New Pulsars Discovered in Arecibo Drift-Scan Searches
M. A. McLaughlinD. R. LorimerD. J. ChampionK. M. XilourisZaven ArzoumanianD. C. BackerJ. M. CordesA. N. LommenA. S. Fruchter
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We report on new pulsars discovered in Arecibo drift-scan data. Processing of 2200 square degrees of data has resulted in the detection of 41 known and 12 new pulsars. New pulsars include two millisecond pulsars, one solitary and one binary recycled pulsar, and one pulsar with very unusual pulse profile morphology and complex drifting subpulse behavior.Keywords:
X-ray pulsar
Pulsar planet
The double pulsar system PSR J0737-3039 offers an unprecedented opportunity for studying General Relativity and neutron-star magnetospheres. This system has a favourable orbital inclination such that the millisecond pulsar, A, is eclipsed when its slower companion, passes in front. High time resolution light curves of the eclipses reveal periodic modulations of the radio flux corresponding to the fundamental and the first harmonic of pulsar spin frequency. Eclipse modelling is highly sensitive to the geometrical configuration of the system and thus provides a unique probe for parameters like the inclination angle of pulsar B spin axis as well as their time evolution due to relativistic effects. We report on detailed fitting of the pulsar A eclipse light curves to a model that includes, for pulsar B, a simple dipolar magnetic field. We find that the eclipses can be reproduced very well, and we obtain precise measurements of pulsar B's orientation in space. We report on a search for secular changes caused by geodetic precession of pulsar B's spin axis.
Pulsar planet
X-ray pulsar
Eclipse
Precession
Ephemeris
Orbital inclination
Astrometry
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A 3.5 millisecond (ms) pulsar in a binary system was recently discovered in the error box of the unidentified EGRET source GRO J0752 + 17. We extend various gamma-ray pulsar models to the ms regime and discuss their predictions for the detectability of the 3.5 ms pulsar as well as for other known ms pulsars. We use the derived luminosities from these models to predict the magnetic field of the 3.5 ms pulsar. We conclude that if the 3.5 ms pulsar is indeed the source of the gamma-ray emission, its emission will either be unpulsed or this ms pulsar cannot have been recycled according to current recycling models
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Binary radio pulsar system J0737-3039 provides an exceptional opportunity to study innermost structure of pulsar magnetospheres due to very tight orbit, favorable directions of pulsars' rotation and magnetic axes and extremely fortuitous orientation of the orbit. In this system the millisecond pulsar A is eclipsed once per orbit. During eclipse a clear modulation at the 2.77 s period of pulsar B is seen, pointing unambiguously to magnetospheric origin of eclipses. A simple geometric model, based on the idea that the radio pulses are attenuated by synchrotron absorption on the closed magnetic field lines of pulsar B, can successfully reproduces the eclipse light curves down to intricate details. This detailed agreement confirms the dipolar structure of the neutron star's magnetic field. The model gives clear predictions for temporal evolution of eclipse profile due to geodetic precession of pulsar B. In addition, pulsar B shows orbital modulations of intensity, being especially bright at two short orbital phases. We showed that these modulations are due to distortion of pulsar B magnetosphere by pulsar A wind which produces orbital phase-dependent changes of the direction along which radio waves are emitted. Thus, pulsar B is intrinsically bright at all times but its radiation beam misses the Earth at most orbital phases.
Pulsar planet
X-ray pulsar
Eclipse
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Binary radio pulsar system J0737-3039 provides an exceptional opportunity to study innermost structure of pulsar magnetospheres due to very tight orbit, favorable directions of pulsars' rotation and magnetic axes and extremely fortuitous orientation of the orbit. In this system the millisecond pulsar A is eclipsed once per orbit. During eclipse a clear modulation at the 2.77 s period of pulsar B is seen, pointing unambiguously to magnetospheric origin of eclipses. A simple geometric model, based on the idea that the radio pulses are attenuated by synchrotron absorption on the closed magnetic field lines of pulsar B, can successfully reproduces the eclipse light curves down to intricate details. This detailed agreement confirms the dipolar structure of the neutron star's magnetic field.
The model gives clear predictions for temporal evolution of eclipse profile due to geodetic precession of pulsar B.
In addition, pulsar B shows orbital modulations of intensity, being especially bright at two short orbital phases. We showed that these modulations are due to distortion of pulsar B magnetosphere by pulsar A wind which produces orbital phase-dependent changes of the direction along which radio waves are emitted. Thus, pulsar B is intrinsically bright at all times but its radiation beam misses the Earth at most orbital phases.
Pulsar planet
X-ray pulsar
Eclipse
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X-ray pulsar
Pulsar planet
Galactic plane
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We report on new pulsars discovered in Arecibo drift-scan data. Processing of 2200 square degrees of data has resulted in the detection of 41 known and 12 new pulsars. New pulsars include two millisecond pulsars, one solitary and one binary recycled pulsar, and one pulsar with very unusual pulse profile morphology and complex drifting subpulse behavior.
X-ray pulsar
Pulsar planet
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The essential characteristics of the pulsar spinning and of the time scales,and the relation between them are analysed. The possible application of the millisecond pulsar to the time metrology is discussed. Based on the measurements of the arrival times of the radio pulses emitted from the millisecond pulsar(s),pulsar time and ensemble pulsar time can be established after the necessary time space transformation,correction and parameters fitting are applied to the measurements.It is possible for pulsar time,especially for ensemble pulsar time,to transfer the accuracy of atomic time from one period to another.It is also possible that pulsar time,especially ensemble pulsar time,may contribute to the knowledge of the stability of atomic time,although there is a dependence of pulsar time(and ensemble pulsar time)on atomic time. In addition, a binary pulsar time can be defined based on the orbital phase of a pulsar in a binary system.
Pulsar planet
Millisecond
X-ray pulsar
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Pulsar J0737-3039 is the only currently known double neutron star system in which both components exhibit themselves as radio pulsars. A number of peculiar properties very compact orbit (with period 2.4 hours), almost edge-on orientation of the orbital plane with respect to our line of sight provide us with unprecedented opportunities of checking effects of general relativity and probing the physics of pulsar magnetospheres. This report will provide a brief overview of our current understanding of some of the unique phenomena that have been observed in the double pulsar system: accumulation of relativistic plasma in the magnetosphere of normal pulsar causes periodic eclipses of its millisecond companion. Powerful wind of the millisecond pulsar distorts the magnetosphere of its normal companion, which affects the spindown and emission properties of normal pulsar. Future observational and theoretical work on this system may turn it into a Rosetta Stone of pulsar physics.
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We discuss the high‐energy emission from isolated and binary pulsars. Models of magnetospheric gamma‐ray emission from isolated pulsars will be constrained by CGRO observations of 'COS‐B‐like' sources. In addition to isolated pulsars, CGRO observations will constrain models for the interaction of pulsar winds with their nebular environments. We briefly describe the characteristics of unpulsed X‐ray and gamma‐ray emission expected in binary interacting pulsar systems where a radiative termination shock of the pulsar wind is produced. Two binary pulsar systems are candicate for high energy emission: young pulsars in massive binaries and old millisecond pulsars with low‐mass companion stars in compact binaries.
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