= Solution
A <cometary dust tail> is a superposition of <synchrones> and <syndynes>, rather than a material line emitted in one fixed direction. For grains larger than the stellar wavelength, $\beta\propto D^{-1}$: small grains have large $\beta$, are displaced rapidly in the anti-stellar direction, and make a relatively straight broad tail. Large grains have small $\beta$, remain closer to the comet's <Kepler orbit>, and make a more strongly curved dust trail. The observed position angle consequently depends on grain size, release time, orbital phase, and projection onto the <plane of the sky>.
Back to article page
