J.E. Pringle, Accretion discs in astrophysics, Ann. Rev. Astron. Astrophys., 19 (1981) 137--162 15 Home/Search Document Not in Database Summary Related Articles Check |
This paper is cited in the following contexts:
The viscous gas ring as an astrophysical test problem for a.. - Speith, Riffert (1999) (Correct)
.... If rotational symmetry Preprint submitted to Elsevier Preprint 21 April 1999 is assumed an evolution equation for the density can be derived, and for a constant kinematic viscosity the solution of an initial value problem is obtained explicitly in terms of Bessel functions and exponentials ( 7] [10], 2] The purpose of this paper is to use the above analytic solution as a test model for a SPH code that is designed to simulate two dimensional viscous gas flows dominated by gravitational forces. The analytic solution is briefly discussed in Section 2 for the case that the viscosity varies ....
....i s p R Sigma j # : 7) An analytic solution can be obtained on the space domain [0; 1) with initial data Sigma(R; 0) Sigma 0 (R) provided the kinematic viscosity has the form s (R) 0 R fl ; 8) where 0 and fl are constants. According to the standard thin disk theory (Pringle [10], Frank et al. 2] the disk is likely to be in a state of fully excited turbulence and s is interpreted as a turbulent viscosity. Therefore, s will in general depend on the radius and the particlular form (8) has been chosen in order to keep the problem analytically solvable. 3 For fl = 0 the ....
[Article contains additional citation context not shown here]
J.E. Pringle, Accretion discs in astrophysics, Ann. Rev. Astron. Astrophys., 19 (1981) 137--162 15
The viscous gas ring as an astrophysical test problem for a.. - Speith, Riffert (1999) (Correct)
....point mass under the in#uence of gravity and viscous torques. If rotational symmetry is assumed an evolution equation for the density can be derived, and for a constant kinematic viscosity the solution of an initial value problem is obtained explicitly in terms of Bessel functions and exponentials [7,10,2]. The purpose of this paper is to use the above analytic solution as a test model for a SPH code that is designed to simulate two dimensional viscous gas #ows dominated by gravitational forces. The analytic solution is brie#y discussed in Section 2 for the case that the viscosity varies as a ....
....3 R R # # R R (# s # R#) # : 7) An analytic solution can be obtained on the space domain [0; #) with initial data #(R; 0) # 0 (R) provided the kinematic viscosity has the form # s (R) # 0 R # ; 8) where # 0 and # are constants. According to the standard thin disk theory [10,2] the disk is likely to be in a state of fully excited turbulence and # s is interpreted as a turbulent viscosity. Therefore, # s will in general depend on the radius and the particlular form (8) has been chosen in order to keep the problem analytically solvable. For # = 0 the solution of (7) is ....
[Article contains additional citation context not shown here]
J.E. Pringle, Accretion discs in astrophysics, Ann. Rev. Astron. Astrophys. 19 (1981) 137--162.
The viscous gas ring as an astrophysical test problem for a.. - Speith, Riffert (1999) (Correct)
....mass under the in uence of gravity and viscous torques. If rotational symmetry is assumed an evolution equation for the density can be derived, and for a constant kinematic viscosity the solution of an initial value problem is obtained explicitly in terms of Bessel functions and exponentials ( 7] [10], 2] The purpose of this paper is to use the above analytic solution as a test model for a SPH code that is designed to simulate two dimensional viscous gas ows dominated by gravitational forces. The analytic solution is brie y discussed in Section 2 for the case that the viscosity varies as a ....
.... p R R s p R # : 7) An analytic solution can be obtained on the space domain [0; 1) with initial data (R; 0) 0 (R) provided the kinematic viscosity has the form s (R) 0 R ; 8) where 0 and are constants. According to the standard thin disk theory (Pringle [10], Frank et al. 2] the disk is likely to be in a state of fully excited turbulence and s is interpreted as a turbulent viscosity. Therefore, s will in general depend on the radius and the particlular form (8) has been chosen in order to keep the problem analytically solvable. For = 0 the ....
[Article contains additional citation context not shown here]
J.E. Pringle, Accretion discs in astrophysics, Ann. Rev. Astron. Astrophys., 19 (1981) 137-162
Numerical Fluid Dynamics in Astrophysics with Smoothed.. - Speith, Riffert, Ruder (Correct)
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Pringle, J.E.: Accretion discs in astrophysics. Ann. Rev. Astron. Astrophys. 19 (1981) 137--162
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