Filamentary structures and instabilities

High resolution images of radio sources often reveal filamentary structure (e.g. Perley et al. 1984; Fomalont et al. 1989; Hines, Owen & Eilek 1989). Much effort has been expended on explaining the formation of the filaments (e.g. Simon & Axford 1967; Eilek & Caroff 1979; Achterberg 1989; Gouveia Dal Pino & Opher 1989; Bodo et al. 1990), although the timescales for filament formation by thermal or synchrotron instability are probably too long (Hines et al. 1989).

There are two aspects of the filaments that any model should explain. These are the shape of the filaments and their enhanced brightness relative to the background emission. The models presented in this paper do not reproduce the linear structures often seen because I have assumed the magnetic field to be a Gaussian random field. The important point to note is that enhanced contrast can and will be obtained from a nonuniform field together with spectral ageing. At low frequencies the image is relatively smooth, with fluctuations about a mean level. At high frequencies the correct description is of high peaks on a generally low background, and it is these local peaks that I am referring to as `filaments.' It is not necessary to invoke instabilities to explain high contrast emission, although a more detailed model of the field structure is necessary to explain the shapes of the filaments.

The effect of spectral ageing in making a source appear more filamentary at high frequencies is perfectly general and does not depend on the assumption of a Gaussian random field. Any intensity histogram will develop a tail of bright points which have not yet faded as the electron population ages.

One way to differentiate between various models for filament formation is to examine the spectral indices of the filament and inter-filament emission (Hines et al. 1989; Carilli et al. 1991). I have considered this in Section 4, with some examples in Fig. 8. In the low-field (high diffusion) case, the inter-filament regions have steeper spectra than the bright peaks. This is true at all frequencies, although at low frequencies the difference in spectral indices is very small. In the intermediate case the correlation between intensity and spectral index is weak, except at very high frequencies nu > 10nubar_T where the very faintest regions start to have steeper spectra.

In the high field case, for low frequencies nu < 0.1nubar_T the bright regions have steeper spectra, whereas at high frequencies the situation is reversed so that the brighter regions tend to have flatter spectra. This behaviour arises because the initially bright regions fade and steepen most rapidly. At low frequencies they are still the brightest regions, so the brighter regions have steeper spectra. At high frequencies the initially bright regions have faded, so the bright regions are now unaged regions of low field and have flatter spectra.

In the low-field, high-diffusion case the correlation between intensity and spectral index is tight. The intermediate- and high-field cases show a great deal of scatter about the mean relation, so that an individual filament may not be typical of the source as a whole.

Explaining radio filaments by synchrotron ageing therefore has several advantages. Synchrotron ageing is ubiquitous and does not require special conditions in the source. The timescale for filament formation is the ageing timescale itself. And, at high frequency, the filaments will be bright and have a flatter spectral index than their surroundings, because the spectra steepen as they age, and the observed filaments are the least aged regions. For the low-field case, the filaments have flatter spectra at all frequencies.

On to:

Up to: ___________________________________
Peter Tribble,