Simulation of transitions between "pasta" phases in dense matter

Physical Review Letters

Volumn 94, Issue 3, 2005, Pages

  Watanabe, Gentaro ^a,b,c   Maruyama, Toshiki ^d   Sato, Katsuhiko ^b,e   Yasuoka, Kenji ^f   Ebisuzaki, Toshikazu ^c  

^a NORDITA   (Denmark)

^b UNIVERSITY OF TOKYO   (Japan)

^c INST OF PHYS AND CHEMICAL RESEARCH   (Japan)

^d JAPAN ATOMIC ENERGY AGENCY   (Japan)

^e UNIVERSITY OF TOKYO   (Japan)

^f KEIO UNIVERSITY   (Japan)

Author keywords

[No Author keywords available]

Indexed keywords

DENSE MATTER; NUCLEAR MATTERS; PASTA PHASES; TIME SCALES;

BOUNDARY CONDITIONS; COMPUTER SIMULATION; FUSION REACTIONS; HAMILTONIANS; MOLECULAR DYNAMICS; PROBLEM SOLVING; QUANTUM THEORY;

NUCLEAR PHYSICS;

EID: 18144383197     PISSN: 00319007     EISSN: 10797114     Source Type: Journal    
DOI: 10.1103/PhysRevLett.94.031101     Document Type: Article

References (25)

1. D. G. Ravenhall, C. J. Pethick, and J. R. Wilson, Phys. Rev. Lett. 50, 2066 (1983).
2. M. Hashimoto, H. Seki, and M. Yamada, Prog. Theor. Phys. 71, 320 (1984).
3. M. Lassaut et al., Astron. Astrophys. 183, L3 (1987).
4. G. Watanabe et al., Phys. Rev. C 69, 055805 (2004).
5. C. J. Pethick and D.G. Ravenhall, Annu. Rev. Nucl. Part. Sci. 45, 429 (1995).
6. K. Iida, G. Watanabe, and K. Sato, Prog. Theor. Phys. 106, 551 (2001).
7. G. Watanabe et al., Phys. Rev. C 66, 012801(R) (2002); 68, 035806 (2003).
8. G. Watanabe et al., Phys. Rev. C 66, 012801(R) (2002); 68, 035806 (2003).
9. J. Aichelin, Phys. Rep. 202, 233 (1991).
10. A. Burrows, S. Reddy, and T. A. Thompson, astro-ph/0404432 [Nucl. Phys. A (to be published)].
11. G. Watanabe, K. Iida, and K. Sato, Nucl. Phys. A687, 512 (2001); A726, 357(E) (2003).
12. G. Watanabe, K. Iida, and K. Sato, Nucl. Phys. A687, 512 (2001); A726, 357(E) (2003).
13. C.J. Horowitz, M. A. Pérez-García, and J. Piekarewicz, Phys. Rev. C 69, 045804 (2004).
14. G. Watanabe et al. (to be published).
15. 2) [12].
16. D.Z. Freedman, Phys. Rev. D 9, 1389 (1974).
17. K. Sato, Prog. Theor. Phys. 53, 595 (1975).
18. T. Maruyama et al., Phys. Rev. C 57, 655 (1998).
19. K. Niita, JAERI-CONF. 96-009, 22 (1996).
20. G. Watanabe and K. Iida, Phys. Rev. C 68, 045801 (2003).
21. 4 fm/c is observed during the compression, its dynamics is determined by the intrinsic physical properties of the system, not by the density change applied externally, whose time scale is much shorter than that of the actual stellar collapse.
22. th except for the state before the fusion and after the system is fully relaxed because the density in the nuclear matter region in the transient states is quite inhomogeneous.
23. K. Michielsen and H. De Raedt, Phys. Rep. 347, 461 (2001).
24. The value of χ is positive for the phases with spherical nuclei and spherical bubbles, and is zero for the other ideal pasta phases, i.e., the phases of rodlike nuclei, slablike nuclei, and cylindrical bubbles.
25. R HdA before χ decreases.