2.1

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1 sekig@th.nao.ac.jp 1. G ab kt ab, (1) k 8pGc 4, G c

2 3 1 2) ( ab ) (g ab ) (K ab ) (g ab, K ab ) 1 t a S n a a b a 2.3 a b i (t a ) g ab ab n a n b K ab (1/2)L n g ab n a L n n a Lie

3 3), 3 BSSN (Baumgarte Shapiro Shibata Nakamura) 3), 4) 10 5) g/cm K 4 6) (inner core) (outer core) 7) (r nuc g/cm 3 ) 5 1 (G 1, G 2, r nuc ) 1.6 M Model G 1 G 2 r nuc (g/cm 3 ) a b c d

4 8) (1) (2) (Y e ) (3) 6 G 4/3 P r G (2 3 M ) (q cj/(gm 2 ) 0 1.1) 7 9) 2 (q) a b d c a a b d c P P cold P th (2) P th P cold 0 P cold K 1 r G 1, r r nuc, P P K 2 r G 2, r r nuc, (3) 6 7 (e F ) (k B T, k B e F Y e k B T 10 1/3 r 1/3 T g/cm K

5 G 1 4/3 G P th P th (G th 1)re th (4) G th G 1 (G 1, G 2, r nuc ) 1.6 M 1 2 (q 0) ( 2 M ) (1.6 M ) 2 M ) G

6 3 x z g 10), 11) 12) 2 M G 4/3 (P r G ) 3 x z

7 4 x z 5 S 17 S/10 17 g/cm 2 t k n S W R 19 km g g g 11) T 11 T/10 11 K S 17 S/10 17 g/cm 2 R disk L n 2pR 2 disk F n T 2 11S ergs/s 70 km 13) E nn ergs/s

8 6 x z (k B ) ) 17) M 6) ) 18) 19) 20) 21) 22) 22)

9 7 10 kpc 7 10 kpc khz

10 1) UT Physics 3, 2) York Jr., J. W., 1979, Kinematics and Dynamics of General Relativity, in Sources of Gravitational Radiation, ed. by Smarr L. (Cambridge University Press, Cambridge) 3) Shibata M., Nakamura T., 1995, Phys. Rev. D 52, ) Baumgarte T. W., Shapiro S. L., 1999, Phys. Rev. D 59, ) Pretorius F., 2009, Binary Black Hole Coalescence, in Physics of Relativistic Objects in Compact Binaries: from Birth to Coalescence, ed. by Colpi M., et al. (Springer Verlag) 6) Woosley S. E., Heger A., Weaver T. A., 2002, Rev. Mod. Phys. 74, ) Bethe H. A., 1990, Rev. Mod. Phys. 62, 801 8) Sekiguchi Y., Shibata M., 2005, Phys. Rev. D 71, ) Takahara M., Sato K., 1984, Prog. Theor. Phys. 72, ) Woosley S. E., 1993, Astrophys. J. 405, ) MacFadyen A., Woosley S. E., 1999, Astrophys. J. 524, ) Sekiguchi Y., Shibata, M., 2007, Prog. Theor. Phys. 117, ) Setiawan S., Ru#ert M., Janka H.-Th., 2004, MNRAS 352, ) Ott C. D., et al., 2007, Phys. Rev. Lett. 98, ) Sekiguchi Y., 2008, Ph.D. thesis, Univ. of Tokyo 16) Sekiguchi Y., 2009, Prog. Theor. Phys. submitted 17) Sekiguchi Y., 2009, Prog. Theor. Phys. submitted 18) Shen H., et al., 1998, Nucl. Phys. A 637, ) Fuller G. M., Fowler W. A., Newman M. J., 1985, Astrophys. J. 293, 1 20) Cooperstein J., van den Horn L. J., Baron E. A., 1986, Astrophys. J. 309, ) Ru#ert M., Janka H.-T., Schaefer G., 1996, Astron. Astrophys. 311, ) Burrows A., Reddy S., Thompson T. A., 2006, Nucl. Phys. A 777, 356 Exploring Massive Stellar Collapse via Numerical Relativity Yuichiro SEKIGUCHI Division of Theoretical Astronomy, National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo , Japan sekig@th.nao.ac.jp Abstract: There are significant progresses in Numerical Relativity, in which Einstein s equation is solved numerically, thanks to the recent advanced e#orts and studies. For example, simulations of black hole formation in the collapse of massive stellar core, and calculations of gravitational waveforms from binary neutron star merger become possible. In this article, first, I will briey address the principle di#erences between simulating in Newtonian theory and in general relativity, aiming at introducing readers into the world of numerical relativity. Then, some recent results such as criteria of prompt black hole formation in gravitational collapse of massive stellar core, and formation mechanism of black hole surrounded by accretion torus, will be reported. Finally, one of the hottest topics in Numerical Relativity, that is, Numerical Relativity with microphysics (a finite temperature nuclear equation of state, weak interactions such as electron capture and neutrino cooling), will be mentioned

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