Phase diagram of nuclear "pasta" and its uncertainties in supernova cores

Physical Review C - Nuclear Physics

Volumn 77, Issue 3, 2008, Pages

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

^a UNIVERSITY OF TOKYO   (Japan)

^b INST OF PHYS AND CHEMICAL RESEARCH   (Japan)

^c UNIVERSITY OF TRENTO   (Italy)

^d NORDITA   (Denmark)

^e UNIVERSITY OF TOKYO   (Japan)

^f KEIO UNIVERSITY   (Japan)

Author keywords

[No Author keywords available]

Indexed keywords

EID: 41549087816     PISSN: 05562813     EISSN: 1089490X     Source Type: Journal    
DOI: 10.1103/PhysRevC.77.035806     Document Type: Article

References (54)

1. D. G. Ravenhall, C. J. Pethick, and J. R. Wilson, Phys. Rev. Lett. PRLTAO 0031-9007 10.1103/PhysRevLett.50.2066 50, 2066 (1983).
2. M. Hashimoto, H. Seki, and M. Yamada, Prog. Theor. Phys. PTPKAV 0033-068X 10.1143/PTP.71.320 71, 320 (1984).
3. B. K. Jennings and A. Schwenk, nucl-th/0512013.
4. H. A. Bethe, Rev. Mod. Phys. RMPHAT 0034-6861 10.1103/RevModPhys.62.801 62, 801 (1990).
5. A. Burrows, S. Reddy, and T. A. Thompson, Nucl. Phys. NUPABL 0375-9474 10.1016/j.nuclphysa.2004.06.012 A777, 356 (2006).
6. H.-T. Janka, K. Langanke, A. Merek, Martínez-Pinedo, and B. Müller, Phys. Rep. PRPLCM 0370-1573 10.1016/j.physrep.2007.02.002 442, 38 (2007).
7. C. J. Horowitz, M. A. Pérez-García, J. Carriere, D. K. Berry, and J. Piekarewicz, Phys. Rev. C PRVCAN 0556-2813 10.1103/PhysRevC.70. 065806 70, 065806 (2004).
8. H. Sonoda, G. Watanabe, K. Sato, T. Takiwaki, K. Yasuoka, and T. Ebisuzaki, Phys. Rev. C PRVCAN 0556-2813 10.1103/PhysRevC.75.042801 75, 042801(R) (2007).
9. C. P. Lorenz, D. G. Ravenhall, and C. J. Pethick, Phys. Rev. Lett. PRLTAO 0031-9007 10.1103/PhysRevLett.70.379 70, 379 (1993).
10. C. J. Pethick and V. Thorsson, Phys. Rev. Lett. PRLTAO 0031-9007 10.1103/PhysRevLett.72.1964 72, 1964 (1994).
11. A. D. Kaminker, C. J. Pethick, A. Y. Potekhin, V. Thorsson, and D. G. Yakovlev, Astron. Astrophys. 343, 1009 (1999).
12. M. E. Gusakov, D. G. Yakovlev, P. Haensel, and O. Y. Gnedin, Astron. Astrophys. AAEJAF 0004-6361 10.1051/0004-6361:20040288 421, 1143 (2004).
13. R. D. Williams and S. E. Koonin, Nucl. Phys. NUPABL 0375-9474 10.1016/0375-9474(85)90191-5 A435, 844 (1985).
14. M. Lassaut, H. Flocard, P. Bonche, P. H. Heenen, and E. Suraud, Astron. Astrophys. 183, L3 (1987).
15. K. Oyamatsu, Nucl. Phys. NUPABL 0375-9474 10.1016/0375-9474(93)90020-X A561, 431 (1993).
16. G. Watanabe, K. Iida, and K. Sato, Nucl. Phys. NUPABL 0375-9474 10.1016/S0375-9474(00)00197-4 A676, 455 (2000).
17. G. Watanabe, K. Iida, and K. Sato, Nucl. Phys. NUPABL 0375-9474 10.1016/S0375-9474(00)00585-6 A687, 512 (2001).
18. G. Watanabe, K. Iida, and K. Sato, Nucl. Phys. NUPABL 0375-9474 10.1016/S0375-9474(03)01601-4 A726, 357 (2003).
19. T. Maruyama, T. Tatsumi, D. N. Voskresensky, T. Tanigawa, and S. Chiba, Phys. Rev. C PRVCAN 0556-2813 10.1103/PhysRevC.72.015802 72, 015802 (2005).
20. K. S. Cheng, C. C. Yao, and Z. G. Dai, Phys. Rev. C PRVCAN 0556-2813 10.1103/PhysRevC.55.2092 55, 2092 (1997).
21. F. Douchin and P. Haensel, Phys. Lett. PYLBAJ 0370-2693 10.1016/S0370-2693(00)00672-9 B485, 107 (2000).
22. G. Watanabe, K. Sato, K. Yasuoka, and T. Ebisuzaki, Phys. Rev. C PRVCAN 0556-2813 10.1103/PhysRevC.66.012801 66, 012801(R) (2002).
23. G. Watanabe, K. Sato, K. Yasuoka, and T. Ebisuzaki, Phys. Rev. C PRVCAN 0556-2813 10.1103/PhysRevC.68.035806 68, 035806 (2003).
24. G. Watanabe, K. Sato, K. Yasuoka, and T. Ebisuzaki, Phys. Rev. C PRVCAN 0556-2813 10.1103/PhysRevC.69.055805 69, 055805 (2004).
25. G. Watanabe and H. Sonoda, in Soft Condensed Matter: New Research, edited by, K. I. Dillon, (Nova Science, New York, 2007), p. 1.
26. K. Oyamatsu and K. Iida, Phys. Rev. C PRVCAN 0556-2813 10.1103/PhysRevC.75.015801 75, 015801 (2007).
27. G. Watanabe, T. Maruyama, K. Sato, K. Yasuoka, and T. Ebisuzaki, Phys. Rev. Lett. PRLTAO 0031-9007 10.1103/PhysRevLett.94.031101 94, 031101 (2005).
28. T. Maruyama, K. Niita, K. Oyamatsu, T. Maruyama, S. Chiba, and A. Iwamoto, Phys. Rev. C PRVCAN 0556-2813 10.1103/PhysRevC.57.655 57, 655 (1998).
29. S. Chikazumi, T. Maruyama, S. Chiba, K. Niita, and A. Iwamoto, Phys. Rev. C PRVCAN 0556-2813 10.1103/PhysRevC.63.024602 63, 024602 (2001).
30. We remark that the expression of the Hamiltonian given in Ref. [29] is erroneous. The quantity L(Lw2 in our notation) in the term VSkyrme in Eq. (2) of Ref. [29] should be modified in a way as in Eq. (8) in the present paper (private communication with T. Maruyama).
31. T. Kido, T. Maruyama, K. Niita, and S. Chiba, Nucl. Phys. NUPABL 0375-9474 10.1016/S0375-9474(99)00736-8 A663, 877c (2000).
32. S. Nosé, J. Chem. Phys. 72, 2384 (1983).
33. S. Nosé, Mol. Phys. MOPHAM 0026-8976 10.1080/00268978400101201 52, 255 (1984).
34. W. G. Hoover, Phys. Rev. A PLRAAN 1050-2947 10.1103/PhysRevA.31.1695 31, 1695 (1985).
35. M. A. Pérez-García, J. Math. Chem. JMCHEG 0259-9791 10.1007/s10910-006-9120-y 40, 63 (2006).
36. W. H. Press, S. A. Teukolsky, W. T. Vettering, and B. P. Flannery, Numerical Recipes (Cambridge University Press, New York, 1986).
37. C. J. Pethick, D. G. Ravenhall, and C. P. Lorentz, Nucl. Phys. NUPABL 0375-9474 10.1016/0375-9474(94)00506-I A584, 675 (1995).
38. However, Fig. 9 of Ref. [26] shows a weak but systematic dependence of μp(0) at ρn=0.1 fm-3 on the density-dependence parameter L of the symmetry energy. Thus the information about L can be extracted from the proton chemical potential. In this case, μp(0) at ρn=0.1 fm-3 of model 1 is slightly smaller than that of model 2, which suggests a smaller L for model 1. This contradicts the conclusion obtained from the energy of pure neutron matter. However, due to the facts that the dependence of μp(0) on L is very weak and the values of μp(0) for both the QMD models are almost the same at this specific density, the comparison of L deduced from the energy of pure neutron matter is more reliable than that from μp(0) [54]. Thus we conclude the value of L for model 1 is greater than that for model 2.
39. G. Audi, A. H. Wapstra, and C. Thibault, Nucl. Phys. NUPABL 0375-9474 10.1016/j.nuclphysa.2003.11.003 A729, 337 (2003).
40. J. Nemeth and H. A. Bethe, Nucl. Phys. NUPABL 0375-9474 10.1016/0375-9474(68)90659-3 A116, 241 (1968).
41. To remove the finite boundary effects of the simulation box we need O(104) nucleons. However, in the previous study [24], we confirmed at least the two-point correlation function of simulations with 2048 nucleons is not so different from that with 16384 nucleons. Thus even in the case of 2048 nucleons the finite boundary effects little affect the phase diagram within the accuracy of Δρ~0.01ρ0 and ΔT~1 MeV.
42. G. Baym, H. A. Bethe, and C. J. Pethick, Nucl. Phys. NUPABL 0375-9474 10.1016/0375-9474(71)90281-8 A175, 225 (1971).
43. C. J. Pethick and D. G. Ravenhall, Annu. Rev. Nucl. Part. Sci. ARPSDF 0163-8998 10.1146/annurev.ns.45.120195.002241 45, 429 (1995).
44. G. Watanabe and K. Iida, Phys. Rev. C PRVCAN 0556-2813 10.1103/PhysRevC.68.045801 68, 045801 (2003).
45. K. Michielsen and H. De Raedt, Phys. Rep. PRPLCM 0370-1573 10.1016/S0370-1573(00)00106-X 347, 461 (2001).
46. J. R. Gott III, A. L. Melott, and M. Dickinson, Astrophys. J. ASJOAB 0004-637X 10.1086/164347 306, 341 (1986).
47. D. H. Weinberg, Publ. Astron. Soc. Pac. PASPAU 0004-6280 10.1086/132337 100, 1373 (1988).
48. T. Ohta, Prog. Theor. Phys. Suppl. PTPSEP 0375-9687 10.1143/PTPS.164.203 164, 203 (2006).
49. These saturation densities and saturation energies at xp=0.3 are determined by calculating the energy of the ground state of nuclear matter (xp=0.3) without the Coulomb interaction around the saturation density.
50. H. Shen, H. Toki, K. Oyamatsu, and K. Sumiyoshi, Nucl. Phys. NUPABL 0375-9474 10.1016/S0375-9474(98)00236-X A637, 435 (1998).
51. S. Yamada (private communication, 2007).
52. R. Susukita, Comput. Phys. Commun. CPHCBZ 0010-4655 10.1016/S0010- 4655(03)00349-7 155, 115 (2003).
53. T. Narumi, in Proceedings of the SC06 (High Performance Computing, Networking, Storage and Analysis) (Tampa, USA, 2006).
54. K. Iida (private communication, 2007).