SCIENTIFIC OBJECTIVES: ASTEROSEISMOLOGY HAS PROVED TO BE A VERY POWERFUL TOOL THANKS TO THE HIGH-PRECISION DATA OBTAINED BY THE SPACE MISSIONS SUCH AS KEPLER AND COROT. SOLAR-LIKE OSCILLATIONS HAVE BEEN DETECTED AND REPORTED FOR AROUND 15 600 RED GIANTS AND 540 MAIN-SEQUENCE STARS OBSERVED BY THE NOMINAL KEPLER MISSION. HENCE THESE STARS HAVE THEIR SURFACE GRAVITIES MASSES AND RADII OBTAINED WITH SEISMOLOGY. HOWEVER ACCORDING TO THE LATEST KEPLER STAR PROPERTIES CATALOG (MATHUR ET AL. IN PREP.) MORE THAN 24 000 RED GIANTS 127 000 FGK DWARFS AND ~10 000 SUBGIANTS WERE TARGETED. K2 HAS BEEN OBSERVING ~90 000 RED GIANTS AND DWARFS. MOREOVER THE CONTINUOUS PHOTOMETRIC DATA OF 4 YEARS (RESP. 3 MO) COLLECTED BY KEPLER (RESP. K2) CONTAIN THE SIGNATURE OF OTHER PHENOMENA SUCH AS CONVECTION ROTATION AND MAGNETISM WHICH ARE VERY IMPORTANT TO UNDERSTAND STELLAR EVOLUTION AND CAN ALSO BE USED TO OBTAIN PRECISE FUNDAMENTAL STELLAR PARAMETERS EVEN WHEN PULSATIONS ARE NOT DETECTED. WE PROPOSE TO PERFORM THE LARGEST HOMOGENEOUS ANALYSIS TO DATE OF SEISMIC OSCILLATIONS CONVECTION AND ROTATION/MAGNETIC ACTIVITY ACROSS THE FULL RANGE OF STELLAR SPECTRAL TYPES AND EVOLUTIONARY STATES PRESENT IN THE K2 AND KEPLER MISSIONS. WE WILL USE THE LONGEST PUBLICLY AVAILABLE TIME SERIES TO DERIVE THE MOST ACCURATE SURFACE GRAVITIES ROTATION PERIODS EVOLUTIONARY STATES AND MAGNETIC ACTIVITY LEVELS TO CHARACTERIZE ROTATION-AGEMAGNETIC ACTIVITY RELATIONSHIPS AND OSCILLATIONS-MAGNETISM INTERACTION. RELEVANCE: THE DETERMINATION OF THE GRAVITY MASS RADIUS AND AGE OF PLANET HOST STARS ALLOW US TO BETTER CHARACTERIZE THE PLANETARY SYSTEMS. BY STUDYING THE STELLAR SURFACE ROTATION PERIODS WE CAN BETTER UNDERSTAND THE ANGULAR MOMENTUM TRANSPORT INVOLVED DURING THE STELLAR EVOLUTION AND HAVE MORE ACCURATE ROTATION-AGE RELATIONSHIPS. FINALLY THE STUDY OF THE MAGNETIC ACTIVITY OF A LARGE NUMBER OF STARS WILL ALLOW US TO PUT THE SUN IN A BROADER CONTEXT. THIS WORK WILL ALSO HAVE AN IMPACT ON GALACTIC EVOLUTION STUDY. METHODOLOGY: WE WILL ANALYZE THE DATA WITH THE NEW VERSION OF THE A2Z PIPELINE (MATHUR ET AL. 2010) ON THE STARS WHERE NO ACOUSTIC MODES HAVE BEEN DETECTED OR COMPLETELY CHARACTERIZED SO FAR. IN THE CASE THAT STILL NO MODES ARE OBSERVED WE WILL STUDY THE CONVECTIVE BACKGROUND AS IT HAS BEEN SHOWN THAT THE GRANULATION TIMESCALE IS PROPORTIONAL TO THE SURFACE GRAVITY OF THE STAR (MATHUR ET AL. 2011). WE WILL DEVELOP AND AUTOMATE THE RECENT METHOD DEVELOPED BY KALLINGER ET AL. (2016) THAT PROVED IT IS POSSIBLE TO MEASURE LOGG VERY PRECISELY WITH THE AUTO-CORRELATION FUNCTION FOR STARS WHERE THE MODES ARE SLIGHTLY ABOVE THE NYQUIST FREQUENCY I.E. SUBGIANTS FOR THE LONG CADENCE DATA. WE WILL ANALYZE DWARFS AND SUBGIANTS OBSERVED BY KEPLER AND K2 TO LOOK FOR THEIR ROTATION PERIODS FOLLOWING GARCIA ET AL. (2014). THIS METHOD WAS SHOWN TO HAVE THE BEST COMBINATION OF COMPLETENESS AND RELIABILITY ACCORDING TO HARE AND HOUNDS BENCHMARKS (AIGRAIN ET AL. 2015). WE WILL CALIBRATE GYROCHRONOLOGY RELATION WITH THE BEST-CHARACTERIZED DWARFS AS DONE BY VAN SADERS ET AL. (2016) AND APPLY IT TO DWARFS WHEN APPLICABLE TO ESTIMATE THEIR AGES. FOR THE STARS WHERE A RELIABLE ROTATION PERIOD IS DETERMINED WE WILL COMPUTE A PHOTOMETRIC MAGNETIC PROXY AS DEFINED IN MATHUR ET AL. (2014). IN MANY CASES WE WILL HAVE COMPLEMENTARY SPECTROSCOPIC OBSERVATIONS (E.G. GAIA). DATA: WE WILL ANALYZE THE KEPLER Q0-Q17 DATA CALIBRATED WITH THE KADACS SOFTWARE (GARCIA ET AL. 2011; MATHUR ET AL. IN PREP.) AND THE K2 C1 TO C7 DATA PROCESSED BY VANDERBURG&JOHNSON (2014).