Interstellar scintillation of PSR J0437–4715

¹ Pushchino Radio Astronomy Observatory of Lebedev Physical Institute, 142290 Pushchino, Russia e-mail: [tania;shishov]@prao.psn.ru
² Isaac Newton Institute of Chile, Pushchino Branch
³ Department of Physics, University of California Santa Barbara, CA 93106, USA e-mail: cgwinn@physics.ucsb.edu

Received: 30 September 2005
Accepted: 13 March 2006

Abstract

Aims.We studied the turbulence spectrum of the local interstellar plasma in the direction of PSR J0437-4715, on the basis of our observations and those reported earlier by others.

Methods.We combine these data to form a structure function for the variations of phase along the line of sight to the pulsar. For observations that did not report them, we infer modulation indices from a theoretical model.

Results.We find that all of the observations fit a power-law spectrum of turbulence with index ± 0.20. We suggest that differences among reported values for scintillation bandwidth and timescale for this pulsar arise from differences in observing parameters. We suggest that refractive effects dominate for this line of sight, with refraction angle about twice the diffraction angle at 330 MHz observing frequency.

Conclusions.We suggest that the scattering of this pulsar lies in a layer of enhanced turbulence, about 10 pc from the Sun. We propose that the flux variations of the extragalactic source PKS 0405-385 arise in the same scattering layer.