Hydrodynamic Simulation of Accretion Disks in Cataclysmic Variables

Hirose, Masakazu; Osaki, Yoji

doi:10.1007/978-94-009-1037-9_19

Cited by 64 publications

(91 citation statements)

References 2 publications

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“…At both outburst stages, the disc orientation is such that superhump maximum occurs when the mass-donor star is aligned with the bulge of the elliptical disc. This lends observational support for the tidal resonance instability model of superhumps [64,32,42].…”

Section: D Eclipse Mapping: Disc Opening Angle and Superhumpssupporting

confidence: 68%

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: D Eclipse Mapping: Disc Opening Angle and Superhumpssupporting

confidence: 68%

Eclipse Mapping: Astrotomography of Accretion Discs

Baptista¹

2016

Astronomy at High Angular Resolution

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“…This effect has a counterpart in the modelling of discs in Cataclysmic binaries. Here, in the lower companion mass range, an eccentric circumprimary disc has been seen (Whitehurst 1988;Hirose & Osaki 1990;Lubow 1991). This in turn is related to the excitation of a m = 2 spiral wave at the 3:1 inner eccentric Lindblad resonance, as described by Lubow (1991).…”

Section: Introductionmentioning

confidence: 90%

Orbital eccentricity growth through disc-companion tidal interaction

Papaloizou

Nelson

Masset

2001

A&A

247

296

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Abstract.We investigate the driving of orbital eccentricity of giant protoplanets and brown dwarfs through disccompanion tidal interactions by means of two dimensional numerical simulations. We consider disc models that are thought to be typical of protostellar discs during the planet forming epoch, with characteristic surface densities similar to standard minimum mass solar nebula models. We consider companions, ranging in mass between 1 and 30 Jupiter masses MJ, that are initially embedded within the discs on circular orbits about a central solar mass. We find that a transition in orbital behaviour occurs at a mass in the range 10-20 MJ. For low mass planetary companions, we find that the orbit remains essentially circular. However, for companion masses > ∼ 20 MJ, we find that non steady behaviour of the orbit occurs, characterised by a growth in eccentricity to values of 0.1 < ∼ e < ∼ 0.25. Analysis of the disc response to the presence of a perturbing companion indicates that for the higher masses, the inner parts of the disc that lie exterior to the companion orbit become eccentric through an instability driven by the coupling of an initially small disc eccentricity to the companion's tidal potential. This coupling leads to the excitation of an m = 2 spiral wave at the 1:3 outer eccentric Lindblad resonance, which transports angular momentum outwards, leading to a growth of the disc eccentricity. The interaction of the companion with this eccentric disc, and the driving produced by direct resonant wave excitation at the 1:3 resonance, can lead to the growth of orbital eccentricity, with the driving provided by the eccentric disc being the stronger. Eccentricity growth occurs when the tidally induced gap width is such that eccentricity damping caused by corotating Lindblad resonances is inoperative. These simulations indicate that for standard disc models, gaps become wide enough for the 1:3 resonance to dominate, such that the transition from circular orbits can occur, only for masses in the brown dwarf range. However, the transition mass might be reduced into the range for extrasolar planets if the disc viscosity is significantly lower enabling wider gaps to occur for these masses. Another possibility is that an eccentric disc is produced by an alternative mechanism, such as viscous overstability resulting in a slowly precessing non axisymmetric mass distribution. A large eccentricity in a planet orbit contained within an inner cavity might then be produced.

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“…An extensive study of SU UMa superhumps showed that the evolution of their periods is often composed of three distinct stages (see Kato et al 2009, and their later papers). These complex period changes can be explained by variation of the accretion disc radius during a superoutburst (Hirose & Osaki 1990), which is possibly accompanied by variable gas pressure effects in the disc (Osaki & Kato 2013). The evolution of the superhump period in SSS J122222 has been investigated by Kato et al (2013).…”

Section: Superoutburst Superhumpsmentioning

confidence: 99%

The remarkable outburst of the highly-evolved post period-minimum dwarf nova SSS J122221.7−311525

Neustroev

Marsh

Zharikov

et al. 2017

Mon. Not. R. Astron. Soc.

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We report extensive 3-yr multiwavelength observations of the WZ Sge-type dwarf nova SSS J122221.7−311525 during its unusual double superoutburst, the following decline and in quiescence. The second segment of the superoutburst had a long duration of 33 d and a very gentle decline with a rate of 0.02 mag d −1 , and it displayed an extended post-outburst decline lasting at least 500 d. Simultaneously with the start of the rapid fading from the superoutburst plateau, the system showed the appearance of a strong near-infrared excess resulting in very red colours, which reached extreme values (B − I ≃ 1.4) about 20 d later. The colours then became bluer again, but it took at least 250 d to acquire a stable level. Superhumps were clearly visible in the light curve from our very first time-resolved observations until at least 420 d after the rapid fading from the superoutburst. The spectroscopic and photometric data revealed an orbital period of 109.80 min and a fractional superhump period excess 0.8 per cent, indicating a very low mass ratio q 0.045. With such a small mass ratio the donor mass should be below the hydrogen-burning minimum mass limit. The observed infrared flux in quiescence is indeed much lower than is expected from a cataclysmic variable with a nearmain-sequence donor star. This strongly suggests a brown-dwarf-like nature for the donor and that SSS J122221.7−311525 has already evolved away from the period minimum towards longer periods, with the donor now extremely dim.

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Hydrodynamic Simulation of Accretion Disks in Cataclysmic Variables

Cited by 64 publications

References 2 publications

Eclipse Mapping: Astrotomography of Accretion Discs

Eclipse Mapping: Astrotomography of Accretion Discs

Orbital eccentricity growth through disc-companion tidal interaction

The remarkable outburst of the highly-evolved post period-minimum dwarf nova SSS J122221.7−311525

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