scholarly journals The Monte Carlo photoionization and moving-mesh radiation hydrodynamics code CMacIonize

2018 ◽  
Vol 23 ◽  
pp. 40-59 ◽  
Author(s):  
B. Vandenbroucke ◽  
K. Wood
Keyword(s):  
Monte Carlo ◽  
Moving Mesh ◽  
Radiation Hydrodynamics

scholarly journals AREPO-MCRT: Monte Carlo Radiation Hydrodynamics on a Moving Mesh

2020 ◽  
Vol 905 (1) ◽  
pp. 27
Author(s):  
Aaron Smith ◽  
Rahul Kannan ◽  
Benny T.-H. Tsang ◽  
Mark Vogelsberger ◽  
Rüdiger Pakmor
Keyword(s):  
Monte Carlo ◽  
Moving Mesh ◽  
Radiation Hydrodynamics

scholarly journals arepo-rt: radiation hydrodynamics on a moving mesh

2019 ◽  
Vol 485 (1) ◽  
pp. 117-149 ◽  
Author(s):  
Rahul Kannan ◽  
Mark Vogelsberger ◽  
Federico Marinacci ◽  
Ryan McKinnon ◽  
Rüdiger Pakmor ◽  
...  
Keyword(s):  
Moving Mesh ◽  
Radiation Hydrodynamics

scholarly journals Monte Carlo radiation hydrodynamics: methods, tests and application to Type Ia supernova ejecta

2012 ◽  
Vol 425 (2) ◽  
pp. 1430-1444 ◽  
Author(s):  
U. M. Noebauer ◽  
S. A. Sim ◽  
M. Kromer ◽  
F. K. Röpke ◽  
W. Hillebrandt
Keyword(s):  
Monte Carlo ◽  
Radiation Hydrodynamics ◽  
Type Ia Supernova ◽  
Type Ia

Outbursts of comet Schwassmann-Wachmann 1, and the cloud of interplanetary boulders

1974 ◽  
Vol 22 ◽  
pp. 307 ◽  
Author(s):  
Zdenek Sekanina
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Method ◽  
Interplanetary Space ◽  
Porous Matrix ◽  
Maximum Diameter ◽  
Expansion Velocity ◽  
Solid Constituent ◽  
Meteoric Material ◽  
Periodic Comet

AbstractIt is suggested that the outbursts of Periodic Comet Schwassmann-Wachmann 1 are triggered by impacts of interplanetary boulders on the surface of the comet’s nucleus. The existence of a cloud of such boulders in interplanetary space was predicted by Harwit (1967). We have used the hypothesis to calculate the characteristics of the outbursts – such as their mean rate, optically important dimensions of ejected debris, expansion velocity of the ejecta, maximum diameter of the expanding cloud before it fades out, and the magnitude of the accompanying orbital impulse – and found them reasonably consistent with observations, if the solid constituent of the comet is assumed in the form of a porous matrix of lowstrength meteoric material. A Monte Carlo method was applied to simulate the distributions of impacts, their directions and impact velocities.

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