Volume 491, Number 1, November III 2008
Diagnostics of interstellar hydrogen in the heliosphere
|Page(s)||1 - 5|
|Published online||17 July 2008|
Determining the LIC H density from the solar wind slowdown
Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 37-655, Cambridge, MA 02139, USA e-mail: [liuxying;jdr]@space.mit.edu
2 State Key Laboratory of Space Weather, Center for Space Science and Applied Research, Chinese Academy of Sciences, P.O. Box 8701, Beijing 100080, PR China e-mail: email@example.com
3 Southwest Research Institute, P.O. Drawer 28510, San Antonio, TX 78228, USA e-mail: firstname.lastname@example.org
Accepted: 8 December 2007
Context. The ionized solar wind interacts directly with the interstellar neutrals which flow into the heliosphere. These neutrals are ionized, mainly by charge exchange, then accelerated to the solar wind speed with the momentum and energy removed from the bulk flow of the solar wind. Thus, by measuring the solar wind slowdown, one can estimate the interstellar neutral density.
Aims. In July 2005, Ulysses at 5 AU and Voyager 2 near 80 AU were at the same heliolatitude. We use this alignment to determine the solar wind speed decrease between these two spacecraft.
Methods. Ulysses data are used as input to a 1-D MHD model which includes the effects of pickup ions. We removed a section of data contaminated by an ICME directed toward Voyager 2.
Results. Comparison of the Voyager 2 speeds with the model results shows that the solar wind speed decreased by 67 km s-1 between Ulysses and Voyager 2, consistent with an interstellar neutral density at the termination shock of 0.09 cm-3.
Key words: solar wind / interplanetary medium
© ESO, 2008
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