Interstellar Material towards the Nearby High Latitude Star eta UMa

Details Interstellar Material towards the Nearby High Latitude Star eta UMa Interstellar Material towards the Nearby High Latitude Star eta UMa

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.1721f&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #17.21; Bulletin of the American Astronomical Society, V

Astronomy and Astrophysics

Astronomy

2

Scientific paper

The rapidly rotating B3 V high latitude star eta UMa (31 pc) samples a typical sightline through the flow of ISM enveloping the Sun. We combine optical, HST GHRS, IMAPS, Copernicus and IUE data to synthesize a fairly complete portrait of the ISM in this direction. Together, these data provide data on HI, DI, CII, CII*, CIV, NI, NII, OI, PII, MgII, MgI, SiII, ArI, CaII, SII, FeII, and ZnII. Two interstellar components are seen. We use theoretical models of the eta UMa atmosphere to extract accurate information on the interstellar HI Lya line. A broad low column density redshifted HI Lya absorption feature is found at the velocity expected for charge exchange between the solar wind and interstellar HI inside of the solar system. This detection constitutes the discovery of a energetic neutral atom charge-exchange component (or `neutral solar wind') formed by interstellar HI and the solar wind, and should provide an important constraint on models of heliospheric X-ray emission. A broad blue-shifted component appears to be due to mass loss from eta UMa. For a cloud temperature comparable to the temperature of the cloud surrounding the Sun (6400 K), we find that n(e) 0.1 /cc. For a nominal 50% ionization (NI NII), N(HI) yields a cloud thickness of 3 pc.
The authors thank NASA for supporting this research.

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