EDP Sciences
Free access
Issue
A&A
Volume 426, Number 3, November II 2004
Page(s) 885 - 895
Section Interstellar and circumstellar matter
DOI http://dx.doi.org/10.1051/0004-6361:20047147


A&A 426, 885-895 (2004)
DOI: 10.1051/0004-6361:20047147

Heliospheric conditions that affect the interstellar gas inside the heliosphere

D. R. McMullin1, M. Bzowski2, E. Möbius3, A. Pauluhn4, R. Skoug5, W. T. Thompson6, M. Witte7, R. von Steiger4, D. Rucinski2, D. Judge8, M. Banaszkiewicz2 and R. Lallement9

1  Space Sciences Center, University of Southern California, Los Angeles, CA 90089, USA Praxis, Inc., Alexandria, VA, USA
    e-mail: mcmullind@pxi.com
2  Space Research Centre PAS, Bratycka 18A, 00-716 Warsaw, Poland
3  Space Science Center and Department of Physics, University of New Hampshire, Durham, NH 03824, USA
4  International Space Science Institute, 3012 Bern, Switzerland
5  Los Alamos National Laboratory, Los Alamos, NM 87545, USA
6  Goddard Space Flight Center, Greenbelt, MD 20771, USA
7  Max-Planck-Institut für Aeronomie, 37191 Katlenburg-Lindau, Germany
8  Space Sciences Center, University of Southern California, Los Angeles, CA 90089, USA
9  Service d'Aéronomie du CNRS, BP 3, 91371, Verrières-le-Buisson, France

(Received 26 January 2004 / Accepted 23 June 2004 )

Abstract
The interstellar gas that flows through the heliosphere is strongly affected by ionization close to the Sun, in particular solar photoionization, electron impact, and charge exchange. Therefore, the interpretation of any observation of interstellar gas in the inner heliosphere hinges upon the accurate knowledge of these effects and their variations. In addition, the irradiance and line profile of the relevant solar spectral line are needed to properly interpret resonant backscattering observations of the interstellar neutral gas. With instrumentation on ACE, SOHO and Wind, continuous monitoring of these important environmental conditions simultaneously with a multitude of interstellar gas observations has become possible for the first time. In this paper we present a compilation of the processes and parameters that affect the distribution of interstellar helium inside the heliosphere and their observation, including the irradiance and line profile of the He 58.4 nm line. We also make the connection to proxies for these parameters and evaluate their accuracy in order to expand the time period of coverage wherever possible.


Key words: ISM: general -- ISM: atoms -- interplanetary medium -- plasmas




© ESO 2004

What is OpenURL?

The OpenURL standard is a protocol for transmission of metadata describing the resource that you wish to access.

An OpenURL link contains article metadata and directs it to the OpenURL server of your choice. The OpenURL server can provide access to the resource and also offer complementary services (specific search engine, export of references...). The OpenURL link can be generated by different means.

  • If your librarian has set up your subscription with an OpenURL resolver, OpenURL links appear automatically on the abstract pages.
  • You can define your own OpenURL resolver with your EDPS Account.
    In this case your choice will be given priority over that of your library.
  • You can use an add-on for your browser (Firefox or I.E.) to display OpenURL links on a page (see http://www.openly.com/openurlref/). You should disable this module if you wish to use the OpenURL server that you or your library have defined.