This article has an erratum: [https://doi.org/10.1051/0004-6361/20079241e]
Volume 491, Number 1, November III 2008
Diagnostics of interstellar hydrogen in the heliosphere
|Page(s)||29 - 41|
|Published online||18 August 2008|
UV optical measurements of the Nozomi spacecraft interpreted with a two-component LIC-flow model
Department of Geophysics, University of Tohoku, Sendai, Japan e-mail: email@example.com
2 Space Research Centre PAS, Bartycka 18A, 00-716 Warsaw, Poland e-mail: firstname.lastname@example.org
3 Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
4 Japan Society for the Promotion of Science, Beijing, PR China
5 Department of Earth and Planetary Science, University of Hokkaido, Japan
6 Department of Physics, College of Science, Rikkyo University, Tokyo, Japan
7 Department of Earth and Planetary Science, University of Tokyo, Tokyo, Japan
8 Earth Observation Research Center, Japan Aerospace Exploration Agency, Tsukuba, Japan
Accepted: 8 July 2008
Aims. Following recent reports on spectroscopic observations by SWAN/SOHO suggesting that the flows of neutral interstellar helium and hydrogen in the inner heliosphere are slightly divergent, we tried to verify them on the basis of simultaneous photometric observations of heliospheric hydrogen and helium glows performed by a spacecraft located on an orbit between the Earth and Mars (which differs from the orbit of SWAN/SOHO). The observations were interpreted with the use of various independent models of interstellar hydrogen and helium in the inner heliosphere, evaluated over a mesh of parameters.
Methods. The data might suggest that the upwind and downwind directions of interstellar H may differ by less than 180°, which we interpret as due to a side shift of the secondary population of interstellar hydrogen, which might be due to a deformation of the outer heliosheath e.g. because of the action of interstellar magnetic field. The simulations we performed do not support the idea that the secondary population is significantly shifted to the side.
Results. The upwind/downwind direction of interstellar hydrogen as derived from our observations agrees within the error bars with the upwind/downwind direction of interstellar helium and the error bars include both the upwind direction of interstellar helium, derived from in-situ observations of GAS/Ulysses, and the upwind direction of interstellar hydrogen, derived from observations of SWAN/SOHO.
Key words: Sun: UV radiation / ISM: atoms / ultraviolet: ISM
© ESO, 2008
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