Solid/liquid/gaseous phase transitions in plasma crystals

1996 ◽  
Vol 14 (2) ◽  
pp. 501-505 ◽  
Author(s):  
Hubertus M. Thomas ◽  
Gregor E. Morfill
1990 ◽  
Vol 24-26 (1) ◽  
pp. 283-342 ◽  
Author(s):  
R. Kofman ◽  
P. Cheyssac ◽  
R. Garrigos

2019 ◽  
Vol 12 (6) ◽  
pp. 770-788 ◽  
Author(s):  
Tilman Barz ◽  
Johannn Emhofer ◽  
Klemens Marx ◽  
Gabriel Zsembinszki ◽  
Luisa F. Cabeza

2003 ◽  
Vol 83 (18) ◽  
pp. 3704-3706 ◽  
Author(s):  
V. A. Gnatyuk ◽  
T. Aoki ◽  
O. S. Gorodnychenko ◽  
Y. Hatanaka

1998 ◽  
Vol 09 (08) ◽  
pp. 1405-1415 ◽  
Author(s):  
G. de Fabritiis ◽  
A. Mancini ◽  
D. Mansutti ◽  
S. Succi

A generalization of mesoscopic Lattice-Boltzmann models aimed at describing flows with solid/liquid phase transitions is presented. It exhibits lower computational costs with respect to the numerical schemes resulting from differential models. Moreover it is suitable to describe chaotic motions in the mushy zone.


2006 ◽  
Vol 20 (22) ◽  
pp. 3113-3198 ◽  
Author(s):  
P. H. CHAVANIS

We discuss the nature of phase transitions in self-gravitating systems. We show the connection between the binary star model of Padmanabhan, the thermodynamics of stellar systems and the thermodynamics of self-gravitating fermions. We stress the inequivalence of statistical ensembles for systems with long-range interactions, like gravity. In particular, we contrast the microcanonical evolution of stellar systems from the canonical evolution of self-gravitating Brownian particles. At low energies, self-gravitating Hamiltonian systems experience a gravothermal catastrophe in the microcanonical ensemble. At low temperatures, self-gravitating Brownian systems experience an isothermal collapse in the canonical ensemble. For classical particles, the gravothermal catastrophe leads to a binary star surrounded by a hot halo while the isothermal collapse leads to a Dirac peak containing all the mass. For self-gravitating fermions, the collapse stops when quantum degeneracy comes into play through the Pauli exclusion principle. The end-product of the collapse is a fermion ball, resembling a cold white dwarf star, surrounded by a halo. We can thus describe a phase transition from a gaseous phase to a condensed phase. At high energies or high temperatures, the condensate can experience an explosion, reverse to the collapse, and return to the gaseous phase. Due to the existence of long-lived metastable states, the points of collapse and explosion differ. This leads to a notion of hysteretic cycle in microcanonical and canonical ensembles.


2012 ◽  
Vol 32 (6) ◽  
pp. 1997-2025 ◽  
Author(s):  
Sylvie Benzoni-Gavage ◽  
◽  
Laurent Chupin ◽  
Didier Jamet ◽  
Julien Vovelle ◽  
...  

2007 ◽  
Vol 3 (12) ◽  
pp. 890-894 ◽  
Author(s):  
Hans Riegler ◽  
Ralf Köhler

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