# 7.5.1 Introduction

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.