Hubble Space Telescope and R-Band Eclipse Maps of the UX Ursae Majoris Accretion Disk

Baptista, R.; Horne, K.; Hilditch, R. W.; Mason, K. O.; Drew, J. E.

doi:10.1086/175970

Cited by 67 publications

(148 citation statements)

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“…Therefore, the spectrum emitted by different regions of the accretion disc may be very distinct. Furthermore, aside of the component stars and the accretion disc, additional sources contribute to the integrated light from the binary: a bright spot (BS) or stream forms where the gas from the mass-donor star hits the Raymundo Baptista Departamento de Física, UFSC, Campus Trindade, 88040-900, Florianópolis, Brazil, e-mail: raybap@gmail.com outer edge of the disc, tidally-induced spiral structures might develop in the outer regions of extended discs [59,8], and a fraction of the transferred mass may also be ejected from the binary in a wind from the disc surface [9,38]. Because what one directly observes is the combination of the spectra emitted from these diverse regions and sources, the interpretation of CVs observations is usually plagued by the ambiguity associated with composite spectra.…”

Section: Context and Motivationsmentioning

confidence: 99%

“…The lines and optically thin continuum emission are most probably emitted in a vertically extended disc chromosphere + wind [9,38]. This additional source of radiation may be responsible both for flattening the ultraviolet spectral slope and for filling in the Balmer jump of the optically thick disc spectrum, and might explain the historical difficulties in fitting integrated disc spectrum with stellar atmosphere disc models [61,25,41,39].…”

Section: Spectral Mapping: Spatially-resolved Disc Spectramentioning

confidence: 99%

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Eclipse Mapping: Astrotomography of Accretion Discs

Baptista¹

2016

Astronomy at High Angular Resolution

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The Eclipse Mapping Method is an indirect imaging technique that transforms the shape of the eclipse light curve into a map of the surface brightness distribution of the occulted regions. Three decades of application of this technique to the investigation of the structure, the spectrum and the time evolution of accretion discs around white dwarfs in cataclysmic variables have enriched our understanding of these accretion devices with a wealth of details such as (but not limited to) moving heating/cooling waves during outbursts in dwarf novae, tidally-induced spiral shocks of emitting gas with sub-Keplerian velocities, elliptical precessing discs associated to superhumps, and measurements of the radial run of the disc viscosity through the mapping of the disc flickering sources. This chapter reviews the principles of the method, discusses its performance, limitations, useful error propagation procedures, and highlights a selection of applications aimed at showing the possible scientific problems that have been and may be addresses with it.

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Section: Context and Motivationsmentioning

confidence: 99%

Section: Spectral Mapping: Spatially-resolved Disc Spectramentioning

confidence: 99%

Eclipse Mapping: Astrotomography of Accretion Discs

Baptista¹

2016

Astronomy at High Angular Resolution

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“…First, the eclipse mapping procedure projects any emission produced at height z above the disc back along the inclined line of sight to the point where it pierces the disc plane, at a distance z tan i away from the secondary star with respect to its true position (Baptista et al 1995). Conversely, if the spiral structures are produced in vertically-extended disc regions, their true positions would be at a distance z tan i towards the secondary star.…”

Section: Spiral Structures: Shocks or Irradiation Effects?mentioning

confidence: 99%

Tracing the spiral arms in IP Pegasi

Baptista¹,

Morales-Rueda²,

Harlaftis

et al. 2005

A&A

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We report the analysis of time-resolved spectroscopy of IP Pegasi in outburst with eclipse mapping techniques to investigate the location and geometry of the observed spiral structures. We were able to obtain an improved view of the spiral structures with the aid of light curves extracted in velocity bins matching the observed range of velocities of the spiral arms combined with a double default map tailored for reconstruction of asymmetric structures. Two-armed spiral structures are clearly seen in all eclipse maps. The arms are located at different distances from the disc centre. The "blue" arm is farther out in the disc (R = 0.55 ± 0.05 R L1 ) than the "red" arm (R = 0.30 ± 0.05 R L1 ). There is evidence that the velocity of the emitting gas along the spiral pattern is lower than the Keplerian velocity for the same disc radius. The discrepancy is smaller in the outer arm (measured velocities 10-15 per cent lower than Keplerian) and is more significant in the inner arm (observed velocities up to 40 per cent lower than Keplerian). We measured the opening angle of the spirals from the azimuthal intensity distribution of the eclipse maps to be φ = 25• ± 3 • . A comparison with similar measurements on data at different outburst stages reveals that the opening angle of the spiral arms in IP Peg decreases while the outbursting accretion disc cools and shrinks, in agreement with the expected evolution of a tidally driven spiral wave. The sub-Keplerian velocities along the spiral pattern and the clear correlation between the opening angle of the spirals and the outburst stage favors the interpretation of these asymmetric structures as tidally-induced spiral shocks.

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“…https://doi.org/10.1017/S007418090008311X is optically thick and fairly hot, in contrast with other parts of the disk at the same radial distance from the disk center. More recently, spectral eclipse mapping was conducted in the UV by Baptista et al (1995) using time-resolved spectra obtained with the Hubble Space Telescope. Such novel information contained in these disk spectra allows much more detailed probing of the accretion disk structure.…”

Section: · Mapping Accretion Disk Structure: Eclipse Mappingmentioning

confidence: 99%

Eclipse mapping and related techniques

Rutten

1996

Symp. - Int. Astron. Union

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Abstract. Eclipse mapping is a technique to deduce spatial structure on very small angular scales in eclipsing cataclysmic variable stars (CVs). By analysing the eclipse light curve, information is obtained on the brightness structure of the accretion disk and of the compact mass-accreting object in these systems. This information would otherwise be well beyond the resolving power of any optical telescope. Since the development of the eclipse mapping technique by K. Home, about one decade ago, it has now become an important tool in the study of CVs. Originally eclipse mapping was employed to construct brightness maps of accretion disks in broad spectral bands. Recently, maps of much higher spectral resolution have become available from which optical and UV spectra have been reconstructed in spatial detail across accretion disks. Such information is very important for our understanding of the physics of the accretion process.In this paper I will describe the eclipse mapping technique and review recent results. In conjunction, I will briefly highlight other techniques related to the mapping of surface structure in CVs. 1· IntroductionCataclysmic variable stars (hereafter abbreviated as CVs) are interacting binary systems which generally consist of a cool low-mass star and a more massive compact white dwarf. CVs are closely related to low-mass X-ray binaries in which the compact object is a neutron star or black hole; both groups of interacting binary stars have many observational and physical features in common.CVs exhibit brightness variations of very different amplitudes and on a wide range of time scales. These variations can be regular, semi-regular, irregular, or unique, and may affect a large wavelength range. The most

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Hubble Space Telescope and R-Band Eclipse Maps of the UX Ursae Majoris Accretion Disk

Cited by 67 publications

References 0 publications

Eclipse Mapping: Astrotomography of Accretion Discs

Eclipse Mapping: Astrotomography of Accretion Discs

Tracing the spiral arms in IP Pegasi

Eclipse mapping and related techniques

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