English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

The pulsar profile is characterised by two distinct emission components, thecore and the cone. The standard model of a pulsar radio emission beamoriginating from dipolar magnetic fields, places the core at the centresurrounded by concentric layers of inner and outer conal components. The coreemission is expected to have steeper spectra compared to the cones. We presenta detailed analysis of the relative differences in spectra between the core andconal emission from a large sample of 53 pulsars over a wide frequency rangebetween 100 MHz and 10 GHz. The core was seen to be much steeper than the conesparticularly between 100 MHz and 1 GHz with a relative difference between thespectral index $\Delta\alpha_{core/cone}\sim$ -1.0. In addition we also foundthe spectra of the outer conal components to be steeper than the inner conewith relative difference in the spectral index $\Delta\alpha_{in/out}\sim$+0.5. The flattening of the spectra from the magnetic axis towards the edge ofthe open field line region with increasing curvature of the field lines is anatural outcome of the coherent curvature radiation from charged solitonbunches, and explains the difference in spectra between the core and the cones.In addition due to the relativistic beaming effect, the radiation is onlyvisible when it is directed towards the observer over a narrow angle$\theta\leq 1/\gamma$, where $\gamma$ is the Lorentz factor of the outflowingplasma clouds. This restricts the emission particularly from outer cones, thatare associated with field lines with larger curvature thereby making thespectra steeper than the inner cones.

Spectral variation across Pulsar Profile due to Coherent Curvature Radiation