WE PROPOSE TO OBSERVE NEARBY COEVAL WIDE BINARY SYSTEMS AS FUNDAMENTAL ASTROPHYSICAL CALIBRATORS FOR PERIOD-AGE RELATIONS FOR LOW-MASS (< 0.8 .. MAIN SEQUENCE STARS). WE TARGET SYSTEMS WHERE SOLAR-LIKE OSCILLATIONS SHOULD BE DETECTABLE IN TESS IN THE F/G PRIMARY STAR ENABLING A PRECISE ASTEROSEISMIC AGE DETERMINATION (10-20%) AND WHERE THE SECONDARY STAR IS OF K OR M SPECTRAL TYPE. WE SELECT SYSTEMS THAT ARE SEPARATED BY MORE THAN 1 ARCMINUTE ON-SKY ENABLING THE SEPARATION OF THE PRIMARY AND SECONDARY LIGHTCURVES IN BOTH TESS AND LONG-BASELINE GROUND-BASED ARCHIVAL DATA. 68 SUCH BINARY SYSTEMS MEET THESE CRITERIA AND ARE VISIBLE IN CYCLE 4 NEARLY DOUBLING THE LITERATURE SAMPLE OF ASTEROSEISMIC AGE CALIBRATORS FOR PERIOD-AGE RELATIONS AND PROVIDING THE FIRST LARGE SAMPLE OF SEISMIC CALIBRATORS FOR LOW-MASS STARS. WE WILL PROVIDE A CALIBRATED PERIOD-AGE RELATIONSHIP APPLICABLE TO OLD-LOW MASS STARS ANCHORED TO THE PRECISE ASTEROSEISMIC AGE SCALE. SUCH A PERIOD-AGE RELATION WILL ENABLE RAPID AND PRECISE DETERMINATION OF AGES FOR TESS EXOPLANET HOST STARS AND OTHER COOL MAIN SEQUENCE DWARFS OF INTEREST. TESS IS UNIQUELY SUITED TO PROBING THE PROPERTIES OF THESE EXTREMELY BRIGHT BENCHMARK STARS. THE CHARACTERIZATION OF THESE SYSTEMS WILL PROVIDE SOME OF THE FEW EXAMPLES OF K/M STARS WITH PRECISION AGES AND CRITICAL TESTS FOR STELLAR EVOLUTIONARY MODELS.

University Of Hawaii, Honolulu

Investigators