Doppler tomography and photometry of the cataclysmic variable 1RXS J064434.5+334451

Santisteban, J. V. Hernández; Echevarría, J.; Michel, R.; Costero, R.

doi:10.1093/mnras/stw2282

Cited by 8 publications

(12 citation statements)

References 26 publications

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“…This allows us to determine exactly the phase 0.0 of the system and make an effort to identify the definite locations of emission-line sources. However, as we already noted, the system parameters determined by Sing et al (2007), Hernández Santisteban (2012), Echevarria (2015), and Hernández Santisteban et al (2017) for 1RXS J064434.5+334451 do not agree.. Moreover, we note that the system parameters of Hernández Santisteban (2012) and Hernández Santisteban et al (2017) do not seem realistic because a secondary star with a mass of M2≥0.79M ⊙ , as it follows from their measurements, noticeably exceeds its Roche lobe for the given orbital period, regardless of whether it is on the main sequence or evolved 3 .…”

Section: Revisiting 1rxs J0644345+334451mentioning

confidence: 78%

“…Spectra of 1RXS J064434.5+334451 were obtained by Hernández Santisteban (2012) and Hernández Santisteban et al (2017) using the same instrument/telescope set-up as in the case of RW Sex, at the same observatory. Moreover, they obtained the time-resolved photometry of the object with the 1.5-m telescope also located at OAN SPM.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…We fitted the combined V−band light curve of 1RXS J064434.5+334451 using the same eclipse modelling technique as in Zharikov et al (2013) and Tovmassian et al (2014). Additionally, in section 4.2 we also reanalyzed spectral data from Hernández Santisteban (2012); Hernández Santisteban et al (2017) with the using newly defined system parameters to determine the location of the 'wide' emission component source in 1RXS J064434.5+334451. Fig.…”

Section: Revisiting 1rxs J0644345+334451mentioning

confidence: 99%

“…Sing et al (2007) reported this object as a deep eclipsing CV with the orbital period of Porb = 0.26937d and derived the physical parameters of the system, such as the WD mass M1 = 0.66M ⊙ , the mass ratio q = 0.78 and the WD temperature TWD∼25 000 K. They classified the system as a NL CV of the UX UMa-type or the SW Sex-type. Hernández Santisteban (2012), Echevarria (2015), and Hernández Santisteban et al (2017) recently reported new time-resolved photometry and echelle spectroscopy of 1RXS J064434.5+334451. They constructed Doppler maps of the system in the Hα, Hβ, and He II 4686 emission lines and refined system parameters based on the obtained data.…”

Section: Introductionmentioning

confidence: 98%

“…They constructed Doppler maps of the system in the Hα, Hβ, and He II 4686 emission lines and refined system parameters based on the obtained data. The WD with M1 = 0.82 ± 0.06M ⊙ and the mass ratio q = 0.96 ± 0.05 were proposed assuming the system inclination of i=78 • ± 2 in Hernández Santisteban et al (2017) that is in a disagreement with Sing et al (2007) and their own recent estimations: M1 = 0.91 ± 0.04M ⊙ , q = 0.91±0.09 from Hernández Santisteban (2012) and M1 = 0.76 ± 0.04M ⊙ , q = 0.75 ± 0.1 from Echevarria (2015). Regardless of different inclination angles, the Doppler maps of Balmer lines of 1RXS J064434.5+334451 and RW Sex are very similar.…”

Section: Introductionmentioning

confidence: 99%

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Structure of accretion flows in nova-like cataclysmic variables: RW Sextantis and 1RXS J064434.5+334451

Hernández

Zharikov

Neustroev

et al. 2017

Monthly Notices of the Royal Astronomical Society

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New time-resolved optical spectroscopic echelle observations of the nova-like cataclysmic variable RW Sextantis were obtained, with the aim to study the properties of emission features in the system. The profile of the Hα emission line can be clearly divided into two ('narrow' and 'wide') components. Similar emission profiles are observed in another nova-like system, 1RXS J064434.5+33445, for which we also reanalysed the spectral data and redetermined the system parameters. The source of the 'narrow', low-velocity component is the irradiated face of the secondary star. We disentangled and removed the 'narrow' component from the Hα profile to study the origin and structure of the region emitting the wide component. We found that the 'wide' component is not related to the white dwarf or the wind from the central part of the accretion disc, but is emanated from the outer side of the disc. Inspection of literature on similar systems indicates that this feature is common for some other long-period nova-like variables. We propose that the source of the 'wide' component is an extended, low-velocity region in the outskirts of the opposite side of the accretion disc, with respect to the collision point of the accretion stream and the disc.

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Section: Revisiting 1rxs J0644345+334451mentioning

confidence: 78%

Section: Observations and Data Reductionmentioning

confidence: 99%

Section: Revisiting 1rxs J0644345+334451mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

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Structure of accretion flows in nova-like cataclysmic variables: RW Sextantis and 1RXS J064434.5+334451

Hernández

Zharikov

Neustroev

et al. 2017

Monthly Notices of the Royal Astronomical Society

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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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New radial velocity observations of AH Her: evidence for material outside the tidal radius

Echevarría

Santisteban

Montero

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Spectroscopic observations of AH Herculis during a deep quiescent state are put forward. We found the object in a rare long minima, allowing us to derive accurately the semi-amplitudes: K1 = 121 ± 4 km s−1 and K2 = 152 ± 2 km s−1 and its mass functions MWsin 3i = 0.30 ± 0.01 M⊙ and MRsin 3i = 0.24 ± 0.02 M⊙, while its binary separation is given by asin i = 1.39 ± 0.02 R⊙. The orbital period Porb = 0.25812 ± 0.00032 days was found from a power spectrum analysis of the radial velocities of the secondary star. These values are consistent with those determined by Horne et al. (1986). Our observations indicate that K5 is the most likely spectral type of the secondary. We discuss why we favour the assumption that the donor in AH Her is a slightly evolved star, in which case we find that the best solution for the inclination yields i = 48○ ± 2○. Nonetheless, should the donor be a ZAMS star, we obtain that the inclination is between i = 43○ and i = 44○. We also present Doppler tomography of Hα and Hβ, and found that the emission in both lines is concentrated in a large asymmetric region at low velocities, but at an opposite position to the secondary star, outside the tidal radius and therefore at an unstable position. We also analyse the Hα and Hβ line profiles, which show a single broad peak and compare it with the previous quiescent state study which shows a double-peaked profile, providing evidence for its transient nature.

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Doppler tomography and photometry of the cataclysmic variable 1RXS J064434.5+334451

Cited by 8 publications

References 26 publications

Structure of accretion flows in nova-like cataclysmic variables: RW Sextantis and 1RXS J064434.5+334451

Structure of accretion flows in nova-like cataclysmic variables: RW Sextantis and 1RXS J064434.5+334451

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

New radial velocity observations of AH Her: evidence for material outside the tidal radius

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