Magnetic Reconnection Events as Contributors to T Tauri Angular Momentum Evolution

Details Magnetic Reconnection Events as Contributors to T Tauri Angular Momentum Evolution Magnetic Reconnection Events as Contributors to T Tauri Angular Momentum Evolution

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.6218a&link_type=abstract

American Astronomical Society, AAS Meeting #211, #62.18; Bulletin of the American Astronomical Society, Vol. 39, p.850

Astronomy and Astrophysics

Astronomy

Scientific paper

The Chandra Orion Ultradeep Project observed hundreds of T Tauri stars undergoing highly energetic X-ray flare events. Favata et al. (2005) applied a standard solar uniform cooling loop model to the 30 strongest flares and derived very large loop lengths on the order of tens of stellar radii. Do these large loops represent magnetospheric accretion structures or, using a solar analogue, do they represent extreme "coronal mass ejections" (CMEs)? We have modeled the spectral energy distributions of this sample and find that the majority lack circumstellar disk material: these are weak-lined T Tauri stars with extremely large flares. This surprising result is the impetus for detailed analysis of the mass and angular momentum shed during events of this magnitude. We present estimates of angular momentum loss via CMEs expected to result from large scale flare events and discuss the implications of this work for stellar angular momentum evolution of young low-mass stars. We also present work in progress to model a wider distribution of reconnection event energies and place the results into context with observations.

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