Astrophysics of young star binaries
Nov, 200263 pages
Published in:
- Astrophys.J. 584 (2003) 853-874
e-Print:
- astro-ph/0211376 [astro-ph]
DOI:
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Abstract: (arXiv)
This paper describes our study of the astrophysics of individual components in close pre-main-sequence binaries. We observed both stars in 17 systems, located in 4 nearby star forming regions, using low-resolution (R=760), infrared spectroscopy and photometry. For 29 components we detected photospheric absorption lines and were able to determine spectral type, extinction, K-band excess, and luminosity. The other 5 objects displayed featureless or pure emission line spectra. In ~50 % of the systems, the extinction and K-band excess of the primary stars dominate those of the secondaries. Masses and ages were determined for these 29 objects by placing them on the H-R diagram, overlaid with theoretical pre-main-sequence tracks. Most of the binaries appear to be coeval. The ages span 5x10^5 to 1x10^7 years. The derived masses range from the substellar, 0.06 M_sun, to 2.5 M_sun, and the mass ratios from M_2/M_1=0.04 to 1.0. Fourteen stars show evidence of circumstellar disks. The K-band excess is well correlated with the K-L color for stars with circumstellar material.References(75)
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