Structure of accretion flows in the nova-like cataclysmic variable RW Tri

Subebekova, G.; Zharikov, S. V.; Tovmassian, G.; Neustroev, V.; Wolf, M.; Hernández, M. S.; Kučáková, H.; Khokhlov, S. A.

doi:10.1093/mnras/staa2091

Cited by 17 publications

(31 citation statements)

References 68 publications

(82 reference statements)

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“…The considerably large distinctions in system parameters indicate that RW Tri is still a mysterious NL variable. In spite of this, the masses of two components recently obtained by Smak [13] and Subebekova et al [14] are basically consistent.…”

Section: Introductionsupporting

confidence: 51%

“…Compared with the other databases and the published data, the similar out-of-eclipse magnitude of the AAVSO light curve indicates that RW Tri always maintains a steady-state accretion disk during the AAVSO observations. A total of 107 new and available light minimum times were obtained, of which 10 are the averages observed by the different observer, including 2 approaching the times obtained by Subebekova et al [14].…”

Section: Data From Aavsomentioning

confidence: 93%

“…Since the previous O-C analyses (e.g., [14,20]) never carried out a detailed verification for all datapoints, but only made the collections for the historical light minimum times available in the literature, a possibility that the data points with the large deviations (many were clearly seen in the historical O-C diagrams) resulted from the incorrect light minimum times, cannot be ruled out. A cross-identification for all the light minimum times from the literature found that some with the small differences are caused by the different observatories and filters, while some listed in O-C gateway [25] are different from the data published in the literature.…”

Section: Cross-identification Of Data From the Literaturementioning

confidence: 99%

“…Moreover, they never found any cyclical change claimed in the previous O-C analyses. By adding many new data points, the two recent O-C diagrams [14,20] again show a pure cyclical variation with a period approaching 40 years, without any secular change. Therefore, a careful verification for all the data including the historic and new observed data they used to carry out their own O-C analyses and the more supplemental new high-precision data may be helpful to solve this apparent controversy.…”

Section: Introductionmentioning

confidence: 97%

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A Brown Dwarf Companion to the Nova-like Variable RW Tri

Dai

Qian

Medagangoda³

2021

Galaxies

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The orbital period of Nova-like variable RW Tri is expected to experience a long-term evolution due to a stable mass transfer from the red dwarf to the white dwarf. By adding 297 new eclipse timings obtained from our own observations and a cross-identification of many databases, we fully reinvestigated the variations in orbital period of RW Tri, based on a total of 658 data points spanning over 80 years. The new O-C diagram demonstrates a more complicate pattern than a pure sinusoidal modulation shown in the previous O-C analyses. The best fit of the O-C variations is a quadratic-plus-sinusoidal curve with a period of 22.66 (2) years and a typical decrease rate of P˙ = −2d.32(4) × 10−9 yr−1. To explain secular orbital period decrease, the magnetic braking effect is required to cause the orbital angular moment loss in RW Tri with a mass ratio less than unity, while a conserved mass transfer is also enough for RW Tri with a mass ratio larger than unity. No matter what the mass ratio is, a slightly enhanced mass transfer rate, 2.4–5.3 × 10−9 M⊙ yr−1, derived from our O-C diagram, providing an evidence supporting the disk instability model and the standard/revised models of cataclysmic variable evolution, is almost the same as that obtained from the light-curve modeling. This further confirms our observed orbital period decrease and the controversial system parameter, mass transfer rate. Our updated O-C analysis further verifies the claimed cyclical changes of orbital period with a period range of 21–24 years, which is approximately one half of the results in the literature. In accordance with the light-travel time effect, this periodical variation shown in our new O-C diagram indicates a brown dwarf hidden in RW Tri at a coplanar orbit. Note that the large scatter in the data range of 0–3 × 104 cycles requires the high-precision photometry in the longer base line in the future.

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Section: Introductionsupporting

confidence: 51%

Section: Data From Aavsomentioning

confidence: 93%

Section: Cross-identification Of Data From the Literaturementioning

confidence: 99%

Section: Introductionmentioning

confidence: 97%

See 2 more Smart Citations

A Brown Dwarf Companion to the Nova-like Variable RW Tri

Dai

Qian

Medagangoda³

2021

Galaxies

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“…Some evidence for a possible expansion of accretion disc material beyond the Roche lobe has been presented for long-period nova-like CVs (see e.g. Hernandez et al 2017;Subebekova et al 2020). However, to the best of our knowledge, the observational confirmation of such an expansion in a short-period CV is obtained for the first time.…”

Section: Discussionmentioning

confidence: 67%

Voracious vortices in cataclysmic variables

Neustroev

Zharikov²

2020

A&A

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Context. In Paper I we showed that the accretion disc radius of the dwarf nova HT Cas in its quiescent state has not changed significantly during many years of observations. It has remained consistently large, close to the tidal truncation radius. This result is inconsistent with the modern understanding of the evolution of the disc radius through an outburst cycle. Aims. Spectroscopic observations of HT Cas during its superoutburst offered us an exceptional opportunity to compare the properties of the disc of this object in superoutburst and in quiescence. Methods. We obtained a new set of time-resolved spectra of HT Cas in the middle of its 2017 superoutburst. We used Doppler tomography to map emission structures in the system, which we compared with those detected during the quiescent state. We used solutions of the restricted three-body problem to discuss again the location of emission structures and the disc size of HT Cas in quiescence. Results. The superoutburst spectrum is similar in appearance to the quiescent spectra, although the strength of most of the emission lines decreased. However, the high-excitation lines significantly strengthened in comparison with the Balmer lines. Many lines show a mix of broad emission and narrow absorption components. Hα in superoutburst was much narrower than in quiescence. Other emission lines have also narrowed in outburst, but they did not become as narrow as Hα. Doppler maps of Hα in quiescence and of the Hβ and He I lines in outburst are dominated by a bright emission arc at the right side of the tomograms, which is located at and even beyond the theoretical truncation limit. However, the bulk of the Hα emission in outburst has significantly lower velocities. Conclusions. We show that the accretion disc radius of HT Cas during its superoutburst has become hot but remained the same size as it was in quiescence. Instead, we detected cool gas beyond the Roche lobe of the white dwarf that may have been expelled from the hot disc during the superoutburst.

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Structure of the accretion flow of IX Velorum as revealed by high-resolution spectroscopy

Kára,

Schmidtobreick,

Pala

et al. 2023

A&A

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Context. Several high mass-transfer cataclysmic variables show evidence of outflow from the system, which could play an important role in their evolution. We investigate the system IX Vel, which was proposed to show similar characteristics. Aims. We study the structure of the IX Vel system, particularly the structure of its accretion flow and accretion disc. Methods. We used high-resolution time-resolved spectroscopy to construct radial velocity curves of the components in IX Vel. We computed Doppler maps of the system, which we used to estimate the temperature distribution maps. Results. We have improved the spectroscopic ephemeris of the system and its orbital period Porb = 0.19392793(3) d. We constructed Doppler maps of the system based on hydrogen and helium emission lines and the Bowen blend. The maps show features corresponding to the irradiated face of the secondary star, the outer rim of the accretion disc, and low-velocity components located outside the accretion disc and reaching towards L3. We constructed a temperature distribution map of the system using the Doppler maps of Balmer lines. Apart from the features found in the Doppler maps, the temperature distribution map shows a region of high temperature in the accretion disc connecting the expected position of a bright spot and the inner parts of the disc. Conclusions. We interpret the low-velocity emission found in the Doppler map as emission originating in the accretion disc wind and in an outflow region located in the vicinity of the third Lagrangian point L3. This makes IX Vel a member of the RW Sex class of cataclysmic variables.

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Structure of accretion flows in the nova-like cataclysmic variable RW Tri

Cited by 17 publications

References 68 publications

A Brown Dwarf Companion to the Nova-like Variable RW Tri

A Brown Dwarf Companion to the Nova-like Variable RW Tri

Voracious vortices in cataclysmic variables

Structure of the accretion flow of IX Velorum as revealed by high-resolution spectroscopy

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