A(nother) Star is Born: the Early Evolution of a Pre-main Sequence Accretion Burst

Astronomy and Astrophysics – Astrophysics

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Chandra Proposal Id #07208258

Scientific paper

Accretion processes produce X-ray emission in a wide variety of astrophysical environments, yet the link between pre-main sequence (PMS) star accretion and X-ray emission remains tenuous at best. Undoubtedly the most convincing example of accretion-driven PMS X-ray emission is that of V1647 Ori; Chandra observations obtained over the (two-year) duration of the optical/IR outburst of this PMS star revealed that its X-ray flux and hardness closely tracked the dramatic rise and subsequent decline of its accretion luminosity (Kastner et al. 2004, Nature, 430, 429 and 2006, ApJ, 648, L43). These results for V1647 Ori suggest that X-ray emission from erupting low-mass, PMS stars is diagnostic of the degree of star-disk magnetic field reorganization during major ("FUor"- or "EXor"-type) accretion events. Prompt post-outburst observations of additional erupting PMS stars are required to test this hypothesis.

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