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Astron. Astrophys. 336, L45-L48 (1998)
Letter to the Editor
Heliopause radio emission scenario
R.A. Treumann 1, 2,
W.M. Macek 1, 3 and
V. Izmodenov 1
1 International Space Science Institute, Bern,
Switzerland
2 Max-Planck-Institute for Extraterrestrial Physics,
Garching, Germany
3 Space Research Center, Polish Academy of Sciences,
Warsaw, Poland
Received 27 March 1998 / Accepted 8 July 1998
Abstract
Heliospheric (HSP) radio emission detected by the Voyager
spacecraft between 1.8 kHz and 3.6 kHz from the distant heliosphere is
interpreted as emission generated close to and at the heliopause (HP),
the interface between the ionised very local interstellar (LIC) gas
and the supersonic solar wind (SW) stream. Radio emission is assumed
to be triggered by secondary charge exchange ionisation of
interstellar neutrals and subsequent generation of lower hybrid (LH)
waves. These waves nonlinearly accelerate electrons into beams along
the spiral compressed heliosheath (HS) magnetic field
![[FORMULA]](img1.gif)
. Langmuir waves locally generated by these beams
may be responsible for the observed emission. Under quiet conditions
the emission is at marginally high frequency for observation. Under
disturbed conditions the plasma density may be high enough to explain
the Voyager observations. In this mechanism
plays a crucial role.
Key words: distant
heliosphere 
heliopause and termination
shock
radio emission mechanism
Send offprint requests to: R.A. Treumann (e-mail: tre@mpe.mpg.de)
This article contains no SIMBAD objects.
Contents
- 1. Introduction
- 2. Properties of the heliopause
- 3. Electron beam formation
- 4. Radiation
- 5. Discussion
- Acknowledgements
- References
© European Southern Observatory (ESO) 1998
Online publication: July 27, 1998
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