A spectrophotometric study of RW Trianguli

Groot, P.; Rutten, R. G. M.; Paradijs, J. van

doi:10.1051/0004-6361:20031771

Cited by 27 publications

(29 citation statements)

References 21 publications

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“…In fact, multiple observations of eclipsing NLs show that the Hα line is only moderately eclipsed compared to the continuum (e.g. Baptista et al 2000;Groot et al 2004; see also section 5.4), implying a significant vertical extent for the line-forming region. This type of model should therefore not be ruled out a priori, but this specific model was not adopted as our optically optimized model due to its unrealistically high continuum level in eclipse.…”

Section: Line Profile Shapes: Producing Single-peaked Emissionmentioning

confidence: 99%

“…There, the single-peaked lines are often only weakly eclipsed, and a significant fraction of the line flux remains visible even near mid-eclipse (e.g. Baptista et al 2000;Groot et al 2004). This points to line formation in a spatially extended region, such as a disk wind (see Fig.…”

Section: Introductionmentioning

confidence: 96%

“…These spectra are typically characterized by H and He emission lines superposed on a blue continuum. In many cases, and particularly in the SW Sex subclass of NLs (Honeycutt et al 1986; T. Gaensicke, private communication) and RW Tri in and out of eclipse (bottom two panels; Groot et al 2004). The data for RW Sex and RW Tri were digitized from the respective publications, and the IX Vel spectrum was obtained using the XSHOOTER spectrograph on the Very Large Telescope on 2014 October 10.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Line Profile Shapes: Producing Single-peaked Emissionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 96%

Section: Introductionmentioning

confidence: 99%

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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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“…Nevertheless, some NLs above the 3−4 h period interval are found to exhibit some of the defining features of the SW Sex stars, like BT Mon ) and, more recently, RW Tri (Groot et al 2004). Beyond the realm of CVs, some Low Mass X-ray Binaries (LMXBs) may show distinctive SW Sex behaviour, such as e.g.…”

Section: Introductionmentioning

confidence: 99%

Time-resolved photometry and spectroscopy of the new deeply-eclipsing SW Sextantis star HS 0728+6738

Rodríguez‐Gil

Gänsicke

Barwig

et al. 2004

A&A

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Abstract. We present time-resolved optical spectroscopy and photometry, and far-ultraviolet spectroscopy of HS 0728+6738, a cataclysmic variable discovered in the Hamburg Quasar Survey. We show that the system is a new eclipsing member of the SW Sex class of CVs with an orbital period of 3.21 h. We derive an orbital inclination of ∼85 ± 4• from the average eclipse profile, making HS 0728+6738 the highest inclination SW Sex star known. The optical and far-ultraviolet emission lines are not or only weakly occulted during the eclipse, indicating the presence of line-emission sites either far outside the Roche lobe of the primary or, more likely, above the orbital plane of the binary. The photometric light curves exhibit fast variability with a period of ∼7 min, which might be related to the spin of the white dwarf.

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“…In the novalike subclass, the mass transfer rate from the secondary lies above the dwarf nova regime, and due to the subsequent higher disc temperatures (e.g. Rutten et al 1993 on UX UMa, and Groot et al 2004 on RW Tri), the accretion discs are stabilized against the dwarf nova instability mechanism. A detailed study of the structure of novalike and dwarf nova discs will therefore contribute to our understanding of the physics of accretion disc in various mass-transfer rates regimes.…”

Section: Introductionmentioning

confidence: 99%

Analysis of spiral structure in the accretion disc of the nova-like cataclysmic variable EC21178–5417

Ruiz-Carmona

Khangale

Woudt

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present an extensive Doppler tomography study of the eclipsing novalike EC21178-5417, which exhibits the classic accretion disc signature in the form of double-peak emission lines in its spectrum. Doppler tomograms confirm the presence of a strong, two-armed spiral pattern visible in the majority of the spectral lines studied. This makes EC21178-5417 one of the very few novalikes that show spiral structure in their discs. We also report night-to-night changes in the position and relative strength of the spiral arms, revealing fluctuations on the conditions in the accretion disc.

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A spectrophotometric study of RW Trianguli

Cited by 27 publications

References 21 publications

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

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

Time-resolved photometry and spectroscopy of the new deeply-eclipsing SW Sextantis star HS 0728+6738

Analysis of spiral structure in the accretion disc of the nova-like cataclysmic variable EC21178–5417

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