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The search for eclipsing binaries and rotation rates for Pre Main Sequence (PMS) Stars

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

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  1. The search for eclipsing binaries and rotation rates for Pre Main Sequence (PMS) Stars Kurt Soto Advisor : Keivan Stassun

  2. 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

  3. 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

  4. Crosstalk

  5. Zero Correction

  6. Dome Flats

  7. Sky Flats

  8. Area Correction

  9. Astrometry

  10. 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

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