candidate high-mass X-ray binary HD 3191

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