AN ATLAS FOR INTERPRETING γ-RAY PULSAR LIGHT CURVES

By K. Watters, R. Romani, P. Weltevrede, Simon Johnston. 2008

163 citations recorded by the source corpus.

We have simulated a population of young spin-powered pulsars and computed the beaming pattern and light curves for the three main geometrical models: polar-cap emission, two-pole caustic (“slot gap”) emission and outer-magnetosphere emission. The light curve shapes depend sensitively on the magnetic inclination α and viewing angle ζ. We present the results as maps of observables such as peak multiplicity and γ-ray peak separation in the (α, ζ) plane. These diagrams can be used to locate allowed regions for radio-loud and radio-quiet pulsars and to convert observed fluxes to true all-sky emission.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/5f3b28b165774187c745c7343ed6036099eb2341

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

MODELING OF GAMMA-RAY PULSAR LIGHT CURVES USING THE FORCE-FREE MAGNETIC FIELD (2009, methodology): “Similar to the conventional TPC and OG models using the vacuum field (Watters et al. 2009), the double peak feature is most likely to appear at relatively large α and ζobs.”
FERMI LARGE AREA TELESCOPE OBSERVATIONS OF THE CRAB PULSAR AND NEBULA (2009, methodology): “The estimated value of α depends on the emission model used to interpret the data (Watters et al. 2009).”
PRECISE γ-RAY TIMING AND RADIO OBSERVATIONS OF 17 FERMI γ-RAY PULSARS (2010, methodology): “For this low Ė, the distance is constrained to be < 870 pc, assuming the flux correction factor fΩ = 1 (Watters et al. 2009) and using the LAT γ-ray flux (G100) from Abdo et al. (2010d) to keep the γ-ray efficiency < 1.”
THE FIRST FERMI LARGE AREA TELESCOPE CATALOG OF GAMMA-RAY PULSARS (2009, methodology): “The distribution can be compared with predictions of the TPC and OG models shown in Watters et al. (2009).”
RESISTIVE SOLUTIONS FOR PULSAR MAGNETOSPHERES (2011, background): “Deviations from the force-free geometry may be important for modeling the light curves of older pulsars which require wider gaps in the outer-gap models (Watters et al. 2009).”
EIGHT γ-RAY PULSARS DISCOVERED IN BLIND FREQUENCY SEARCHES OF FERMI LAT DATA (2010, background): “This is referred to as the γ-ray pulsar pseudo-distance dps, and incorporates the presumption of fΩ ∼ 1 in the absence of refined estimates of the solid angle, which can be obtained using pulse profile information (Watters et al. 2009).”