Emission of whistler-mode waves and diffusion of electrons around interplanetary shocks

Journal Article · Mon Jul 01 04:00:00 EDT 1996 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.51475· OSTI ID:574658

Pierre, F; Solomon, J ^[1]; Cornilleau-Wehrlin, N; Canu, P ^[2]; Scime, E E ^[3]; Phillips, J L ^[4]; Balogh, A; Forsyth, R J ^[5]

---

1. IAS/CNRS/Univ. Paris 11, Orsay (France)
2. CETP/CNRS, Velizy (France)
3. Physics Dpt., West Virginia University, Morgantown, West Virginia (United States of America)
4. Los Alamos National Laboratory, Los Alamos, New Mexico (United States of America)
5. Imperial College of Science and Technology, London (England)

We present a study of whistler-mode wave generation and wave particle interaction in the vicinity of interplanetary shocks in the ecliptic plane, as observed by the Ulysses spacecraft. Generally the whistler-mode waves (measured in the frequency range 0.22{endash}448 Hz) are observed downstream of the shocks where they persist for some hours. From the electron distribution functions (EDF) in the energy range 1.6 to 862 eV, we compute the temperature anisotropy and the wave growth rate of the electromagnetic electron cyclotron instability for the case of parallel propagation of the waves with respect to the interplanetary magnetic field (IMF) {bold B}. In general, in agreement with the wave measurements, the instability grows only downstream of the shock fronts. Following the wave activity, velocity space diffusion of the electrons results in a marginally stable state with sporadic fluctuations. {copyright} {ital 1996 American Institute of Physics.}

• OSTI ID: 574658
• Report Number(s): CONF-9506256--
• Journal Information: AIP Conference Proceedings, Journal Name: AIP Conference Proceedings Journal Issue: 1 Vol. 382; ISSN 0094-243X; ISSN APCPCS
• Country of Publication: United States
• Language: English

Related Subjects

66 PHYSICS
DIFFUSION
DISTRIBUTION FUNCTIONS
ELECTRONS
INSTABILITY GROWTH RATES
INTERPLANETARY SPACE
SHOCK WAVES
SOLAR WIND
WHISTLER INSTABILITY