On the origin of X-ray emission from Herbig Ae/Be stars

Details On the origin of X-ray emission from Herbig Ae/Be stars On the origin of X-ray emission from Herbig Ae/Be stars

Sep 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005cxo..prop.1878s&link_type=abstract

Chandra Proposal ID #07200005

Computer Science

Chandra Proposal Id #07200005

Scientific paper

Intermediate-mass pre-main sequence stars (=HAeBe stars) evolve along fully radiative tracks and are not expected to sustain a dynamo. Consequently - in contrast to the T Tauri stars - HAeBe stars are not expected to display phenomena related to magnetic activity such as X-ray emission. Nevertheless, many X-ray observatories have detected HAeBe stars. Possibly the observed X-ray emission must be attributed to T Tauri like companions. This is the most wide-spread explanation for X-rays from main-sequence A and B stars. But the hypothesis has never been tested for HAeBe stars. We propose for X-ray imaging of 6 HAeBe stars with recently discovered cool companions resolvable with Chandra covering a wide range in the HR diagram, and will put very stringent limits to their X-ray luminosity.

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