Physical Parameter Eclipse Mapping

Vrielmann, Sonja

doi:10.1007/3-540-45339-3_24

Cited by 7 publications

(13 citation statements)

References 34 publications

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“…Due to lack of any true constraint to weigh the two values we take the simple average of the distance (207 pc). In Vrielmann et al (2002b) we show a test case using an artificial non-axisymmetric disc and derive a distance 2.5 % larger than the assumed true distance. We have not included reddening in these calculation, however, as BSH point out, the reddening is nearly negligible and would change the distance by at most 5 pc.…”

Section: Ppem Distance Estimatesmentioning

confidence: 97%

“…An overview of applications of this method to various systems is given in Vrielmann (2001). Vrielmann, Stiening & Offutt (2002a) and Vrielmann, Hessman & Horne (2002b) show applications to V2051 Oph and HT Cas, respectively. We will give here only a very short description of the method, the interested reader is referred to the above articles for more details.…”

Section: The Ppem Analysismentioning

confidence: 99%

“…The dashed lines are parabolic fits to the data, they peak at 206 pc and 208 pc, respectively. regions of real disc will be typically much higher, leading to overestimated temperatures for disc regions cooler than about 6300 K. For a more detailed discussion on the applicability of the model see Vrielmann et al (2002b).…”

Section: The Spectral Model Used For Ppemmentioning

confidence: 99%

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UU Aqr from high to low state

Vrielmann

Baptista

2002

Astron. Nachr.

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In this paper we present Physical Parameter Eclipse Mapping (PPEM) of UBVRI eclipse light curves of UU Aqr from high to low states. We used a simple, pure hydrogen LTE model to derive the temperature and surface density distribution in the accretion disc. The reconstructed effective temperatures in the disc range between 9000 K and 15000 K in the inner part of the disc and below 7000 K in the outer parts. In the higher states it shows a more or less prominent bright spot with Teff between about 7000 K and 8000 K. The inner part of the disc (R < 0.3R) isL1 optically thick at all times, while the outer parts of the disc up to the disc edge (0.51 ± 0.04RL1 in the high state and 0.40 ± 0.03RL1 in the low state) deviate from a simple black body spectrum indicating that either the outer disc is optically thin or it shows a temperature inversion in the vertical direction. While during high state the disc is variable, it appears rather stable in low state. The variation during high state affects the size of the optically thick part of the disc, the white dwarf or boundary layer temperature and the uneclipsed component (originating in a disc chromosphere and/or cool disc wind), while the actual size of the disc remains constant. The difference between high and low state is expressed as a change in disc size that also affects the size of the optically thick part of the disc and the presence of the bright spot. Using the PPEM method we retrieve a distance for UU Aqr of 207±10 pc, compatible with previous estimates.

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Section: Ppem Distance Estimatesmentioning

confidence: 97%

Section: The Ppem Analysismentioning

confidence: 99%

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UU Aqr from high to low state

Vrielmann

Baptista

2002

Astron. Nachr.

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“…However, the slope of optical spectra is not well described by the standard disk theory. The eclipsing mapping also shows a deviation from the expected temperature distribution of the steady-state accretion disk [44,45]. With the orbital period decreasing with time, the mass transfer rate falls and the accretion disk contribution to the total flux is diminished, as evident from clearly seen absorption lines of the WD in many WZ Sge-type objects.…”

Section: Accretion Disk Structurementioning

confidence: 99%

Short Orbital Period Cataclysmic Variables

Zharikov¹

2017

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects - III — PoS(Golden2015)

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Cataclysmic Variables (CVs) are semi-detached binary systems consisting red/brown dwarfs filling its corresponding Roche lobe and loosing matter onto white dwarf (WD) companions. Classification of CVs is based on behavior of outbursts. In this report, we review properties of Short Orbital Period Cataclysmic Variables (77 min < P orb < 120 min). In mentioned orbital period range three subclasses of CVs were distinguished: SU UMa-, ER UMa-and WZ Sge-type objects. WZ Sge-type objects more probably includes also systems evolved past of the period minimum. The last are formed so-called bounce-backs or post-period minimum systems. Main characteristics of WDs, donor stars and accretion disks in the Short Orbital Period Cataclysmic Variables are discussed.

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“…Of promising prospects are the direct mapping of physical parameters in the accretion disc [54], the mapping of the brightness distribution along the accretion stream and accretion column in magnetic CVs [29], the 3-D mapping of flared discs and the surface of the secondary star [15,43], and the combination of eclipse mapping and Doppler tomography [12].…”

Section: Future Prospectsmentioning

confidence: 99%

Eclipse Mapping of Accretion Discs

Baptista

Astrotomography

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Abstract. The eclipse mapping method is an inversion technique that makes use of the information contained in eclipse light curves to probe the structure, the spectrum and the time evolution of accretion discs. In this review I present the basics of the method and discuss its different implementations. I summarize the most important results obtained to date and discuss how they have helped to improve our understanding of accretion physics, from testing the theoretical radial brightness temperature distribution and measuring mass accretion rates to showing the evolution of the structure of a dwarf novae disc through its outburst cycle, from isolating the spectrum of a disc wind to revealing the geometry of disc spiral shocks. I end with an outline of the future prospects.

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Physical Parameter Eclipse Mapping

Cited by 7 publications

References 34 publications

UU Aqr from high to low state

UU Aqr from high to low state

Short Orbital Period Cataclysmic Variables

Eclipse Mapping of Accretion Discs

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