منابع مشابه
PSR J1829+2456: a relativistic binary pulsar
We report the discovery of a new binary pulsar, PSR J1829+2456, found during a mid-latitude drift-scan survey with the Arecibo telescope. Our initial timing observations show the 41-ms pulsar to be in a 28-hr, slightly eccentric, binary orbit. The advance of periastron ω̇ = 0.28 ± 0.01 deg yr is derived from our timing observations spanning 200 days. Assuming that the advance of periastron is pu...
متن کاملIs PSR B1757-24 a binary pulsar?
Binary pulsars with very small radial velocity corresponds to weak orbital effect at time scale of orbital period, and thus be treated as singular ones. However such pulsars may show their binary nature at long time scale by affecting pulsar frequency derivatives. Subtracting the magnetic dipole radiation predicted frequency derivatives from the measured ones, the intensity of long term orbital...
متن کاملThe Formation of the Double Pulsar PSR J0737−3039A/B
Recent timing observations of the double pulsar J0737−3039A/B have shown that its transverse velocity is extremely low, only 10 km/s, and nearly in the Plane of the Galaxy. With this new information, we rigorously re-examine the history and formation of this system, determining estimates of the pre-supernova companion mass, supernova kick and misalignment angle between the preand post-supernova...
متن کاملThe Formation of the Most Relativistic Pulsar PSR J0737−3039
We present an updated set of constraints for the progenitor of PSR J0737−3039 and for the natal kicks imparted to pulsar B taking into account both the evolutionary and kinematic history of the double neutron star. For this purpose, we use recently reported scintillation velocity measurements to trace the motion of the system in the Galaxy backwards in time as a function of the unknown orientat...
متن کاملRadiation pattern of the isolated pulsar PSR B 1828 - 11
Based on the free precession model of the isolated pulsar PSR B1828-11, Link & Epstein (2001) showed that the observed pulse durations require the radio beam to have a non-standard shape: the beam duration is larger for beam sweeps farthest from the dipole axis. In their analysis they assumed that the actual precession period is ≃ 500 d. Recent theoretical studies suggested that the actual prec...
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ژورنال
عنوان ژورنال: Symposium - International Astronomical Union
سال: 1981
ISSN: 0074-1809
DOI: 10.1017/s0074180900092913