Post-Newtonian smoothed particle hydrodynamics

被引:35
作者
Ayal, S [1 ]
Piran, T
Oechslin, R
Davies, MB
Rosswog, S
机构
[1] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel
[2] Univ Basel, Dept Phys & Astron, CH-4003 Basel, Switzerland
[3] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England
[4] Univ Cologne, Ctr Parallel Comp ZPR ZAIK, D-5000 Cologne 41, Germany
关键词
gravitation; hydrodynamics; relativity; stars : neutron;
D O I
10.1086/319769
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We introduce an adaptation of the well-known tree+SPH numerical scheme to post-Newtonian (PN) hydrodynamics and gravity. Our code solves the (0 + 1 + 2.5)PN equations. These equations include Newtonian hydrodynamics and gravity (0PN), the first-order relativistic corrections to those (1PN), and the lowest order gravitational radiation terms (2.5PN). We test various aspects of our code using analytically solvable test problems. We then proceed to study the 1PN effects on binary neutron star coalescence by comparing calculations with and without the 1PN terms. We find that the effect of the 1PN terms is rather small. The largest effect arises with a stiff equation of state for which the maximum rest mass density increases. This could induce black hole formation. The gravitational wave luminosity is also affected.
引用
收藏
页码:846 / 859
页数:14
相关论文
共 38 条
[1]  
BARISH BC, 1998, NEW WORLDS ASTROPART, P391
[2]   A HIERARCHICAL O(N-LOG-N) FORCE-CALCULATION ALGORITHM [J].
BARNES, J ;
HUT, P .
NATURE, 1986, 324 (6096) :446-449
[3]   General relativistic models of binary neutron stars in quasiequilibrium [J].
Baumgarte, TW ;
Cook, GB ;
Scheel, MA ;
Shapiro, SL ;
Teukolsky, SA .
PHYSICAL REVIEW D, 1998, 57 (12) :7299-7311
[4]  
BENZ W, 1990, NATO ADV SCI I C-MAT, V302, P269
[5]   DYNAMIC MASS EXCHANGE IN DOUBLY DEGENERATE BINARIES .1. 0.9 AND 1.2 M STARS [J].
BENZ, W ;
BOWERS, RL ;
CAMERON, AGW ;
PRESS, WH .
ASTROPHYSICAL JOURNAL, 1990, 348 (02) :647-667
[6]   POST-NEWTONIAN HYDRODYNAMICS AND POST-NEWTONIAN GRAVITATIONAL-WAVE GENERATION FOR NUMERICAL RELATIVITY [J].
BLANCHET, L ;
DAMOUR, T ;
SCHAFER, G .
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 1990, 242 (02) :289-305
[7]   MERGING NEUTRON-STARS .1. INITIAL RESULTS FOR COALESCENCE OF NONCOROTATING SYSTEMS [J].
DAVIES, MB ;
BENZ, W ;
PIRAN, T ;
THIELEMANN, FK .
ASTROPHYSICAL JOURNAL, 1994, 431 (02) :742-753
[8]  
DAVIES MB, 1993, ASTRON ASTROPHYS, V272, P430
[9]  
FIDECARO F, 1997, P 12 IT C GEN REL GR, P163
[10]   Possible explanation for star-crushing effect in binary neutron star simulations [J].
Flanagan, ÉÉ .
PHYSICAL REVIEW LETTERS, 1999, 82 (07) :1354-1357