Modeling Period Distribution of T Tauri Stars

Details Modeling Period Distribution of T Tauri Stars Modeling Period Distribution of T Tauri Stars

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...205.1603y&link_type=abstract

American Astronomical Society Meeting 205, #16.03; Bulletin of the American Astronomical Society, Vol. 36, p.1363

Astronomy and Astrophysics

Astronomy

Scientific paper

Observations of low-mass T Tauri stars in the Orion Nebula Cluster have shown evidence for a bimodal distribution. Stars with M > 0.25 M&sun; exhibit a population peak at rotational period of order 8 days, while lower mass stars do not. Magnetic locking between the star and the circumstellar disk has been proposed as an explanation for the peak in the distribution of higher mass stars. To test this hypothesis, we examined a steady-state accretion model, in which the torques on a T Tauri star (from accretion, stellar wind, and magnetic disk braking) balance to produce the 8-day rotation period. We explored a range of plausible values for the accretion rate, ˙ {M}, and magnetic field strengths, B, for stars with M < 0.5 M&sun;. Our preliminary results indicate that a steady-state model with ˙ {M} ˜ 10-7}-10{-8 M&sun;/yr and B ˜ 0.5-1 kG (values typically quoted in the literature) can not explain the observed period distribution of T Tauri stars.
This work was supported by the Beckman award from Harvey Mudd College.

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