# Post-Newtonian hydrodynamic equations using the (3+1) formalism in general relativity

Banach Center Publications (1997)

- Volume: 41, Issue: 2, page 85-93
- ISSN: 0137-6934

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topAsada, Hideki. "Post-Newtonian hydrodynamic equations using the (3+1) formalism in general relativity." Banach Center Publications 41.2 (1997): 85-93. <http://eudml.org/doc/252235>.

@article{Asada1997,

abstract = {The post-Newtonian (PN) hydrodynamic equations are obtained in the (3+1) formalism, which include the 2.5PN order as the reaction due to the quadrupole gravitational radiation. These equations are valid in various slice conditions, while we adopt a kind of transverse gauge condition to determine the shift vector. In particular, we describe methods to solve the 2PN tensor potential which arises from the spatial 3-metric. Our formulaton in the PN approximation using the (3+1) formalism will be useful for numerical computations providing an initial data for the final merging phase of coalescing binary neutron stars which can be treated only by fully general relativistic simulations.},

author = {Asada, Hideki},

journal = {Banach Center Publications},

keywords = {post-Newtonian hydrodynamic equations; quadrupole gravitational radiation; (3+1) formalism},

language = {eng},

number = {2},

pages = {85-93},

title = {Post-Newtonian hydrodynamic equations using the (3+1) formalism in general relativity},

url = {http://eudml.org/doc/252235},

volume = {41},

year = {1997},

}

TY - JOUR

AU - Asada, Hideki

TI - Post-Newtonian hydrodynamic equations using the (3+1) formalism in general relativity

JO - Banach Center Publications

PY - 1997

VL - 41

IS - 2

SP - 85

EP - 93

AB - The post-Newtonian (PN) hydrodynamic equations are obtained in the (3+1) formalism, which include the 2.5PN order as the reaction due to the quadrupole gravitational radiation. These equations are valid in various slice conditions, while we adopt a kind of transverse gauge condition to determine the shift vector. In particular, we describe methods to solve the 2PN tensor potential which arises from the spatial 3-metric. Our formulaton in the PN approximation using the (3+1) formalism will be useful for numerical computations providing an initial data for the final merging phase of coalescing binary neutron stars which can be treated only by fully general relativistic simulations.

LA - eng

KW - post-Newtonian hydrodynamic equations; quadrupole gravitational radiation; (3+1) formalism

UR - http://eudml.org/doc/252235

ER -

## References

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