Multi-epoch Doppler tomography and polarimetry of QQ Vul

Schwope, A. D.; Catalán, M. S.; Beuermann, K.; Metzner, André; Smith, Robert C.; Steeghs, D.

doi:10.1046/j.1365-8711.2000.03240.x

Cited by 55 publications

(49 citation statements)

References 19 publications

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“…The trailed spectra of the emission lines (Figure 3) look different from the ones shown by Schwope et al (2000). The tomograms of HeIA4921, HeIIA4686, and H/3 show a NEL and emission from the accretion stream.…”

Section: Qq Vulmentioning

confidence: 78%

“…To fill this gap and to get data of a quality already available for much fainter objects, we observed AM Her with the double-beam spectrograph TWIN at the 3.5m-telescope at Calar Alto (Spain) on June 5 and 6, 2000. We also observed QQ Vul (on June 4 and 7), for which there is some optical spectroscopy published (Schwope et al 2000). But in this system the trailed spectra and tomograms looked different whenever observations were performed.…”

Section: Introductionmentioning

confidence: 87%

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Tomography of AM Her and QQ Vul

Staude

Schwope

Hedelt

et al. 2004

International Astronomical Union Colloquium

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Section: Qq Vulmentioning

confidence: 78%

Section: Introductionmentioning

confidence: 87%

Tomography of AM Her and QQ Vul

Staude

Schwope

Hedelt

et al. 2004

International Astronomical Union Colloquium

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“…This novel approach rests on the assumption that the Doppler velocity in the not-yet magnetically threadened part of the stream reflects just the free-fall velocity with some thermal broadening. Multiepoch tomography of QQ Vul has cast doubt on this assumption (Schwope et al 2000). Watson et al (2003) used Roche tomography reconstructions of the secondary star in HU Aqr to derive the system parameters (M WD , M 2 , i, γ) from the shape of the entropy landscape.…”

Section: Discussionmentioning

confidence: 99%

Dissecting the donor star in the eclipsing polar HU Aquarii

Schwope

Horne

Steeghs

et al. 2011

A&A

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Medium-resolution spectroscopic observations with full phase coverage of the eclipsing polar HU Aqr are presented. Na i absorption and Ca ii emission lines are used to trace the secondary star. While the Na i lines seem to have contributions from both hemispheres of the donor star, the Ca ii lines were found to originate from the irradiated part of its surface alone. An irradiation model was applied and the irradiation-weighted radial velocity amplitude was used to determine the mass ratio Q = M WD /M 2 = 4.58 ± 0.20. When combined with high-speed photometric low-state eclipse light curves, the white dwarf mass is constrained to 0.75 < M WD /M < 0.84 with a best-fit value of M WD = (0.80 ± 0.04) M , and M 2 = (0.18 ± 0.06) M at an orbital inclination of i = 87• +0.8 −0.5 .

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“…The accretion regions on the white-dwarf primaries in polars can show asymmetric and extended shapes, as investigated in detail for instance by Wickramasinghe et al (1991) and Sirk & Howell (1998). Partial self-eclipses of such an extended accretion region have also been suggested by Beuermann et al (1987) for EF Eri on the basis of Einstein light curves and by Schwope et al (2000) for QQ Vul on the basis of polarimetric data. The soft X-ray emission of QS Tel is reduced by a factor of about ten during the faint phase, possibly by the self-eclipse of the inner part of the extended accretion region, while the mekal flux diminishes by a factor between two and three.…”

Section: A Partially Self-eclipsing Main Accretion Regionmentioning

confidence: 90%

XMM-Newtonobservations of the X-ray soft polar QS Telescopii

Traulsen¹,

Reinsch²,

Schwope³

et al. 2011

A&A

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Context. On the basis of XMM-Newton observations, we investigate the energy balance of selected magnetic cataclysmic variables, which have shown an extreme soft-to-hard X-ray flux ratio in the ROSAT All-Sky Survey. Aims. We intend to establish the X-ray properties of the system components, their flux contributions, and the accretion geometry of the X-ray soft polar QS Tel. In the context of high-resolution X-ray analyses of magnetic cataclysmic variables, this study will contribute to better understanding the accretion processes on magnetic white dwarfs. Methods. During an intermediate high state of accretion of QS Tel, we have obtained 20 ks of XMM-Newton data, corresponding to more than two orbital periods, accompanied by simultaneous optical photometry and phase-resolved spectroscopy. We analyze the multi-wavelength spectra and light curves and compare them to former high-and low-state observations. Results. Soft emission at energies below 2 keV dominates the X-ray light curves. The complex double-peaked maxima are disrupted by a sharp dip in the very soft energy range (0.1−0.5 keV), where the count rate abruptly drops to zero. The EPIC spectra are described by a minimally absorbed black body at 20 eV and two partially absorbed mekal plasma models with temperatures around 0.2 and 3 keV. The black-body-like component arises from one mainly active, soft X-ray bright accretion region nearly facing the mass donor. Parts of the plasma emission might be attributed to the second, virtually inactive pole. High soft-to-hard X-ray flux ratios and hardness ratios demonstrate that the high-energy emission of QS Tel is substantially dominated by its X-ray soft component.

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Multi-epoch Doppler tomography and polarimetry of QQ Vul

Cited by 55 publications

References 19 publications

Tomography of AM Her and QQ Vul

Tomography of AM Her and QQ Vul

Dissecting the donor star in the eclipsing polar HU Aquarii

XMM-Newtonobservations of the X-ray soft polar QS Telescopii

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