Solar-like stars are characterised by variability phenomena due to a solar-like
magnetic activity that occurs in all the main sequence stars with a spectral type
later the F5. The most important variability phenomena exhibited by solar-like stars
are the rotational modulation of the stellar flux and the occurrence of flare events.
The rotational modulation of the stellar flux is due to the dark spots and bright
faculae unevenly distributed over the stellar disk. The stellar rotation modulate the
visibility of such surface inhomogeneities and consequently the flux coming from the
star. Hence, the period of light curves, for these stars, is coincident with the
stellar rotation period. Flare events are sporadic outbursts due to reconnection of
magnetic fields with subsequent plasma heating, particles acceleration and emission in
several bands, particularly UV and X-rays. A description of solar-like variability
phenomena can be found in Distefano et al. (2012) and references therein. The
detection and characterisation of solar-like stars is performed by means of the
SVD-Solar-Like and the SOS-Rotational-Modulation packages. The first package has the
tasks to perform a first selection of solar-like candidates and to identify
photometric outliers. The SOS package has the task to detect and characterise
rotational-modulation variability on the solar-like candidates.