Images of accretion discs - II. Doppler tomography

Marsh, T. R.; Horne, K.

doi:10.1093/mnras/235.1.269

Cited by 426 publications

(405 citation statements)

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“…in the trailed spectrogram of the Hα line we used Doppler tomography (Marsh & Horne 1988). We used the MODMAP code described in Steeghs (2003) to reconstruct the Doppler map shown in Figure 5, using all the data from May 5th 2013.…”

Section: Prominence Featuresmentioning

confidence: 99%

The crowded magnetosphere of the post-common-envelope binary QS Virginis

Parsons

Hill

Marsh

et al. 2016

Mon. Not. R. Astron. Soc.

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We present high speed photometry and high resolution spectroscopy of the eclipsing post common envelope binary QS Virginis (QS Vir). Our UVES spectra span multiple orbits over more than a year and reveal the presence of several large prominences passing in front of both the M star and its white dwarf companion, allowing us to triangulate their positions. Despite showing small variations on a timescale of days, they persist for more than a year and may last decades. One large prominence extends almost three stellar radii from the M star. Roche tomography reveals that the M star is heavily spotted and that these spots are longlived and in relatively fixed locations, preferentially found on the hemisphere facing the white dwarf. We also determine precise binary and physical parameters for the system. We find that the 14, 220 ± 350 K white dwarf is relatively massive, 0.782 ± 0.013M ⊙ , and has a radius of 0.01068 ± 0.00007R ⊙ , consistent with evolutionary models. The tidally distorted M star has a mass of 0.382 ± 0.006M ⊙ and a radius of 0.381 ± 0.003R ⊙ , also consistent with evolutionary models. We find that the magnesium absorption line from the white dwarf is broader than expected. This could be due to rotation (implying a spin period of only ∼700 seconds), or due to a weak (∼100kG) magnetic field, we favour the latter interpretation. Since the M star's radius is still within its Roche lobe and there is no evidence that its over-inflated we conclude that QS Vir is most likely a pre-cataclysmic binary just about to become semi-detached.

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Section: Prominence Featuresmentioning

confidence: 99%

The crowded magnetosphere of the post-common-envelope binary QS Virginis

Parsons

Hill

Marsh

et al. 2016

Mon. Not. R. Astron. Soc.

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“…This filtered back-projection formula can be extended to the next dimension to calculate f (v x , v y , v z ) (see Appendix of Marsh & Horne 1988).…”

Section: Tomographymentioning

confidence: 99%

“…A notable reconstruction of the surface of Venus in Cartesian coordinates was achieved with the use of radar data since the surface is obscured by thick clouds; the reconstruction was achieved with data collected by the Magellan satellite which orbited the planet for four years. However, applications to eclipsing binaries and rotating stars (which provide us with changing views of the system) require the use of spectra, and the technique is termed "Doppler tomography" since the gas motions detected through Doppler shifts are used to provide an image of the gas flows in velocity coordinates (e.g., Marsh & Horne 1988).…”

Section: Application To Interacting Binary Star Systemsmentioning

confidence: 99%

Tomography of Interacting Binary Systems: Algols to Gamma-Ray Binaries

Richards

2011

Proc. IAU

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Abstract. Three-dimensional Doppler tomography of interacting binaries has now provided some interesting perspectives of the gas flows beyond the central plane corresponding to the orbital plane. These images suggest that the magnetic field of the mass losing star influences the gas flows in some cases. Earlier 2D tomograms displayed evidence of gas flows associated with the gas stream, accretion disks, accretion annuli, and hot spots as well as evidence of magnetic flows associated with the mass loser. These indirect images have revealed the active environments that exist in the slow-mass-transfer Algols, cataclysmic variables, polars, x-ray binaries, and gamma ray binaries.

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“…One of these methods is the Doppler tomography (Marsh & Horne 1988), where the system emissivity is reconstructed from the observed line profiles. Diaz (2001) proposed an extension of the Doppler tomography, the flickering tomography, where the line profile variability is mapped.…”

Section: Introductionmentioning

confidence: 99%

Tomographic Simulations of Accretion Disks in Cataclysmic Variables – Flickering and Wind

Ribeiro

Diaz

2006

Astrophys Space Sci

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Both continuum and emission line flickering are phenomena directly associated with the mass accretion process. In this work we simulate accretion disk Doppler maps including the effects of winds and flickering flares. Synthetic flickering Doppler maps are calculated and the effect of the flickering parameters on the maps is explored. Jets and winds occur in many astrophysical objects where accretion disks are present. Jets are generally absent among the cataclysmic variables (CVs), but there is evidence of mass loss by wind in many objects. CVs are ideal objects to study accretion disks and consequently to study the wind associated with these disks. We also present simulations of accretion disks including the presence of a wind with orbital phase resolution. Synthetic Hα line profiles in the optical region are obtained and their corresponding Doppler maps are calculated. The effect of the wind simulation parameters on the wind line profiles is also explored. From this study we verified that optically thick lines and/or emission by diffuse material into the primary Roche lobe are necessary to generate single peaked line profiles, often seen in CVs. The future accounting of these effects is suggested for interpreting Doppler tomography reconstructions.

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Images of accretion discs - II. Doppler tomography

Cited by 426 publications

References 0 publications

The crowded magnetosphere of the post-common-envelope binary QS Virginis

The crowded magnetosphere of the post-common-envelope binary QS Virginis

Tomography of Interacting Binary Systems: Algols to Gamma-Ray Binaries

Tomographic Simulations of Accretion Disks in Cataclysmic Variables – Flickering and Wind

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