The newly discovered eclipsing cataclysmic star 2MASS J16211735 + 4412541 and its peculiarity

Kjurkchieva, D.; Popov, V.; Vasileva, D.; Petrov, N.

doi:10.1016/j.newast.2016.10.001

Cited by 11 publications

(13 citation statements)

References 28 publications

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“…Moreover, the strong rotational disturbance of the emission lines in the eclipse indicates the presence of a rapidly-rotating disk (Thorstensen 2016). Therefore, after the merging of a contact binary was ruled out to explain the outburst of J 162117, this event was attributed to a dwarf-nova outburst (Scaringi et al 2016;Kjurkchieva et al 2017). However, when comparing with known CVs, J 162117 shows several peculiarities (Kjurkchieva et al 2017), namely a deeper eclipse at outburst than at quiescence (by a factor 2.8) and outburst amplitudes at the lowest limit of dwarf nova eruptions.…”

Section: Discussionmentioning

confidence: 99%

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A New Stellar Outburst Associated with the Magnetic Activities of the K-type Dwarf in a White Dwarf Binary

Qian

Han

Zhang

et al. 2017

ApJ

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1SWASP J162117.36+441254.2 was originally classified as an EW-type binary with a period of 0.20785 days. However, it was detected to have undergone a stellar outburst on June 3, 2016. Although the system was latter classified as a cataclysmic variable (CV) and the event was attributed as a dwarf-nova outburst, the physical reason is still unknown. This binary has been monitored photometrically since April 19, 2016 and many light curves were obtained before, during and after the outburst. Those light and color curves observed before the outburst indicate that the system is a special CV. The white dwarf is not accreting material from the secondary and there are no accretion disks surrounding the white dwarf. By comparing the light curves obtained from April 19 to September 14, 2016, it was found that magnetic activity of the secondary is associated with the outburst. We show strong evidence that the L 1 region on the secondary was heavily spotted before and after the outburst and thus quench the mass transfer, while the outburst is produced by a sudden mass accretion of the white dwarf. These results suggest that J162117 is a good astrophysical laboratory to study stellar magnetic activity and its influences on CV mass transfer and mass accretion.

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Section: Discussionmentioning

confidence: 99%

“…After the report of the outburst from J 162117 (Drake et al 2016), the binary system was monitored continuously (Zejda & Pejcha 2016;Pavlenko et al 2016;Zola et al 2016;Kjurkchieva et al 2017). The phased light curve obtained by Zejda & Pejcha (2016) during the outburst showed deep primary eclipses and shallower secondary eclipses.…”

Section: Introductionmentioning

confidence: 99%

A New Stellar Outburst Associated with the Magnetic Activities of the K-type Dwarf in a White Dwarf Binary

Qian

Han

Zhang

et al. 2017

ApJ

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“…The non-sinusoidal nature of this light curve is likely to be due to starspots on the surface. The model published by Kjurkchieva et al (2017) included a cool spot on the secondary with a temperature factor of 0.9 and an angular size of 20 • .…”

Section: Published Survey Photometrymentioning

confidence: 99%

V1460 Her: a fast spinning white dwarf accreting from an evolved donor star

Ashley

Marsh

Breedt

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present time-resolved optical and ultraviolet spectroscopy and photometry of V1460 Her, an eclipsing cataclysmic variable with a 4.99 h orbital period and an overluminous K5-type donor star. The optical spectra show emission lines from an accretion disc along with absorption lines from the donor. We use these to measure radial velocities, which, together with constraints upon the orbital inclination from photometry, imply masses of M1 = 0.869 ± 0.006 M⊙ and M2 = 0.295 ± 0.004 M⊙ for the white dwarf and the donor. The radius of the donor, R2 = 0.43 ± 0.002 R⊙, is ≈50 per cent larger than expected given its mass, while its spectral type is much earlier than the M3.5 type that would be expected from a main sequence star with a similar mass. HST spectra show strong N v 1240 Å emission but no C iv 1550 Å emission, evidence for CNO-processed material. The donor is therefore a bloated, over-luminous remnant of a thermal-timescale stage of high mass transfer and has yet to re-establish thermal equilibrium. Remarkably, the HST ultraviolet data also show a strong 30 per cent peak-to-peak, 38.9 s pulsation that we explain as being due to the spin of the white dwarf, potentially putting V1460 Her in a similar category to the propeller system AE Aqr in terms of its spin frequency and evolutionary path. AE Aqr also features a post-thermal timescale mass donor, and V1460 Her may therefore be its weak magnetic field analogue since the accretion disc is still present, with the white dwarf spin-up a result of a recent high accretion rate.

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“…The magnitudes of the comparison and check stars (Table ) were taken from the catalog APASS DR9 (Henden et al ). The transformation of the obtained instrumental magnitudes into standard ones was made as reported in Kjurkchieva et al ().…”

Section: Observationsmentioning

confidence: 99%

Photometric and spectral observations of two W UMa stars with periods of one third of a day

2018

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Photometric and spectral observations of the W UMa binaries NSVS 254037 and V505 Lac with periods of around 8 hr are presented. The simultaneous light curve and radial velocity curve solutions revealed that their components are of G spectral type. The two targets undergo partial eclipses. They both have overcontact configurations of W subtype with fill‐out factor f ∼ 0.1. The derived parameters of NSVS 254037 are: mass ratio q = 2.42; orbital inclination i = 67.1°; temperatures T1 = 5800 K and T2 = 5585 K; masses M1 = 0.47 M⊙ and M2 = 1.15 M⊙; radii R1 = 0.72 R⊙ and R2 = 1.07 R⊙; luminosities L1 = 0.53 L⊙ and L2 = 1.0 L⊙; equatorial velocities V1 = 89 km−1 and V2 = 146 km−1; and distance d = 175 pc, almost the same as those of GAIA(DR2). The derived parameters of V505 Lac are: mass ratio q = 2.53; orbital inclination i = 57.30; temperatures T1 = 5,600 K and T2 = 5,166 K; masses M1 = 0.38 M⊙ and M2 = 0.97 M⊙; radii R1 = 0.69 R⊙ and R2 = 1.04 R⊙; luminosities L1 = 0.41 L⊙ and L2 = 0.68 L⊙; equatorial velocities V1 = 106 km−1 and V2 = 129 km−1; and distance d = 117 pc, smaller than those of GAIA by 19%. Thus, NSVS 254037 and V505 Lac turned out similar not only in periods and magnitudes but also in mass ratios, radii, and fill‐out factors.

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The newly discovered eclipsing cataclysmic star 2MASS J16211735 + 4412541 and its peculiarity

Cited by 11 publications

References 28 publications

A New Stellar Outburst Associated with the Magnetic Activities of the K-type Dwarf in a White Dwarf Binary

A New Stellar Outburst Associated with the Magnetic Activities of the K-type Dwarf in a White Dwarf Binary

V1460 Her: a fast spinning white dwarf accreting from an evolved donor star

Photometric and spectral observations of two W UMa stars with periods of one third of a day

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