X-ray Tomography of the Heliosheath

Details X-ray Tomography of the Heliosheath X-ray Tomography of the Heliosheath

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsh23a..06m&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH23A-06

Astronomy and Astrophysics

Astronomy

2124 Heliopause And Solar Wind Termination, 2126 Heliosphere/Interstellar Medium Interactions

Scientific paper

The heliosheath is glowing in X-rays due to charge-exchange collisions between solar wind ions and neutrals from the ISM. The overall appearance of the X-ray glow is determined by the interaction of the Solar wind and the local ISM. Spectral information, in turn, delivers valuable information on various parameters of the Solar wind (e.g., temperatures and densities of the minor species -- highly stripped ions) and the details of the Solar wind interaction with neutrals in the heliosheath region. Using numerical models for the heliosphere, we traced the charge-exchange evolution of 45 different solar wind ions along the wind stream-lines. The evolution from high-ionization states to low-ionization states is clearly seen, thus indicating the importance of the collisional thickness effect for the outer heliosphere composition. From charge-exchange transitions, we determine the X- ray emissivity and create surface brightness and spectral maps for any viewing direction (the outside view). The evolution of the wind ion-composition and the accompanying spectral changes across the heliosheath (from nose to tail) are remarkable and can serve as a diagnostic for the wind-ISM interaction. Chandra and XMM-Newton are well suited for this task. Similar models can be made for astrospheres of nearby Sun-like stars.

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