Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.276l..51z&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 276, Issue 4, pp. L51-L54.
Astronomy and Astrophysics
Astronomy
1
Shock Waves, Binaries: Close, Stars: Mass-Loss, Stars: Pre-Main-Sequence, Infrared: Stars
Scientific paper
We present model calculations of the infrared coronal-line emission that arises from colliding supersonic winds in pre-main-sequence binary stars. For typical wind velocities between 300 and 500 km s^-1, the interaction region has a temperature range well suited for coronal lines to attain peak emissivities. Infrared spectral-line observations at wavelengths <~1 μm can provide a unique opportunity to probe the physical conditions of the gas flows in these systems. We derive simple scaling laws that allow us to estimate the coronal-line fluxes as a function of the model parameters and compare the results with those obtained for the X-ray emission. The advantage of using coronal lines instead of X-rays to test the colliding winds paradigm is the greatly reduced absorption at infrared wavelengths. Finally, we discuss the possibility of detecting the most intense lines from known binary systems.
Palla Francesco
Prusti Timo
Zhekov Svetozar A.
No associations
LandOfFree
Infrared coronal-line emission from pre-main-sequence binaries: testing the colliding winds model does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Infrared coronal-line emission from pre-main-sequence binaries: testing the colliding winds model, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Infrared coronal-line emission from pre-main-sequence binaries: testing the colliding winds model will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1355661