Bunching Coherent Curvature Radiation in Three-dimensional Magnetic Field Geometry: Application to Pulsars and Fast Radio Bursts

• Published in: The Astrophysical journal Vol. 868; no. 1; pp. 31 - 59
• Main Authors: Yang, Yuan-Pei, Zhang, Bing
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 20-11-2018; IOP Publishing
• Subjects: Astrophysics; Brightness temperature; Charge density; Coherent radiation; Curvature; Electron energy distribution; Magnetic fields; Neutron flux; Neutron stars; Power law; Powered models; Pulsar magnetospheres; Pulsars; Radiation; radiation mechanisms: non-thermal; Radiation spectra; Radio bursts; radio continuum: general; Variation
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/aae685

The extremely high brightness temperatures of pulsars and fast radio bursts (FRBs) require their radiation mechanisms to be coherent. Coherent curvature radiation from bunches has been long discussed as the mechanism for radio pulsars and recently for FRBs. Assuming that bunches are already generated in pulsar magnetospheres, we calculate the spectrum of coherent curvature radiation under a three-dimensional magnetic field geometry. Different from previous works assuming parallel trajectories and a monoenergetic energy distribution of electrons, we consider a bunch characterized by its length, curvature radius of the trajectory family, bunch opening angle, and electron energy distribution. We find that the curvature radiation spectra of the bunches are characterized by a multisegment broken power law, with the break frequencies depending on bunch properties and trajectory configuration. We also emphasize that in a pulsar magnetosphere, only the fluctuation of net charges with respect to the background (Goldreich-Julian) outflow can make a contribution to coherent radiation. We apply this model to constrain the observed spectra of pulsars and FRBs. For a typical pulsar ( , P = 0.1 s), a small fluctuation of the net charge δnGJ ∼ 0.1nGJ can provide the observable flux. For FRBs, the fluctuating net charge may be larger due to its abrupt nature. For δnGJ ∼ nGJ, a neutron star with a strong magnetic field and fast rotation is required to power an FRB in the spindown-powered model. The requirement is less stringent in the cosmic comb model thanks to the larger cross section and compressed charge density of the bunch made by the external astrophysical stream that combs the magnetosphere.