Dayside chorus waves at high L-shells: Conjugate observations of PENGUIn/AGO and THEMIS

Details Dayside chorus waves at high L-shells: Conjugate observations of PENGUIn/AGO and THEMIS Dayside chorus waves at high L-shells: Conjugate observations of PENGUIn/AGO and THEMIS

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm11b1705m&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM11B-1705

Physics

[2487] Ionosphere / Wave Propagation, [2720] Magnetospheric Physics / Energetic Particles: Trapped, [2753] Magnetospheric Physics / Numerical Modeling, [2772] Magnetospheric Physics / Plasma Waves And Instabilities

Scientific paper

We study chorus waves on the dayside at high L-shells (L>7), using ground-based VLF observations at automated geophysical observatories (AGO) in Antarctica in the PENGUIn project, in-situ field and plasma observations by THEMIS, and 3D electron-tracing simulation. The goal of this study is to identify where in magnetic latitudes and radial distances the dayside and high L-shell chorus waves can be preferably generated. In this poster, we present dayside conjugate observations at AGO and THEMIS on 26 July 2008. The VLF receiver at the AGO P2 station (AP2: MLAT = -76.6 deg.) detected the intensification of VLF signals at the frequency range of 0.5-1.0 kHz between ~1400 and ~1700 UT. At the AGO P3 station (AP3: MLAT = -83.63 deg.), VLF signals increased at the 0.5-1.0 kHz frequency range between ~1400 and ~1800 UT; the increased rate was smaller than at AP2. The fluxgate magnetometer data confirmed that AP2 and AP3 were equator-ward of the open-closed boundary. During these intervals, THEMIS A, D, and E traveled in an outbound path at L = 7-10 and MLT = 11.5-13h. Both THEMIS A and D were magnetically conjugated to AP2 between ~1600 and ~1700 UT and to AP3 between ~1430 and ~1530 UT. THEMIS E was conjugated to AP2 between ~1530 and ~1630 UT. Specifically, the THEMIS A and D trajectories were magnetically connected to the estimated VLF viewing area of AP2 and AP3; the THEMIS E trajectory was connected to the viewing area of AP2. The viewing area is defined as a 500 km circle around a station. THEMIS A registered wave intensification in the 287-1240 Hz band from ~1330 to ~1600 UT. For the same frequency band, THEMIS D and E also observed intensification from ~1230 to ~1530 UT and from ~1430 to ~1630 UT, respectively. After we estimate important resonant energies of observed chorus waves from the THEMIS observations, we simulate motion of electrons with the energies in a realistic 3D magnetic field model (TS04) and a global convection electric field. We then calculate the rate of linear wave growth for the observed wave frequencies inside the L-shells for which the AGO-THEMIS conjugate observations were available. The calculation enables us to examine how the chorus growth rate is distributed along the field line and how drift-shell splitting affects the distribution.

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