Voyager 1/UVS data and model computations of the interplanetary Lyman alpha background in the outer heliosphere: 1993 to 2002.

Details Voyager 1/UVS data and model computations of the interplanetary Lyman alpha background in the outer heliosphere: 1993 to 2002. Voyager 1/UVS data and model computations of the interplanetary Lyman alpha background in the outer heliosphere: 1993 to 2002.

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh21a0486q&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH21A-0486

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Computation

2124 Heliopause And Solar Wind Termination, 2144 Interstellar Gas, 2151 Neutral Particles, 2162 Solar Cycle Variations (7536)

Scientific paper

The analysis of the latest Voyager 1 scans from mid-1998 to mid-2002 has shown a steep increase of the Lyman alpha background in all the observed directions. It is likely that this increase is linked to the 11-year solar cycle flux variation. Yet the increase obtained from the Voyager 1 UVS data is larger than the increase obtained by the direct measurements of the solar Lyman alpha flux obtained by UARS/SOLSTICE. Comparison with the measurements of the SWAN/SOHO instrument at 1 AU from the sun during the same period of time gives an indication on how the solar Lyman alpha flux at line center has actually changed. This study is essential to correctly derive the actual upwind Lyman alpha intensity gradient seen by UVS/Voyager 1. In this study we show comparisons of the interplanetary Lyman alpha background data obtained by UVS/Voyager 1 in the outer heliosphere and corrected for solar flux variations with a model of the Lyman alpha background emission in the outer heliosphere based on hydrogen distributions derived from a model describing the effects of the heliospheric interface. In this presentation, we will show how intensity gradients in the upwind direction are modified by the effects of the heliospheric interface on the hydrogen atoms. Although no data are available on lineshifts (apparent velocity) and linewidths (apparent temperature) in the outer heliosphere, we show model computations of these parameters and how they change as the heliosphere interface gets closer to the spacecraft.

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