Mass Transfer by Tidally Induced Spiral Shocks in An Accretion Disc

Matsuda, Takuya; Sekino, Nobuhiro; Shima, Eiji; Sawada, Keisuke; Spruit, H. C.

doi:10.1007/978-94-009-1037-9_35

Cited by 32 publications

(25 citation statements)

References 22 publications

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“…Chakrabarti (1992), Bisikalo et al (1999), spiral patterns do not appear if a polytropic index (appearing in the perfect gas state equation) γ > 1.16 is adopted. According to some others, such as Sawada et al (1987), Spruit et al (1987), Kaisig (1989), Matsuda et al (1990Matsuda et al ( , 1992, Ichikawa & Osaki (1992, 1994, Sawada & Matsuda (1992), Savonije et al (1994), Yukawa et al (1997), Makita et al (2000), spiral patterns and radial shocks always exist whatever the γ is and the initial kinematic conditions are. Tidal effects should be responsible for spirals and spiral shock development in the disc bulk, starting from the outer disc edge.…”

Section: Introductionmentioning

confidence: 98%

Low compressibility accretion disc formation in close binaries: the role of physical viscosity

Lanzafame

Belvedère

Molteni

2006

A&A

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Aims. Physical viscosity naturally hampers gas dynamics (rarefaction or compression). Such a role should support accretion disc development inside the primary gravitation potential well in a close binary system, even for low compressibility modelling. Therefore, from the astrophysical point of view, highly viscous accretion discs could exist even in the low compressibility regime showing strong thermal differences to high compressibility ones Methods. We performed simulations of stationary Smooth Particle Hydrodynamics (SPH) low compressibility accretion disc models for the same close binary system. Artificial viscosity operates in all models. The absence of physical viscosity and a supersonic high mass transfer characterize the first model. Physical viscosity and the same supersonic high mass transfer characterize the second model, whilst physical viscosity and a subsonic low mass transfer characterize the third model. The same binary system parameters, such as stellar masses and their separation, have been adopted, as well as the same polytropic index γ = 5/3. Thus we investigated the role of physical viscosity in mass and angular momentum transport in the two viscid models and compare them to the inviscid model. An initial value of the parameter α = 1 has been considered for the physically viscous models, according to the well-known Shakura and Sunjaev formulation, but simulations were carried out also for α = 0.1 and α = 0.5 in the case of a supersonic mass transfer. Physical viscosity is represented by the viscous force contribution expressed by the divergence of the symmetric viscous stress tensor in the Navier-Stokes equation, while the viscous energy contribution is given by a symmetric combination of the symmetric shear tensor times the particle velocity. Results. The results show that physical viscosity supports and favours accretion disc formation despite the very low compressibility assumed. On the contrary, in the inviscid case no evident disc structure appears. In all models neither shock fronts nor extended clear spirals in the radial flow develop.

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Section: Introductionmentioning

confidence: 98%

Low compressibility accretion disc formation in close binaries: the role of physical viscosity

Lanzafame

Belvedère

Molteni

2006

A&A

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“…The problem of the development of spirals in the radial flow of spiral shocks in physically inviscid accretion discs has been studied by various authors: Sawada et al (1987), Spruit et al (1987), Kaisig (1989), Matsuda et al (1990Matsuda et al ( , 1992, Ichikawa & Osaki (1992, Sawada & Matsuda (1992), Savonije et al (1994), Lanzafame & Belvedere (1997, 1998, Murray (1996), Yukawa et al (1997), Bisikalo et al (1998aBisikalo et al ( ,b, 1999, Blondin (2000), Lanzafame et al (2000, Makita et al (2000), , Truss et al (2001), Belvedere & Lanzafame (2002). Common opinion supported in many of such papers is that outer edge perturbations are responsible for spiral pattern structure generation.…”

Section: Introductionmentioning

confidence: 99%

“…Bisikalo et al (1999), Chakrabarty (1992), spiral patterns do not appear if γ > 1.16 is adopted. Instead, according to some others, such as Matsuda et al (1990Matsuda et al ( , 1992, Yukawa et al (1997), Makita et al (2000), spiral patterns and radial shocks always exist whatever γ is and whatever the initial kinematic conditions are. Recently we wrote some papers (Lanzafame et al 2000Belvedere & Lanzafame 2002) concluding, via 2D and 3D SPH computer simulations, that initial conditions as far as angular momentum and energy are concerned are crucial in spiral formation.…”

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confidence: 99%

Spiral and shock front development in accretion discs in close binaries: Physically viscous and non-viscous SPH modelling

Lanzafame

2003

A&A

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Abstract.A comparison between an accretion disc model, whose transport mechanisms are driven only by artificial viscosity, and a physically viscous accretion disc model for the same close binary system is performed here by adopting the same parameters and boundary conditions. These assumptions mean that artificial viscosity, included in both models, shares, together with physical viscosity, mass and angular momentum transport in the second disc model. The Smooth Particle Hydrodynamics (SPH) Lagrangian scheme has been adopted in both models and α ss = 1 has been considered as for the viscous model according to the well-known Shakura and Sunjaev formulation. Physical viscosity is represented by the viscous force contribution as a divergence of the symmetric viscous stress tensor in the Navier-Stokes equation, whilst the viscous energy contribution is given by a symmetric combination of the symmetric shear tensor times to the particle velocity. Adopting a supersonic particle inflowing at the inner lagrangian point L1, clear spiral strong shocks in the radial flux develop from the inviscid 3D model. Extended spirals and shock fronts are even more evident in the viscous accretion disc model, which is larger than the non-viscous one in the XY orbital plane. Characteristics of the two disc structures as well as observational consequences are discussed.

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“…At present there are two approaches to this problem: according to the first one, angular momentum is transported due to the presence of turbulent or magnetic viscosity in the disk (Shakura & Sunyaev 1973). On the other hand, hydrodynamical numerical calculations have shown that tidal forces of the secondary induce spiral shock waves in the accretion disk, which may provide an efficient transfer mechanism (Sawada et al 1986;Matsuda et al 1990). Self-similar solutions having spiral shocks, was constructed in a semi-analytic manner in two dimensions by Spruit (1987, see also Chakrabarti 1990.…”

Section: Introductionmentioning

confidence: 99%

IP Pegasi: Investigation of the accretion disk structure

Neustroev¹,

Borisov²,

Barwig³

et al. 2002

A&A

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Abstract. We present the results of spectral investigations of the cataclysmic variable IP Peg in quiescence. Optical spectra obtained on the 6-m telescope at the Special Astrophysical Observatory (Russia), and on the 3.5-m telescope at the GermanSpanish Astronomical Center (Calar Alto, Spain), have been analysed by means of Doppler tomography and Phase Modelling Technique. From this analysis we conclude that the quiescent accretion disk of IP Peg has a complex structure. There are also explicit indications of spiral shocks. The Doppler maps and the variations of the peak separation of the emission lines confirm this interpretation. We have detected that all the emission lines show a rather considerable asymmetry of their wings varying with time. The wing asymmetry shows quasi-periodic modulations with a period much shorter than the orbital one. This indicates the presence of an emission source in the binary rotating asynchronously with the binary system. We also have found that the brightness of the bright spot changes considerably during one orbital period. The spot becomes brightest at an inferior conjunction, whereas it is almost invisible when it is located on the distant half of the accretion disk. Probably, this phenomenon is due to an anisotropic radiation of the bright spot and an eclipse of the bright spot by the outer edge of the accretion disk.

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Mass Transfer by Tidally Induced Spiral Shocks in An Accretion Disc

Cited by 32 publications

References 22 publications

Low compressibility accretion disc formation in close binaries: the role of physical viscosity

Low compressibility accretion disc formation in close binaries: the role of physical viscosity

Spiral and shock front development in accretion discs in close binaries: Physically viscous and non-viscous SPH modelling

IP Pegasi: Investigation of the accretion disk structure

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