Rotation plays an important role in the evolution of stars. For decades rotation-age relationships have been used as surface rotation can be measured rather easily. Here we show the result of the measurement of rotation periods for a large number of Kepler solar-like stars along with their level of magnetic activity. We also study solar-like stars

During the last morning of the conference, a one-hour open discussion allowed the participants to debate some of the "hot" topics presented all along the meeting as well as on some of the key issues in the field mostly related with the work Prof. Michael J. Thompson studied during his carrier. The discussion covered theory and methods, current and

Seismic data contains information on stellar internal rotation, which plays an important role on dynamo models. Due to the uncertainties on the observations and stellar models, determining internal rotation of main-sequence solar-type stars has been challenging. Here, we use artificial rotational splittings for two-zone profiles to explore the

The SONG spectrograph has recently demonstrated its ability to perform solar radial velocity measurement during the first test run of the Solar-SONG initiative. A preliminary assessment of its performance is carried out here by comparing the results of Solar-SONG during the summer 2018 test run, with GOLF and VIRGO/SPM taken as reference

We determine Zr and Nb elemental abundances in barium stars to probe the operation temperature of the s-process that occurred in the companion asymptotic giant branch (AGB) stars. Along with Zr and Nb, we derive the abundances of a large number of heavy elements. They provide constraints on the s-process operation temperature and therefore on the s

We present confirmation of the planetary nature of PH-2b, as well as the first mass estimates for the two planets in the Kepler-103 system. PH-2b and Kepler-103c are both long-period and transiting, a sparsely populated category of exoplanets. We use Kepler light-curve data to estimate a radius, and then use HARPS-N radial velocities to determine