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The search for eclipsing binaries and rotation rates for Pre Main Sequence (PMS) Stars. Kurt Soto Advisor : Keivan Stassun. Masses of Pre-Main-Sequence Stars. Life of a star determined by its mass Theoretical models used to infer masses of stars have not been well tested for sub-solar masses
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The search for eclipsing binaries and rotation rates for Pre Main Sequence (PMS) Stars Kurt Soto Advisor : Keivan Stassun
Masses of Pre-Main-Sequence Stars • Life of a star determined by its mass • Theoretical models used to infer masses of stars have not been well tested for sub-solar masses • Need eclipsing binary stars! • Only 1 sub-solar mass PMS eclipsing binary Angular Momentum • Stars deplete most of their angular momentum by the time they reach the main sequence • The details of this are still poorly understood • Need rotation rates of stars at various stages of early evolution
Obtaining the Data(WIYN 0.9m!) • Mosaic capable of imaging 1 degree by 1 degree • 1.8 degree by 1.8 degree region • Two exposure lengths: 2 sec, 240 sec • Cycle every 45 minutes (detect eclipses) • 9 night observing run • Collaborator extends observing length to 20 days (long rotation periods and diurnal gaps) • 660 frames = 70 Gb of raw data => light curves for 100,000 stars
What’s Next • Use DAOFIND to locate stars from frame to frame • Adjust images for sky opacity • Prepare light curves • Look for signature eclipsing binary light curves • Calculate rotation rates and masses