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Dynamical Mass Ratios of the Youngest Low-Mass Stars

Dynamical Mass Ratios of the Youngest Low-Mass Stars. Gregory Mace Mentor: Lisa Prato Northern Arizona University Physics and Astronomy. This Project. Goal: To measure mass ratios of very young binary stars. Why: To calibrate the parameters used in models of young star formation.

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Dynamical Mass Ratios of the Youngest Low-Mass Stars

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  1. Dynamical Mass Ratios of the Youngest Low-Mass Stars Gregory Mace Mentor: Lisa Prato Northern Arizona University Physics and Astronomy

  2. This Project • Goal: To measure mass ratios of very young binary stars. • Why: To calibrate the parameters used in models of young star formation. • How: High resolution IR spectroscopy of young spectroscopic binaries.

  3. Target Objects • RX J0529.3+1210 P= 462.54 days e=0.91 SpT= K7-M0 • NTTS 160814-1857 P= 144.7 days e=0.26 SpT= K2 • NTTS 155808-2219 P=16.93 days e=0.10 SpT=M3 All are pre-main sequence single-lined spectroscopic binaries.

  4. Introduction

  5. Introduction • Why infrared? • Flux Ratio Closer to Unity Reference: Web http://www.astro.helsinki.fi/~lehtinen/Work/DC303.html

  6. Observations • Data from the instrument CSHELL on the 3-meter NASA IRTF Telescope. NASA IRTF CSHELL

  7. Observations • Data from the instrument NIRSPEC on the Keck II Telescope. Keck NIRSPEC

  8. Spectral Changes NTTS 160814-1857 CSHELL NIRSPEC

  9. Spectral Changes RX J0529.3+1210 NIRSPEC

  10. Parameter Determination • Two-Dimensional Cross Correlation (Dashed line) (Solid line) Spectrum Compared to Templates

  11. Mass Ratio Determination RX J0529.3+1210 • Mass ratio: q = - slope • Center of Mass Velocity:  = (y-intercept)/(1+q) O. C. Wilson (1941)

  12. Results • RX J0529.3+1210 q= 0.93 ± 0.13 = 16.74 ± 1.69 km/s periastron  0.12 AU apastron  2.56 AU • NTTS 160814-1857 Mass ratio and center of mass velocity to be determined. • NTTS 155808-2219 Mass ratio and center of mass velocity to be determined.

  13. Results

  14. Future Research RX J0529.3+1210 • Future work: • Observe RX J0529.3+1210 • Complete mass ratios for NTTS stars

  15. Conclusions • The mass ratio of RX J0529.3+1210 is near unity. • RX J0529.3+1210 is the most eccentric pre-main-sequence spectroscopic binary know. • RX J0529.3+1210 has 24m excess which my be evidence of a circumbinary debris disk. • Planet formation in RX J0529.3+1210 is unlikely. • Comparison of templates supports likelihood of lower mass ratios for NTTS stars.

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