TY - GEN
T1 - “Numerical relativity
T2 - 23rd Workshop on General Relativity and Gravitation in Japan, JGRG 2013
AU - Collaborators
AU - Hotokezaka, Kenta
AU - Kiuchi, K.
AU - Muransushi, T.
AU - Nagakura, H.
AU - Sekiguchi, Y.
AU - Shibata, M.
AU - Kyutoku, K.
AU - Okawa, H.
AU - Taniguchi, K.
AU - Tanaka, M.
AU - Wanajo, S.
AU - Ioka, K.
N1 - Publisher Copyright:
© JGRG 2013.
PY - 2013
Y1 - 2013
N2 - Neutron Star equation of State can be measured through • tidal effects in the late inspiral stage and • fourier peak frequency of gws from HMNS. However, to succeed in measuring the EOS, higher order PN corrections and • longer and more accurate NR computation are needed. GRB130603B is a golden event • This could be direct evidence of compact binary merger hypothesis of short GRBs. • The time scale, brightness, and color of Kilonova are quite consistent with the NR prediction. For NS5NS merger models, soft EOSs are favored. For BH5NS merger models, stiff EOSs are favored.
AB - Neutron Star equation of State can be measured through • tidal effects in the late inspiral stage and • fourier peak frequency of gws from HMNS. However, to succeed in measuring the EOS, higher order PN corrections and • longer and more accurate NR computation are needed. GRB130603B is a golden event • This could be direct evidence of compact binary merger hypothesis of short GRBs. • The time scale, brightness, and color of Kilonova are quite consistent with the NR prediction. For NS5NS merger models, soft EOSs are favored. For BH5NS merger models, stiff EOSs are favored.
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M3 - Conference contribution
AN - SCOPUS:85092190102
T3 - JGRG 2013 - Proceedings of the 23rd Workshop on General Relativity and Gravitation in Japan
SP - 388
EP - 409
BT - JGRG 2013 - Proceedings of the 23rd Workshop on General Relativity and Gravitation in Japan
PB - Hirosaki University
Y2 - 5 November 2013 through 8 November 2013
ER -