Extremely Anisotropic Scintillations

TL;DR

This paper models extremely anisotropic interstellar scintillation patterns as effectively one-dimensional, explaining rapid quasar scintillations and predicting repeatable flux variations, thereby constraining the scattering medium's properties.

Contribution

It introduces a totally anisotropic, one-dimensional scintillation model that fits observational data and discusses implications for the scattering medium's anisotropy and velocity.

Findings

The model fits two-station time-delay measurements well.

Predicted flux variation repeats seasonally for J1819+3845.

Finite anisotropy introduces minor improvements but is not justified by data.

Abstract

A small number of quasars exhibit interstellar scintillation on time-scales less than an hour; their scintillation patterns are all known to be anisotropic. Here we consider a totally anisotropic model in which the scintillation pattern is effectively one-dimensional. For the persistent rapid scintillators J1819+3845 and PKS1257-326 we show that this model offers a good description of the two-station time-delay measurements and the annual cycle in the scintillation time-scale. Generalising the model to finite anisotropy yields a better match to the data but the improvement is not significant and the two additional parameters which are required to describe this model are not justified by the existing data. The extreme anisotropy we infer for the scintillation patterns must be attributed to the scattering medium rather than a highly elongated source. For J1819+3845 the totally anisotropic model predicts that the particular radio flux variations seen between mid July and late August should repeat between late August and mid November, and then again between mid November and late December as the Earth twice changes its direction of motion across the scintillation pattern. If this effect can be observed then the minor-axis velocity component of the screen and the orientation of that axis can both be precisely determined. In reality the axis ratio is finite, albeit large, and spatial decorrelation of the flux pattern along the major axis may be observable via differences in the pairwise fluxes within this overlap region; in this case we can also constrain both the major-axis velocity component of the screen and the magnitude of the anisotropy.