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Coherent Radio Emission from Pulsars  [PDF]
Dipanjan Mitra,G. Melikidze,Janusz Gil
Physics , 2015,
Abstract: We review a physical model where the high brightness temperature of 10$^{25}-10^{30}$ K observed in pulsar radio emission is explained by coherent curvature radiation excited in the relativistic electron-positron plasma in the pulsar magnetosphere.
Coherent Radio Emission from Pulsars  [PDF]
Y. E. Lyubarsky
Physics , 2002,
Abstract: Generation of the pulsar radio emission from plasma waves excited by the two-stream instability is considered. Special attention is given to propagation effects.
Emission altitude in radio pulsars  [PDF]
J. Kijak
Physics , 2002,
Abstract: This paper presents a method of estimation of emission altitudes using observational data - precise measurements of pulse profile widths at low intensity level. The analysis of emission altitudes obtained using this method for a large number of pulsars gives constraints that should be useful for theory of coherent pulsar emission. It seems that radio emission originates at altitudes of about few percent of the light cylinder and that they depend on frequency, pulsar period and period derivative.
Radio Pulsars  [PDF]
V. S. Beskin,S. V. Chernov,C. R. Gwinn,A. Tchekhovskoy
Physics , 2015, DOI: 10.1007/s11214-015-0173-8
Abstract: Almost 50 years after radio pulsars were discovered in 1967, our understanding of these objects remains incomplete. On the one hand, within a few years it became clear that neutron star rotation gives rise to the extremely stable sequence of radio pulses, that the kinetic energy of rotation provides the reservoir of energy, and that electromagnetic fields are the braking mechanism. On the other hand, no consensus regarding the mechanism of coherent radio emission or the conversion of electromagnetic energy to particle energy yet exists. In this review, we report on three aspects of pulsar structure that have seen recent progress: the self-consistent theory of the magnetosphere of an oblique magnetic rotator; the location, geometry, and optics of radio emission; and evolution of the angle between spin and magnetic axes. These allow us to take the next step in understanding the physical nature of the pulsar activity.
Radio pulsars: the search for truth  [PDF]
V. S. Beskin,Ya. N. Istomin,A. A. Philippov
Physics , 2013, DOI: 10.3367/UFNe.0183.201302e.0179
Abstract: It was as early as the 1980s that A V Gurevich and his group proposed a theory to explain the magnetosphere of radio pulsars and the mechanism by which they produce coherent radio emission. The theory has been sharply criticized and is currently rarely mentioned when discussing the observational properties of radio pulsars, even though all the criticisms were in their time disproven in a most thorough and detailed manner. Recent results show even more conclusively that the theory has no internal inconsistencies. New observational data also demonstrate the validity of the basic conclusions of the theory. Based on the latest results on the effects of wave propagation in the magnetosphere of a neuron star, we show that the developed theory does indeed allow quantitative predictions of the evolution of neutron stars and the properties of the observed radio emission.
On the Search for Coherent Radiation from Radio Pulsars  [PDF]
J. M. Smits,B. W. Stappers,J-P. Macquart,R. Ramachandran,J. Kuijpers
Physics , 2003, DOI: 10.1051/0004-6361:20030699
Abstract: We have examined data from pulsars B0950+08 and B0329+54 for evidence of temporally coherent radiation using the modified coherence function (MCF) technique of Jenet et al. (2001). We consider the influence of both instrumental bandpass and interstellar propagation effects. Even after removal of the effects due to the instrumental bandpass, we detect a signature in the MCF of our PSR B0329+54 data which is consistent with the definition of a coherent signal. However, we model the effects due to interstellar scintillation for this pulsar and show that it reproduces the observed signature. In particular, the temporal coherence time is close to the reciprocal of the decorrelation bandwidth due to diffractive scintillation. Furthermore, comparison of the coherence times of three pulsars reported by Jenet et al. (2001) with their expected diffractive decorrelation bandwidths suggests that the detection of coherence in these pulsars is also likely a result of interstellar scintillation, and is not intrinsic to the pulsars.
On the Possibility of Curvature Radiation from Radio Pulsars  [PDF]
H. Lesch,A. Jessner,M. Kramer,Th. Kunzl
Physics , 1998,
Abstract: We consider the widespread hypothesis that coherent curvature radiation is responsible for the radio emission of pulsars. The comparison of energy conservation and the published data and luminosities explicitely proves that coherent curvature radiation cannot be the source for the radio emission of pulsars for frequencies below a few GHz. At higher frequencies coherent curvature radiation can be ruled out because neither the observationally deduced emission heights nor the observed radius to frequency mapping can be reproduced by this mechanism. Our argumentation is in accordance with the more general critics (e.g. Melrose 1992) that no adequate bunching mechanism has been identified for coherent curvature radiation. We present 5 examples (0329+29, 0355+54, 0540+23, 1133+16, 1916+10) of pulsars whose high frequency (larger than 1.4. GHz, up to 32 GHz) luminosities are well known, and as a low frequency example the faintest radio pulsar 0655+64 of the Taylor et al (1993) sample.
Unraveling the nature of coherent pulsar radio emission  [PDF]
Dipanjan Mitra,Janusz Gil,George I. Melikidze
Physics , 2009, DOI: 10.1088/0004-637X/696/2/L141
Abstract: Forty years have passed since the discovery of pulsars, yet the physical mechanism of their coherent radio emission is a mystery. Recent observational and theoretical studies strongly suggest that the radiation outcoming from the pulsar magnetosphere consists mainly of extraordinary waves polarized perpendicular to the planes of pulsar dipolar magnetic field. However, the fundamental question whether these waves are excited by maser or coherent curvature radiation, remains open. High quality single pulse polarimetry is required to distinguish between these two possible mechanisms. Here we showcase such {\it decisive} strong single pulses from 10 pulsars observed with the GMRT, showing extremely high linear polarization with the position angle following locally the mean position angle traverse. These pulses, which are relatively free from depolarization, must consist of exclusively single polarization mode. We associate this mode with the extraordinary wave excited by the coherent curvature radiation. This crucial observational signature enables us to argue, for the first time, in favor of the coherent curvature emission mechanism, excluding the maser mechanism.
Energetic Young Radio Pulsars  [PDF]
J. F. Bell
Physics , 1997,
Abstract: Young radio pulsars shed vast amounts of rotational energy, sometimes as high as 100,000 times the total energy loss rate from the sun. The wide range of phenomena resulting from this energy loss include: glitches, timing noise, jets, bow shocks, bullets and plerions and are be reviewed from an observational perspective. Past and proposed surveys for young radio pulsars are summarised along with pulsar birth velocities and associations with supernova remnants. There are now 4 radio pulsars with measured braking indices. The resulting constraints on the evolution of young radio pulsars are discussed in light of the presently observed population of pulsars. Observations at optical, X-ray and gamma ray energies which provide a unique opportunity to study the emission and magnetospheric processes are described briefly. The status of pulsar birth velocities and supernova remnant associations are summarised.
A Fan Beam Model for Radio Pulsars. I. Observational Evidence  [PDF]
Hong Guang Wang,Fei Peng Pi,Xiao Ping Zheng,Chun Lan Deng,Sai Qin Wen,Feng Ye,Kai Ying Guan,Yi Liu,Li Qing Xu
Physics , 2014, DOI: 10.1088/0004-637X/789/1/73
Abstract: We propose a novel beam model for radio pulsars based on the scenario that the broadband and coherent emission from secondary relativistic particles, as they move along a flux tube in a dipolar magnetic field, forms a radially extended sub-beam with unique properties. The whole radio beam may consist of several sub-beams, forming a fan-shaped pattern. When only one or a few flux tubes are active, the fan beam becomes very patchy. This model differs essentially from the conal beam models in the respects of beam structure and predictions on the relationship between pulse width and impact angle $\beta$ (the angle between line of sight and magnetic pole) and the relationship between emission intensity and beam angular radius. The evidence for this model comes from the observed patchy beams of precessional binary pulsars and three statistical relationships found for a sample of 64 pulsars, of which $\beta$ were mostly constrained by fitting polarization position angle data with the Rotation Vector Model. With appropriate assumptions, the fan beam model can reproduce the relationship between 10\% peak pulse width and $|\beta|$, the anticorrelation between the emission intensity and $|\beta|$, and the upper boundary line in the scatter plot of $|\beta|$ versus pulsar distance. An extremely patchy beam model with the assumption of narrowband emission from one or a few flux tubes is studied and found unlikely to be a general model. The implications of the fan beam model to the studies on radio and gamma-ray pulsar populations and radio polarization are discussed.
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