Table 1:
Known and likely DNS binaries. Listed are the pulse period , orbital period , orbital eccentricity , characteristic age , and expected binary coalescence timescale due to gravitational wave emission calculated from Equation (7). To distinguish between definite and candidate DNS systems, we also list whether the masses of both components have been determined via the measurement of two or more post-Keplerian parameters as described in Section 4.4. |

Table 2:
Parameters for the 20 isolated millisecond pulsars currently known in the Galactic disk. Four of the pulsars (J0609+2130, J1038+0032, J1753–1914 and J2235+1506) are thought to be the descendants of high-mass binary systems. Listed are the spin period , the base-10 logarithms of the characteristic age and surface magnetic field strength (see Section 2.2), the distance derived from the Cordes & Lasio electron density model [88, 89] or independently (when available), and the transverse speed inferred from and a proper motion measurement (when available). Key publications for each pulsar are referenced to the bibliography. |

Table 3:
Parameters for the 19 eccentric (e > 0.05) binary pulsars currently known that are not in globular clusters. In addition to the parameters listed in Table 2, we also give the binary period , the projected semi-major axis of the orbit in units of light seconds, the orbital eccentricity , and the companion mass evaluated from the mass function assuming a pulsar mass of and an inclination angle of 60 degrees (see Section 4.4) or (when known) from independent measurements. |

Table 4:
Parameters for 64 low-eccentricity binary pulsars currently known in the Galactic disk. The parameters listed are defined in Tables 2 and 3. |

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