Mode Conversion of Gaussian Light Beams Propagating Through a Random Medium

Imai, Masaaki; Kikuchi, Shoichi; Matsumoto, Tadashi

doi:10.1029/rs005i007p01009

Cited by 2 publications

(1 citation statement)

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“…In the SELENE mission, the VLBI observation (Iwata et al 2001) used the VLBI Exploration of Radio Astronomy (VERA) network, which consisted of four Japanese telescopes located at Mizusawa (MZ), Iriki (IR), Ishigaki (IS) and Ogasawara (OG) (Kobayashi et al 2003), and used four additional international telescopes located in Urumqi (UR, China), Shanghai (SH, China), Wettzell (WZ, Germany) and Hobart (HO, Australia) (Schlüter et al 2002). The baselines ranged from 796 km (SH-IS) to 12 247 km (HO-WZ) (Liu et al 2010) Both subsatellites had the shape of an octagonal prism with size 1 m × 1 m × 0.65 m. They were covered by solar panels on all sides and weighed approximately 45 kg. Both were also spinstabilized.…”

Section: Setting Up the Experimentsmentioning

confidence: 99%

Electron content near the lunar surface using dual-frequency VLBI tracking data in a single lunar orbiter mission

Wang

Ping

2015

Res. Astron. Astrophys.

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In VLBI observations of Vstar, a subsatellite of the Japanese lunar mission SELENE, there were opportunities for lunar grazing occultation when Vstar was very close to the limb of the Moon. This kind of chance made it possible to probe the thin plasma layer above the Moon's surface as a meaningful by-product of VLBI, by using the radio occultation method with coherent radio waves from the S/X bands. The dual-frequency measurements were carried out at Earth-based VLBI stations. In the line-of-sight direction between the satellite and the ground-based tracking station where VLBI measurements were made, the effects of the terrestrial ionosphere, interplanetary plasma and the thin lunar ionosphere mixed together in the combined observables of dual-frequency Doppler shift and phase shift. To separate the variation of the ionospheric total electron content (TEC) near the surface of the Moon from the mixed signal, the influences of the terrestrial ionosphere and interplanetary plasma have been removed by using an extrapolation method based on a short-term trend. The lunar TEC is estimated from the dual-frequency observation for Vstar from UT 22:18 to UT 22:20 on 2008 June 28 at several tracking stations. The TEC results obtained from VLBI sites are identical, however, they are not as remarkable as the result obtained at the Usuda deep space tracking station.

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Section: Setting Up the Experimentsmentioning

confidence: 99%