Defining Pre-Outburst and Post-Outburst Characteristics of Eruptive Young Stars

Details Defining Pre-Outburst and Post-Outburst Characteristics of Eruptive Young Stars Defining Pre-Outburst and Post-Outburst Characteristics of Eruptive Young Stars

Oct 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005xmm..prop..236s&link_type=abstract

XMM-Newton Proposal ID #04065707

Physics

Stars, White Dwarfs, Solar System, Ex Lup, Vy Tau, Hbc 366, V1143 Ori, V350 Cep, Pv Cep, Dr Tau, Xmm-Newton Proposal 04065707

Scientific paper

EXORs are extreme T Tauri stars that experience major UV-optical eruptions (3-5 mag) that last about a year. These recurring outbursts driven by high accretion rates assist in dispersal of the circumstellar disk and the large X-ray-UV flux injected into the local environment modifies the physical and chemical history, influencing planet formation and time scales. Little X-ray data exists on these stars during either quiescent or outburst phases, so basic details such as how much X-ray flux is produced during eruption is unknown. We will characterize the X-ray properties of 7 EXORs in their quiescent phase. TOO time is requested to obtain high-quality spectra if an eruption occurs during AO5. Contrasting quiescent and outburst properties provides crucial insight into the physics.

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