A spectroscopic analysis of the eclipsing nova-like EC 21178−5417 – discovery of spiral density structures

Khangale, Z. N.; Woudt, P. A.; Potter, S.; Warner, Brian D.; Kilkenny, D.; Heyden, K. van der

doi:10.1093/mnras/staa680

Cited by 5 publications

(4 citation statements)

References 45 publications

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“…The orbital inclination must be high in view of the deep eclipses in the light curves. This is confirmed by Khangale et al (2020) who estimate i = 83 o ± 7 o . The data available for this study consist of light curves already presented by Bruch (2017b).…”

Section: Appendix B: System Parameterssupporting

confidence: 64%

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A comparative study of the strength of flickering in cataclysmic variables

Bruch

2021

Preprint

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Flickering is a universal phenomenon in accreting astronomical systems which still defies detailed physical understanding. It is particularly evident in cataclysmic variables (CVs). Attempting to define boundary conditions for models, the strength of the flickering is measured in several thousand light curves of more than 100 CVs. The flickering amplitude is parameterized by the FWHM of a Gaussian fit to the magnitude distribution of data points in a light curve. This quantity requires several corrections before a comparison between different sources can be made. While no correlations of the flickering strength with simple parameters such as component masses, orbital inclination or period were detected, a dependence on the absolute magnitude of the primary component and on the CV subtype is found. In particular, flickering in VY Scl tpye novalike variables is systematically stronger than in UX UMa type novalikes. The broadband spectrum of the flickering light source can be fit by simple models but shows excess in the U band. When the data permitted to investigate the flickering strength as a function of orbital phase in eclipsing CVs, such a dependence was found, but it is different for different systems. Surprisingly, there are also indications for variations of the flickering strength with the superhump phase in novalike variables with permanent superhumps. In dwarf novae, the flickering amplitude is high during quiescence, drops quickly at an intermediate magnitude when the system enters into (or returns from) an outburst and, on average, remains constant above a given brightness threshold.

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Section: Appendix B: System Parameterssupporting

confidence: 64%

“…Time resolved photometry was published by Bruch (2017b) who measured the orbital period. It was refined by Khangale et al (2020) who published a spectroscopic analysis of the system. Component masses remain unknown.…”

Section: Appendix B: System Parametersmentioning

confidence: 99%

A comparative study of the strength of flickering in cataclysmic variables

Bruch

2021

Preprint

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“…The disk eclipsing variability seen in OGLE LMC-ECL-28271 is observed by both ASAS-SN and OGLE, making this system also unlikely to be a blend. Characterization of these exotic systems can be used to study unique stages of binary evolution (e.g., Østensen et al 2010;Khangale et al 2020).…”

Section: Discussionmentioning

confidence: 99%

“…Photometric observations of this system have identified quasi-periodic oscillations (QPOs) and dwarf-nova oscillations (DNOs, Warner et al 2003) in addition to the eclipses. Spectroscopic observations identified double-peaked HeII emission lines, suggesting an inclined accretion disk (Khangale et al 2020).…”

Section: White Dwarf+ms Disk Systemsmentioning

confidence: 96%

The value-added catalogue of ASAS-SN eclipsing binaries: parameters of 30 000 detached systems

Rowan

Jayasinghe

Stanek

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Detached eclipsing binaries are a fundamental tool for measuring the physical parameters of stars that are effectively evolving in isolation. Starting from more than 40,000 eclipsing binary candidates identified by the All-Sky Automated Survey for Supernovae (ASAS-SN), we use PHOEBE to determine the sum of the fractional radii, the ratio of effective temperatures, the inclinations, and the eccentricities for 35,576 systems. We visually inspect all the light curve models to verify the model fits and examine the TESS light curves, when available, to select systems with evidence for additional physics, such as spots, mass transfer, and hierarchical triples. We examine the distributions of the eclipsing binary model parameters and the orbital parameters. We identify two groups in the sum of the fractional radii and effective temperature ratio parameter space that may distinguish systems approaching the semidetached limit. Combining Gaia EDR3 with extinction estimates from 3-dimensional dust maps, we examine the properties of the systems as a function of their absolute magnitude and evolutionary state. Finally, we present light curves of selected eclipsing binaries that may be of interest for follow-up studies.

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

Subebekova

Zharikov²,

Tovmassian³

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We obtained photometric observations of the nova-like cataclysmic variable RW Tri and gathered all available AAVSO and other data from the literature. We determined the system parameters and found their uncertainties using the code developed by us to model the light curves of binary systems. New time-resolved optical spectroscopic observations of RW Tri were also obtained to study the properties of emission features produced by the system. The usual interpretation of the single-peaked emission lines in nova-like systems is related to the bi-conical wind from the accretion disc’s inner part. However, we found that the Hα emission profile is comprised of two components with different widths. We argue that the narrow component originates from the irradiated surface of the secondary, while the broader component’s source is an extended, low-velocity region in the outskirts of the accretion disc, located opposite to the collision point of the accretion stream and the disc. It appears to be a common feature for long-period nova-like systems – a point we discuss.

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A spectroscopic analysis of the eclipsing nova-like EC 21178−5417 – discovery of spiral density structures

Cited by 5 publications

References 45 publications

A comparative study of the strength of flickering in cataclysmic variables

A comparative study of the strength of flickering in cataclysmic variables

The value-added catalogue of ASAS-SN eclipsing binaries: parameters of 30 000 detached systems

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

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