Solar UV Backscattering Observations of the Neutral Local Interstellar Medium

Details Solar UV Backscattering Observations of the Neutral Local Interstellar Medium Solar UV Backscattering Observations of the Neutral Local Interstellar Medium

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh32c..02v&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH32C-02

Physics

7549 Ultraviolet Emissions, 2124 Heliopause And Solar Wind Termination, 2144 Interstellar Gas, 2151 Neutral Particles

Scientific paper

Most of the neutral gas flowing inside the heliosphere (>99%) is interstellar in origin and has been observed remotely by its resonance scattering of solar Lyman alpha radiation of both hydrogen (121.6 nm) and helium (58.6 nm) using UV sensitive instruments on EUVE, Prognoz, and SOHO (SWAN). In deriving LISM parameters from backscatter measurements, the solar flux distribution in both time, space and wavelength becomes the key limiting factor in the accuracy of the results. Hence the importance of the multi-satellite campaign of 1999-2000 where an assortment of spacecraft (SOHO, ACE, and Ulysses) observed the He wind, both in-situ and remotely. I will review the UV backscatter measurements and how they constrain LISM parameters such as temperature, velocity vector, and neutral density and compare them to those determined from the ``Local Cloud'' using high resolution UV absorption lines. In particular, the EUVE measurements of neutral helium over the period of 1992-2000 have a very high signal to noise ratio ( ~ 30:1 in 2 seconds) and show long term variability which is most likely solar in origin but intriguing if interstellar.

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