A Generic Pulsar Radio Emission Mechanism

2006 ◽  
Vol 6 (S2) ◽  
pp. 74-80 ◽  
Author(s):  
D. B Melrose
Keyword(s):  
Radio Emission ◽  
Emission Mechanism ◽  
Pulsar Radio ◽  
Pulsar Radio Emission

scholarly journals Microstructure and the Pulsar Radio Emission Mechanism

1992 ◽  
Vol 128 ◽  
pp. 343-346
Author(s):  
Valentín Boriakoff
Keyword(s):  
Radio Emission ◽  
Radio Pulse ◽  
Emission Mechanism ◽  
Pulsar Radio ◽  
Pulsar Radio Emission

AbstractThe properties of pulsar radio pulse microstructure are reviewed, then consideration is given on how, in the frame of the Ruderman-Sutherland pulsar model, an emission mechanism can be devised which explains many of the known characteristics of micropulses and of subpulses.

scholarly journals Pulsar radio emission mechanism: Why no consensus?

2017 ◽  
Vol 932 ◽  
pp. 012011
Author(s):  
D B Melrose ◽  
M Z Rafat
Keyword(s):  
Radio Emission ◽  
Emission Mechanism ◽  
Pulsar Radio ◽  
Pulsar Radio Emission

scholarly journals Computer Simulation of Electron-Flow Bunching in the Pulsar Magnetosphere

1992 ◽  
Vol 128 ◽  
pp. 319-321
Author(s):  
Yu. A. Rylov
Keyword(s):  
Radio Emission ◽  
Electron Bunch ◽  
Electron Flow ◽  
Emission Mechanism ◽  
Pulsar Radio ◽  
Electron Bunches ◽  
Thermal Radio Emission ◽  
Gas Heating ◽  
Outflow Channel ◽  
Pulsar Radio Emission

Bunch curvature emission is one of the well known pulsar radio emission mechanisms. The problem of bunch formation is very important for understanding the pulsar radio emission mechanism. In the axisymmetric pulsar magnetospheric bunching arises in the outflow channel as a result of interaction between moving electrons (DP) and captured ones (SP) (Rylov 1988). A numerical simulation was undertaken to determine how strongly the electron flow is bunched. The bunching appears to be very strong. It can be treated as a gas of electron bunches rather than small fluctuations of the electron flow. The thermal radio emission of the electron-bunch gas has a very high brightness temperature and sharp directivity. The power consumed in electron-bunch gas heating is sufficient to explain the pulsar radio emission. The pulsar radio emission mechanism appears to be thermal (the electron bunches move chaotically) and coherent (electrons of the bunch emit coherently) at the same time. For this reason the radio emission mechanism is very stable.

Pulsar Radio Emission Mechanism

1973 ◽  
Vol 182 ◽  
pp. 935 ◽  
Author(s):  
Virtamo Jorma ◽  
Pekka Jauho
Keyword(s):  
Radio Emission ◽  
Emission Mechanism ◽  
Pulsar Radio ◽  
Pulsar Radio Emission

scholarly journals A rotation-driven pulsar radio emission mechanism

2020 ◽  
Vol 500 (4) ◽  
pp. 4549-4559
Author(s):  
D B Melrose ◽  
M Z Rafat ◽  
A Mastrano
Keyword(s):  
Radio Emission ◽  
Rest Frame ◽  
Radial Distance ◽  
Lorentz Factor ◽  
Emission Mechanism ◽  
Pulsar Radio ◽  
Specific Frequency ◽  
The Mean ◽  
Pulsar Radio Emission ◽  
Streaming Motion

ABSTRACT We propose and discuss an alternative pulsar radio emission mechanism that relies on rotation-driven plasma oscillations, rather than on a beam-driven instability, and suggest that it may be the generic radio emission mechanism for pulsars. We identify these oscillations as superluminal longitudinal waves in the pulsar plasma and point out that these waves can escape directly in the O mode. We argue that the frequency of the oscillations is ω0 ≈ ωp(2〈γ〉)1/2/γs, where γs is the Lorentz factor of bulk streaming motion and 〈γ〉 is the mean Lorentz factor in the rest frame of the plasma. The dependence of the plasma frequency ωp on radial distance implies a specific frequency-to-radius mapping, ω0∝r−3/2. Escape of the energy in these oscillations is possible if they are generated in overdense, field-aligned regions that we call fibres; the wave energy is initially refracted into underdense regions between the fibres, which act as ducts. Some implications of the model for the interpretation of pulsar radio emission are discussed.

scholarly journals Maser Theory of Pulsar Radiation

1971 ◽  
Vol 46 ◽  
pp. 414-428
Author(s):  
Hong-Yee Chiu
Keyword(s):  
Radio Emission ◽  
Plasma Emission ◽  
Emission Mechanism ◽  
Radio Flux ◽  
High Brightness ◽  
Pulsar Radio ◽  
Pulsar Radiation ◽  
Amplification Process ◽  
Coherent Plasma ◽  
Pulsar Radio Emission

In this paper we present an account of a theory of pulsar radio emission. The emission mechanism is via a maser amplification process. This theory avoids the difficulty of coherent plasma emission, that the bandwidth of radiation must be less than 1/2 λ. The high brightness radio temperature and the insensitivity of pulsar radio flux to pulsar periods can be easily accounted for.

scholarly journals Pulsar Radio Emission Mechanism: Radio Nanoshots as a Low-frequency Afterglow of Relativistic Magnetic Reconnection

2019 ◽  
Vol 876 (1) ◽  
pp. L6 ◽  
Author(s):  
Alexander Philippov ◽  
Dmitri A. Uzdensky ◽  
Anatoly Spitkovsky ◽  
Benoît Cerutti
Keyword(s):  
Radio Emission ◽  
Magnetic Reconnection ◽  
Low Frequency ◽  
Emission Mechanism ◽  
Pulsar Radio ◽  
Pulsar Radio Emission

scholarly journals Characteristics of Pulsar Radio Emission at Single-pulse Resolution

2000 ◽  
Vol 177 ◽  
pp. 149-154
Author(s):  
Avinash A. Deshpande
Keyword(s):  
Radio Emission ◽  
Weighted Average ◽  
Single Pulse ◽  
Position Angle ◽  
Complex Nature ◽  
Stable States ◽  
Pulsar Radio ◽  
Emission Profile ◽  
Secondary State ◽  
Pulsar Radio Emission

Pulsar radio emission shows remarkably rich, but complex behavior in both intensity and polarization when considered on a pulse-to-pulse basis. A large number of pulses, when averaged together, tend to approach & define stable shapes that can be considered as distinct signatures of different pulsars. Such average profiles have shapes ranging from that describable as a simple one-component profile to those suggesting as many as 9 components. The components are understood as resulting from an average of many, often narrower, intities — the subpulses —that appear within the longitude range of a given component. The pulse components are thusformedand represent statistically an intensity-weighted average pattern of the radiation received as a function of longitude. The profile mode changes recognized in many pulsars suggest that the emission profile of a given pulsar may have two quasi-stable states, with one (primary) state more probable/brighter than the other (secondary) state. There are also (often associated) polarization modes that represent polarization states that are orthogonal to each other. The complex nature of orthogonaljumpsobserved in polarization position-angle sweeps may be attributable to possible superposition of two profile/polarization modes with orthogonal polarizations.

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