Monitoring the X-ray Emission of the Newly Erupted EXor-type V1118 Ori

Details Monitoring the X-ray Emission of the Newly Erupted EXor-type V1118 Ori Monitoring the X-ray Emission of the Newly Erupted EXor-type V1118 Ori

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004cxo..prop.1855a&link_type=abstract

Chandra Proposal ID #06208199

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Chandra Proposal Id #06208199

Scientific paper

The origin of the X-ray emission in young, accreting stars remains a mystery. Accretion seems the dominant mechanism in TW Hya (cool plasma; high densities). However, other moderately accreting classical T Tauri stars show high temperatures and low densities. Eruptive young stars (FUors and EXors) are the key to understanding the importance of accretion for X-rays since they suddenly display increased accretion rates from 1E-7 to 1E-4 Msol/year. FUors display brighter and longer outbursts than EXors but they are far less frequent. Recently, the (FUor-type) V1647 Ori erupted and triggered an international observation campaign. In X-rays, Kastner et al. (2004) reported a 30-fold flux increase from the pre-outburst flux, indicating that the high-energy emission in young stars can increase dramatically due to the rapid increase of accretion rates in FUor/EXor outbursts. However, the flux rapidly dropped in the steady high state.

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