Dark spot, spiral waves and the SW Sextantis behaviour: it is all about UX Ursae Majoris

Neustroev, V.; Suleimanov, V.; Borisov, N. V.; Belyakov, K. V.; Shearer, A.

doi:10.1111/j.1365-2966.2010.17495.x

Cited by 33 publications

(26 citation statements)

References 67 publications

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“…The high excitation line Heii λ4686 ( right panels) is seen in the tomogram as a single blob of material around or close to the WD centred at (Vx,Vy)= (+0,-200) km s −1 . These tomograms are consistent with previous studies on NL-type systems (Kaitchuck et al 1994;Neustroev et al 2011).…”

Section: Doppler Tomographysupporting

confidence: 92%

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

Santisteban

Echevarría

Michel³

et al. 2016

Mon. Not. R. Astron. Soc.

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We have obtained simultaneous photometric and spectroscopic observations of the cataclysmic variable 1RXS J064434.5+334451. We have calibrated the spectra for slit losses using the simultaneous photometry allowing to construct reliable Doppler images from Hα and Heii 4686Å emission lines. We have improved the ephemeris of the object based on new photometric eclipse timings, obtaining HJD = 2453403.759533+ 0.26937446E. Some eclipses present a clear internal structure which we attribute to a central Heii emission region surrounding the white dwarf, a finding supported by the Doppler tomography. This indicates that the system has a large inclination angle i = 78 ± 2 • . We have also analyzed the radial velocity curve from the emission lines to measure its semi-amplitude, K 1 , from Hα and Heii 4686 and derive the masses of the components: M 1 = 0.82 ± 0.06 M , M 2 = 0.78 ± 0.04 M and their separation a = 2.01 ± 0.06 R . The Doppler tomography and other observed features in this nova-like system strongly suggests that this is a SW Sex-type system.

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Section: Doppler Tomographysupporting

confidence: 92%

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

Santisteban

Echevarría

Michel³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Moreover, the line-to-continuum contrast increases during eclipse, as expected for emission produced in a disk wind. This trend is in line with the observations of RW Tri, and it has also been seen in other NLs, including members of the SW Sex class (Neustroev et al 2011). As noted in section 5.2, the majority of the escaping radiation has been reprocessed by the wind in some way (particularly the eclipsed light).…”

Section: Comparison To Rw Trisupporting

confidence: 88%

The impact of accretion disc winds on the optical spectra of cataclysmic variables

Matthews¹,

Knigge²,

Long³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Many high-state non-magnetic cataclysmic variables (CVs) exhibit blue-shifted absorption or P-Cygni profiles associated with ultraviolet (UV) resonance lines. These features imply the existence of powerful accretion disk winds in CVs. Here, we use our Monte Carlo ionization and radiative transfer code to investigate whether disk wind models that produce realistic UV line profiles are also likely to generate observationally significant recombination line and continuum emission in the optical waveband. We also test whether outflows may be responsible for the single-peaked emission line profiles often seen in high-state CVs and for the weakness of the Balmer absorption edge (relative to simple models of optically thick accretion disks). We find that a standard disk wind model that is successful in reproducing the UV spectra of CVs also leaves a noticeable imprint on the optical spectrum, particularly for systems viewed at high inclination. The strongest optical wind-formed recombination lines are Hα and He ii λ4686. We demonstrate that a higher-density outflow model produces all the expected H and He lines and produces a recombination continuum that can fill in the Balmer jump at high inclinations. This model displays reasonable verisimilitude with the optical spectrum of RW Trianguli. No single-peaked emission is seen, although we observe a narrowing of the double-peaked emission lines from the base of the wind. Finally, we show that even denser models can produce a single-peaked Hα line. On the basis of our results, we suggest that winds can modify, and perhaps even dominate, the line and continuum emission from CVs.

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“…This change in spectral features from emission to absorption is attributed to variability of the mass transfer rate from the secondary star to the WD, or, at times EC21178-5417 is dominated by an additional absorption component associated with the bright spot. Recently, UX UMa was reported to show similar variations on a yet undetermined time scale (Neustroev et al 2011). We have seen that the bright spot appears strong at 0.75 ≤ φ ≤ 0.95 (Section 4.2), and the higher Balmer lines change to absorption when the bright spot is visible.…”

Section: Discussionsupporting

confidence: 54%

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

Khangale

Woudt

Potter

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present phase-resolved optical spectroscopy of the eclipsing nova-like cataclysmic variable EC21178-5417 obtained between 2002 and 2013. The average spectrum of EC21178-5417 shows broad double-peaked emission lines from HeII 4686Å (strongest feature) and the Balmer series. The high-excitation feature, CIII/NIII at 4640-4650Å, is also present and appears broad in emission. A number of other lines, mostly HeI, are clearly present in absorption and/or emission. The average spectrum of EC21178-5417 taken at different months and years shows variability in spectral features, especially in the Balmer lines beyond Hγ, from pure line emission, mixed line absorption and emission to pure absorption lines. Doppler maps of the HeII 4686Å emission reveal the presence of a highly-inclined asymmetric accretion disc and a two spiral armlike structure, whereas that of the Balmer lines (Hα and Hβ) reveal a more circular accretion disc. There is no evidence of a bright spot in the Doppler maps of EC21178-5417 and no emission from the secondary star is seen in the tomograms of the HeII 4686Å and Balmer lines. Generally, the emission in EC21178-5417 is dominated by emission from the accretion disc. We conclude that EC21178-5417 is a member of the RW Tri or UX UMa sub-type of nova-like variables based on these results and because it shows different spectral characteristics at different dates. This spectral behaviour suggests that EC21178-5417 undergoes distinct variations in mass transfer rate on the observed time scales of months and years.

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Dark spot, spiral waves and the SW Sextantis behaviour: it is all about UX Ursae Majoris

Cited by 33 publications

References 67 publications

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

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

The impact of accretion disc winds on the optical spectra of cataclysmic variables

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

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