Lambda polarization in the reaction K−p → Λ + anything at 14.3 GeV/c

Abramowicz, H.; Barloutaud, R.; Borg, A.; Spiro, M.; Paler, K.; Shah, T.; Tovey, S. N.; Chaurand, B.; Drévillon, B.; Gago, J.; Salmeron, R.

doi:10.1016/0550-3213(76)90263-7

Cited by 20 publications

(9 citation statements)

References 13 publications

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“…The basic equations describing conservations of mass and momentum in the vertically integrated disk remain same as of earlier works which assumed γ and then β to be constant throughout (e.g. Abramowicz et al 1988;Chakrabarti 1996;Rajesh & Mukhopadhyay 2010b). Abramowicz et al (1988) also showed that the geometrically slimmer flow is stable for β > 0.4.…”

Section: Model Equationsmentioning

confidence: 99%

“…Abramowicz et al 1988;Chakrabarti 1996;Rajesh & Mukhopadhyay 2010b). Abramowicz et al (1988) also showed that the geometrically slimmer flow is stable for β > 0.4. For simplicity, following e.g.…”

Section: Model Equationsmentioning

confidence: 99%

“…Very recently, Chattopadhyay & Ryu (2009) showed that composition of the fluid plays an important role to determine the value of γ and then solutions of inviscid spherical flows around black holes. This would have impact on a hot accre-tion disk as well which was shown to exhibit significant nuclear burning, producing the variation of compositions in the disk (Chakrabarti & Mukhopadhyay 1999, Mukhopadhyay & Chakrabarti 2000. Earlier, while Chen & Taam (1993) discussed structure and stability of the transonic optically thick accretion disks without restricting the gas and radiation content therein, did not show the actual variation of the gas/radiation content as a function of radial coordinate and then its impact to the solutions.…”

Section: Introductionmentioning

confidence: 99%

“…We essentially concentrate on the region of the flows which is expected to be sub-Keplerian in nature. Therefore, following previous work (Muchotrzeb & Paczynski 1982;Abramowicz et al 1988;Chakrabarti 1996;Mukhopadhyay & Ghosh 2003;Rajesh & Mukhopadhyay 2010a) we model the flow from the Keplerian to sub-Keplerian transition radius (x t ) to the black hole event horizon (x + ). We plan to concentrate, in particular, the class of flows which is not geometrically very thick, yet sub-Keplerian in nature including a nonzero component of advection and gradient of pressure in general.…”

Section: Introductionmentioning

confidence: 99%

“…Hence, the underlying equations can be integrated/averaged vertically without losing important physics, in obtaining the solutions. Therefore, following previous work (Muchotrzeb & Paczynski 1982;Abramowicz et al 1988;Chakrabarti 1996;Mukhopadhyay & Ghosh 2003;Rajesh & Mukhopadhyay 2010a, 2010b, we consider vertically integrated infall consisting of gas and radiation. While the flow around x t might be non-relativistic with a high γ (depending on the size of the disk), as it advances towards x + , γ must be varying.…”

Section: Introductionmentioning

confidence: 99%

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Variation of the gas and radiation content in the sub-Keplerian accretion disk around black holes and its impact to the solutions

Mukhopadhyay

Dutta

2012

New Astronomy

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We investigate the variation of the gas and the radiation pressure in accretion disks during the infall of matter to the black hole and its effect to the flow. While the flow far away from the black hole might be non-relativistic, in the vicinity of the black hole it is expected to be relativistic behaving more like radiation. Therefore, the ratio of gas pressure to total pressure (β) and the underlying polytropic index (γ) should not be constant throughout the flow. We obtain that accretion flows exhibit significant variation of β and then γ, which affects solutions described in the standard literature based on constant β. Certain solutions for a particular set of initial parameters with a constant β do not exist when the variation of β is incorporated appropriately. We model the viscous sub-Keplerian accretion disk with a nonzero component of advection and pressure gradient around black holes by preserving the conservations of mass, momentum, energy, supplemented by the evolution of β. By solving the set of five coupled differential equations, we obtain the thermo-hydrodynamical properties of the flow. We show that during infall, β of the flow could vary upto ∼ 300%, while γ upto ∼ 20%. This might have a significant impact to the disk solutions in explaining observed data, e.g. super-luminal jets from disks, luminosity, and then extracting fundamental properties from them. Hence any conclusion based on constant γ and β should be taken with caution and corrected.

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Section: Model Equationsmentioning

confidence: 99%

Section: Model Equationsmentioning

confidence: 99%