Improving Pulsar Distances by Modelling Interstellar Scattering

Details Improving Pulsar Distances by Modelling Interstellar Scattering Improving Pulsar Distances by Modelling Interstellar Scattering

1998-06-22

arxiv.org/abs/astro-ph/9806291v1

Astronomy and Astrophysics

Astrophysics

To be published in MNRAS, 7 pages, 3 figures

Scientific paper

10.1046/j.1365-8711.1998.01926.x

We present here a method to study the distribution of electron density fluctuations in pulsar directions as well as to estimate pulsar distances. The method, based on a simple two-component model of the scattering medium discussed by Gwinn et al. (1993), uses scintillation & proper motion data in addition to the measurements of angular broadening & temporal broadening to solve for the model parameters, namely, the fractional distance to a discrete scatterer and the ascociated relative scattering strength. We show how this method can be used to estimate pulsar distances reliably, when the location of a discrete scatterer (e.g. an HII region), if any, is known. Considering the specific example of PSR B0736-40, we illustrate how a simple characterization of the Gum nebula region (using the data on the Vela pulsar) is possible and can be used along with the temporal broadening measurements to estimate pulsar distances.

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