Cassini UVIS Time-Series Observations of Interplanetary H Lyman-alpha Emissions

Details Cassini UVIS Time-Series Observations of Interplanetary H Lyman-alpha Emissions Cassini UVIS Time-Series Observations of Interplanetary H Lyman-alpha Emissions

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh21b0156p&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH21B-0156

Physics

7536 Solar Activity Cycle (2162), 7549 Ultraviolet Emissions, 7837 Neutral Particles

Scientific paper

The Cassini Ultraviolet Imaging Spectrograph (UVIS) has been routinely obtaining high signal-to-noise ratio measurements of interplanetary H Lyman-alpha, H Lyman-beta, and He 58.4 nm emissions during the cruise phase of its mission to Saturn. We report here on the time-series Lyman-alpha data obtained to date. These data can be compared to a model of the interstellar H flowing through the heliosphere and illuminated by the Sun. Of particular interest in these data is the presence of modulations due to the rotation of solar active regions that strongly emit Lyman-alpha radiation. We compare the observed modulations to those predicted from our model. If the observed modulations are damped compared to the model predictions, this may be evidence for multiple scattering of solar photons in the heliosphere. The amount of multiple scattering is an indicator of the heliospheric H density, a quantity that remains poorly constrained. Additional background measurements are planned for the orbital phase of the Cassini mission (2004-2008).

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