  Disintegrating/evaporating rocky exoplanets can be observed not only as
transiting planets, but also in a grazing, non-transiting regime, where the
solid body of the planet does not transit, but part of the comet-like tail can
transit. In this case the forward scattering on the escaping particles is the
dominant process, which amplifies the photometric signal of the parent star
detected by the observer. The change in the flux is small, about 10^-3 (1000
ppm) at the best properties of the planetary system, but if the observation is
enough precise, the detection is possible. The planned Ariel space observatory
is designed to achieve a stability of < 100 ppm (the goal is 10 ppm) over the
temporal bandwidth of the transit, typically less than 10 hours. In this case
study we took the disintegrating exoplanet Kepler-1520b and changed the orbital
properties of the system to get a grazing, non-transiting orbit scenario, and
investigated, how different particle sizes, species, Ariel observational
channels, and other factors affect the amplitude of the forward-scattering
peak, and the detectability of the scattering event. Our most important result
is that the forward-scattering amplitude is not sensitive to the dust
composition, but is very sensitive to the particle size, observational channel,
and other factors. These factors can reduce mainly the detectability of
1-micron grains. 0.1-micron grains will be detectable at short wavelengths.
0.01-micron grains generate long and very small forward scattering amplitude,
which is below the detection limit. Based on our results we can conclude that
using Ariel will be possible to detect and investigate not only transiting, but
also grazing, non-transiting disintegrating exoplanets based on the forward
scattering. From the viewpoint of such objects the big advantage of Ariel will
be the possibility of multiwavelength observations.
