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SelfSimilar Shocked Accretion of Collisional Gas with Radiative Cooling
, 1999
"... We describe similarity solutions that characterize the collapse of collisional gas onto scalefree perturbations in an Einsteinde Sitter universe. We consider the effects of radiative cooling and derive selfsimilar solutions under the assumption that the ..."
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We describe similarity solutions that characterize the collapse of collisional gas onto scalefree perturbations in an Einsteinde Sitter universe. We consider the effects of radiative cooling and derive selfsimilar solutions under the assumption that the
Spherical Isothermal SelfSimilar Shock Flows
, 2005
"... We explore selfsimilar dynamical processes in a spherical isothermal selfgravitational fluid with an emphasis on shocks and outline astrophysical applications of such shock solutions. The previous similarity shock solutions of Tsai & Hsu and of Shu et al. may be classified into two types: Clas ..."
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We explore selfsimilar dynamical processes in a spherical isothermal selfgravitational fluid with an emphasis on shocks and outline astrophysical applications of such shock solutions. The previous similarity shock solutions of Tsai & Hsu and of Shu et al. may be classified into two types
SelfSimilar Shocks in Polytropic Gas Flows around StarForming Regions
, 2006
"... Accepted. Received; in original form Selfsimilar shock solutions in spherically symmetric polytropic gas flows are constructed and analyzed in contexts of protostar formation processes. Among other possible solutions, we model a similarity shock across the sonic critical curve with an inner freef ..."
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Cited by 1 (0 self)
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fall core collapse and a simultaneous outer expansion of the extended envelope; the separation or stagnation surface between these two flow zones travels outwards in a selfsimilar manner at a variable speed. One readily obtains accretion shock solutions. Semicomplete selfsimilar solutions across
SelfSimilar Accretion Flows with Convection
, 1999
"... We consider heightintegrated equations of an advectiondominated accretion flow (ADAF), assuming that there is no mass outflow. We include convection through a mixing length formalism. We seek selfsimilar solutions in which the angular velocity and sound speed scale as R −1/2, where R is the radiu ..."
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We consider heightintegrated equations of an advectiondominated accretion flow (ADAF), assuming that there is no mass outflow. We include convection through a mixing length formalism. We seek selfsimilar solutions in which the angular velocity and sound speed scale as R −1/2, where R
Stability of SelfSimilar Spherical Accretion
, 2005
"... Abstract. Spherical accretion flows are simple enough for analytical study, by solution of the corresponding fluid dynamic equations. The solutions of stationary spherical flow are due to Bondi. The questions of the choice of a physical solution and of stability have been widely discussed. The answe ..."
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. The answer to these questions is very dependent on the problem of boundary conditions, which vary according to whether the accretor is a compact object or a black hole. We introduce a particular, simple form of stationary spherical flow, namely, selfsimilar Bondi flow, as a case with physical interest
A General Class of Selfsimilar Selfgravitating Fluids
, 1994
"... I present a general classification of selfsimilar solutions to the equations of gravitational hydrodynamics that contain many previous results as special cases. For cold flows with spherical symmetry, the solution space can be classified into several regions of behavior similar to the Bondi solutio ..."
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in the presence of finite pressure. These solutions serve as analytic models for problems such as spherical accretion for star formation, infall or outflow of gas into galaxies, Lyman alpha cloud dynamics, etc. Most previous selfsimilar results are obtained as special cases. The critical values for a
Selfsimilar evolution of . . .
, 2008
"... Using an improved version of the previously introduced CRASH (Cosmic Ray Acceleration SHock) code, we have calculated the time evolution of cosmicray (CR) modified quasiparallel plane shocks for Bohmlike diffusion, including selfconsistent models of Alfvén wave drift and dissipation, along with ..."
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the evolution of the CR partial pressure expressed in terms of a momentum similarity variable is selfsimilar. The shock precursor, which scales as the diffusion length of the highest energy CRs, subsequently broadens approximately linearly with time, independent of diffusion model, so long as CRs continue
Selfsimilar solutions for weak shock reflection
 SIAM J. Appl. Math
, 2002
"... Abstract. We present numerical solutions of a twodimensional Riemann problem for the unsteady transonic small disturbance equations that provides an asymptotic description of the Mach reflection of weak shock waves. We develop a new numerical scheme to solve the equations in selfsimilar coordinates ..."
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Cited by 27 (9 self)
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Abstract. We present numerical solutions of a twodimensional Riemann problem for the unsteady transonic small disturbance equations that provides an asymptotic description of the Mach reflection of weak shock waves. We develop a new numerical scheme to solve the equations in selfsimilar
AdvectionDominated Accretion: A SelfSimilar Solution,” Astrophys
 J. p
, 1994
"... We consider axisymmetric viscous accretion flows where a fraction f of the viscously dissipated energy is stored in the accreting gas as entropy and a fraction 1 − f is radiated. Assuming αviscosity we obtain a twoparameter family of selfsimilar solutions. Very few such exact selfconsistent solu ..."
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Cited by 26 (0 self)
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We consider axisymmetric viscous accretion flows where a fraction f of the viscously dissipated energy is stored in the accreting gas as entropy and a fraction 1 − f is radiated. Assuming αviscosity we obtain a twoparameter family of selfsimilar solutions. Very few such exact self
SelfSimilar Shocks and Winds in Galaxy Clusters
, 801
"... A theoretical model framework of spherical symmetry is presented for a composite astrophysical system of two polytropic fluids coupled together by gravity to explore largescale shocks and flow dynamics in clusters of galaxies or in globular clusters. The existence of such largescale shocks in clus ..."
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Cited by 2 (2 self)
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in clusters of galaxies as inferred by highresolution Xray and radio imaging observations implies largescale systematic flows that are beyond usual static models for clusters of galaxies. Here, we explore selfsimilar twofluid flow solutions with shocks for a hot polytropic gas flow in a cluster
Results 1  10
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1,244