High resolution calculations of merging neutron stars I: model description and hydrodynamic evolution

We present the results of 3D, high-resolution calculations of neutron star mergers. Using Newtonian gravity, but adding the forces from the emission of gravitational waves, we solve the hydrodynamics equations using the smoothed particle hydrodynamics method. The microscopic properties of the neutron star matter are described in terms of a new nuclear equation of state (EOS) based on the tables of Shen et al. (1998). The effects of neutrino emission of all flavours are accounted for. The new EOS is noticeably stiffer than the Lattimer-Swesty-EOS used in previous investigations. We find in general somewhat lower temperatures than previous investigations. This allows a substantial fraction of heavy nuclei to be present even in the inner parts of the torus that forms around the central object and yields important contributions to the neutrino opacity. The central object shows a rapid differential rotation with periods of

\sim

2ms, which we suspect to stabilize the central object on (at least) the simulation time scale against gravitational collapse. The differential rotation could wind up initial magnetic fields to

\sim 10^17

G.

References(53)

Figures(0)

LIGO: The Laser interferometer gravitational wave observatory

Alex Abramovici
(
- Caltech and
- Caltech, JPL and
- MIT, LNS
)
,
William E. Althouse
(
- Caltech and
- Caltech, JPL and
- MIT, LNS
)
,
Ronald W.P. Drever
(
- Caltech and
- Caltech, JPL and
- MIT, LNS
)
,
Yekta Gursel
(
- Caltech and
- Caltech, JPL and
- MIT, LNS
)
,
Seiji Kawamura
(
- Caltech and
- Caltech, JPL and
- MIT, LNS
)

et al.

- Science 256 (1992) 325-333
•
DOI:
- 10.1126/science.256.5055.325

PostNewtonian SPH

- Astrophys.J. 550 (2001) 846-859
•
e-Print:
- astro-ph/9910154
•
DOI:
- 10.1086/319769

- J.Comput.Phys. 121 357

Binary neutron stars in general relativity: Quasiequilibrium models

- Phys.Rev.Lett. 79 (1997) 1182-1185
•
e-Print:
- gr-qc/9704024
•
DOI:
- 10.1103/PhysRevLett.79.1182

The Stability of relativistic neutron stars in binary orbit

T.W. Baumgarte
(
- Illinois U., Urbana
)
,
G.B. Cook
(
- Cornell U., Radio. Space Res. Ctr.
)
,
M.A. Scheel
(
- Cornell U., Radio. Space Res. Ctr.
)
,
S.L. Shapiro
(
- Illinois U., Urbana and
- NCSA, Urbana
)
,
S.A. Teukolsky
(
- Cornell U., Radio. Space Res. Ctr. and
- Cornell U., LNS
)

- Phys.Rev.D 57 (1998) 6181-6184
•
e-Print:
- gr-qc/9705023
•
DOI:
- 10.1103/PhysRevD.57.6181

General relativistic models of binary neutron stars in quasiequilibrium

T.W. Baumgarte
(
- Illinois U., Urbana
)
,
G.B. Cook
(
- Cornell U., Radio. Space Res. Ctr.
)
,
M.A. Scheel
(
- Cornell U., Radio. Space Res. Ctr.
)
,
S.L. Shapiro
(
)
,
S.A. Teukolsky
(
)

- Phys.Rev.D 57 (1998) 7299-7311
•
e-Print:
- gr-qc/9709026
•
DOI:
- 10.1103/PhysRevD.57.7299

On the maximum mass of differentially rotating neutron stars

Thomas W. Baumgarte
(
- Illinois U., Urbana
)
,
Stuart L. Shapiro
(
)
,
Masaru Shibata
(
- Illinois U., Urbana and
- Osaka U.
)

- Astrophys.J.Lett. 528 (2000) L29
•
e-Print:
- astro-ph/9910565
•
DOI:
- 10.1086/312425

- Astrophys.J. 348 647

Tidal interactions of inspiraling compact binaries

- Astrophys.J. 400 (1992) 175-180
•
DOI:
- 10.1086/171983

The Virgo Project: A Wide Band Antenna for Gravitational Wave Detection

A. Giazotto
(
- INFN, Pisa
)

- Nucl.Instrum.Meth.A 289 (1990) 518-525,
- In *Cavalese 1988, Proceedings, General relativity and gravitational physics* 221-237.
•
DOI:
- 10.1016/0168-9002(90)91525-G