ROSAT-IUE observations of symbiotic stars. The X ray morphology of high latitude associations

Details ROSAT-IUE observations of symbiotic stars. The X ray morphology of high latitude associations ROSAT-IUE observations of symbiotic stars. The X ray morphology of high latitude associations

Oct 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993colo.reptq....s&link_type=abstract

Final Report Colorado Univ., Boulder.

Astronomy and Astrophysics

Astronomy

Iue, Molecular Clouds, Rosat Mission, Star Formation, Stellar Evolution, Stellar Mass Accretion, Stellar Systems, Symbiotic Stars, X Ray Astronomy, Accretion Disks, B Stars, Massive Stars, O Stars, Supernova Remnants, T Tauri Stars

Scientific paper

The purposes of this grant included: to provide for continuing investigations of the x-ray properties of a class of interacting binaries known as symbiotic stars through analysis of their detection statistics in the ROSAT All-Sky Survey and simultaneous IUE observations; and to obtain and analyze ROSAT images of selected high latitude OB star associations, in order to permit multi-wavelength dissection of their contents and energetics. The first study is expected to result in enhanced information on mass transfer and accretion in such systems, and provide a more quantitative basis for interpretation of the spectra of these and similar stellar and extragalactic systems. This particular effort represents NASA support for an approved collaboration between the PI and the ROSAT Team at MPE Garching. In the second study, we seek to correlate the strength with which the diffuse clouds have been shocked and the recent star formation triggered, namely, the O and B stars of the Association, as well as nearby T Tauri stars. The large scale X-ray emission in deep ROSAT PSPC images will be compared with the optical, infrared, and radio topology of nearby supernova remnants, molecular clouds, and the distribution of massive stars in the regions. This should enable us to test whether the star formation triggering shocks originate from in the galactic plane (nearby supernovae) or from the collision of infalling matter with the disk material (galactic fountain dynamics).

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