### Abstract

A convenient formalism for averaging the losses produced by gravitational radiation back reaction over one orbital period was developed in an earlier paper. In the present paper we generalize this formalism to include the case of a closed system composed from two bodies of comparable masses, one of them having the spin S. We employ the equations of motion given by Barker and O'Connell, where terms up to linear order in the spin (the spin-orbit interaction terms) are kept. To obtain the radiative losses up to terms linear in the spin, the equations of motion are taken to the same order. Then the magnitude L of the angular momentum L, the angle κ subtended by S and L and the energy E are conserved. The analysis of the radial motion leads to a new parametrization of the orbit. From the instantaneous gravitational radiation losses computed by Kidder the leading terms and the spin-orbit terms are taken. Following Apostolatos, Cutler, Sussman, and Thorne, the evolution of the vectors S and L in the momentary plane spanned by these vectors is separated from the evolution of the plane in space. The radiation-induced change in the spin is smaller than the leading-order spin terms in the momentary angular momentum loss. This enables us to compute the averaged losses in the constants of motion E, L and L_{S} = L COSκ. In the latter, the radiative spin loss terms average to zero. An alternative description using the orbital elements a, e, and κ is given. The finite mass effects contribute terms, comparable in magnitude, to the basic, test-particle spin terms in the averaged losses.

Original language | English |
---|---|

Pages (from-to) | 3423-3432 |

Number of pages | 10 |

Journal | Physical Review D - Particles, Fields, Gravitation and Cosmology |

Volume | 57 |

Issue number | 6 |

Publication status | Published - Mar 15 1998 |

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### ASJC Scopus subject areas

- Mathematical Physics
- Physics and Astronomy(all)
- Nuclear and High Energy Physics
- Physics and Astronomy (miscellaneous)

### Cite this

*Physical Review D - Particles, Fields, Gravitation and Cosmology*,

*57*(6), 3423-3432.

**Spin effects in gravitational radiation back reaction. II. Finite mass effects.** / Gergely, L.; Perjés, Z.; Vasúth, M.

Research output: Contribution to journal › Article

*Physical Review D - Particles, Fields, Gravitation and Cosmology*, vol. 57, no. 6, pp. 3423-3432.

}

TY - JOUR

T1 - Spin effects in gravitational radiation back reaction. II. Finite mass effects

AU - Gergely, L.

AU - Perjés, Z.

AU - Vasúth, M.

PY - 1998/3/15

Y1 - 1998/3/15

N2 - A convenient formalism for averaging the losses produced by gravitational radiation back reaction over one orbital period was developed in an earlier paper. In the present paper we generalize this formalism to include the case of a closed system composed from two bodies of comparable masses, one of them having the spin S. We employ the equations of motion given by Barker and O'Connell, where terms up to linear order in the spin (the spin-orbit interaction terms) are kept. To obtain the radiative losses up to terms linear in the spin, the equations of motion are taken to the same order. Then the magnitude L of the angular momentum L, the angle κ subtended by S and L and the energy E are conserved. The analysis of the radial motion leads to a new parametrization of the orbit. From the instantaneous gravitational radiation losses computed by Kidder the leading terms and the spin-orbit terms are taken. Following Apostolatos, Cutler, Sussman, and Thorne, the evolution of the vectors S and L in the momentary plane spanned by these vectors is separated from the evolution of the plane in space. The radiation-induced change in the spin is smaller than the leading-order spin terms in the momentary angular momentum loss. This enables us to compute the averaged losses in the constants of motion E, L and LS = L COSκ. In the latter, the radiative spin loss terms average to zero. An alternative description using the orbital elements a, e, and κ is given. The finite mass effects contribute terms, comparable in magnitude, to the basic, test-particle spin terms in the averaged losses.

AB - A convenient formalism for averaging the losses produced by gravitational radiation back reaction over one orbital period was developed in an earlier paper. In the present paper we generalize this formalism to include the case of a closed system composed from two bodies of comparable masses, one of them having the spin S. We employ the equations of motion given by Barker and O'Connell, where terms up to linear order in the spin (the spin-orbit interaction terms) are kept. To obtain the radiative losses up to terms linear in the spin, the equations of motion are taken to the same order. Then the magnitude L of the angular momentum L, the angle κ subtended by S and L and the energy E are conserved. The analysis of the radial motion leads to a new parametrization of the orbit. From the instantaneous gravitational radiation losses computed by Kidder the leading terms and the spin-orbit terms are taken. Following Apostolatos, Cutler, Sussman, and Thorne, the evolution of the vectors S and L in the momentary plane spanned by these vectors is separated from the evolution of the plane in space. The radiation-induced change in the spin is smaller than the leading-order spin terms in the momentary angular momentum loss. This enables us to compute the averaged losses in the constants of motion E, L and LS = L COSκ. In the latter, the radiative spin loss terms average to zero. An alternative description using the orbital elements a, e, and κ is given. The finite mass effects contribute terms, comparable in magnitude, to the basic, test-particle spin terms in the averaged losses.

UR - http://www.scopus.com/inward/record.url?scp=0012340418&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=0012340418&partnerID=8YFLogxK

M3 - Article

AN - SCOPUS:0012340418

VL - 57

SP - 3423

EP - 3432

JO - Physical review D: Particles and fields

JF - Physical review D: Particles and fields

SN - 1550-7998

IS - 6

ER -