Radio Atmospheric Science Center, Kyoto University
This page shows the radar and optical observation
of the mesopause region during the Leonid meteor
stream activity in November 1998, using the
instruments of Japanese PSMOS(Planetary Scale Mesopause
Observing System) group.
MU radar data (Houly Rate),
MU radar data (Time-range plot),
What to observe?
Atmospheric dynamics around the mesopause
Atmospheric waves such as gravity waves, tides, and planetary
waves, and their interactions, propagations will be studied
by the coordinated radar and optical measurements.
Leonid meteor activity
The forthcoming outburst of the leonid meteor stream
will be monitored with the MU radar, the most sensitive "meteor radar"
in the world to detect ionized meteor trails.
The same observation parameter has been used
from 1990 every year for leonids. A new technique to observe
meteor head echo will also applied during the observation this year.
Effects of the severe meteor outburst on the atmosphere
If there should be a severe meteor storm such as observed 32
years ago in USA, a significant amount of meteoriods would be
scattered around the mesopause. Variations of the atmosphere,
especially the minor consituents are monitored with active
and passive optical remote sensing.
Shigaraki (34.9N, 136.1E)
MU radar (RASC, Kyoto Univ.:T.Tsuda, T.Nakamura)
Nov. 13, 21:00 -- Nov.22 10:00 JST(UT+9)
Meteor mode operation (meteor trail number, wind velocity
and temperature fluctuation at 80-100km height)
NOTE: on Nov. 17/18 meteor head echo mode will be
operated for 15 minutes every hour (T.Sato).
OMTI(STE lab., Nagoya University:T.Ogawa, K.Shiokawa)
Airglow intensity, wind and temperature around the mesopause
(87km - 97km) will be observed
All sky imager-1: OI(558nm) and NaD (589nm) airglow image
All sky imager-2: O2() and OH (Meinel-band) airglow image
FPI (Fabry Perot Interferometer): OI(558nm) wind
SATI (Spectral Airglow Temperature Imager): OH and O2 rotational
NOTE: Meteor and train images will be recorded by All sky imagers.
Sodium Lidar (Shinshu Univ.:A.Nomura)
Nov. 13 -- Nov.22
Atomic sodium (Na) density at 85 - 105 km will be observed.
NIR(1.2um) Photometer (Rikkyo Univ.:H.Yamamoto)
Nov. 16 - 19
O2, OH airglow intensity; OH rotational temperature.
OH-imager (RASC, Kyoto Univ.:T.Tsuda, T.Nakamura)
OH airglow image (87km) every 3 minutes.
Amateur meteor researchers will operate video camera with I.I.
around the expected maximum (Nov.15-19) (M.Ueda et al.).
Sodium lidar will be operated (Tokyo Metrop. Univ.:C.Nagasawa, M.Abo)
Zao (38.1N, 140.6E)
Tohoku University (H.Fukunishi, Y.Takahashi, T.Sakanoi)
will operate very fast photomultiplier
array to observe light curve of meteor luminosity.
OH(Meinel band)/OI(558nm) all sky imager
FPI(558nm) (neutral wind at 97km)
Routine observation of airglow intensity will be carried out by
Niigata University (Y.Kiyama).
Yamagawa(31.2N, 130.6E), Wakkanai(45.4N,141.8E)
Continuous operation (radar), Nov. 16-20 (Optical)
MF radars are operated continuously at these sites by CRL
(Communications Res. Lab.:K.Igarashi), which observed winds at 70-100km.
Optical observations are also planned at Wakkanai:
an OH all-sky imager (OH intensity) and a CCD camera for meteor
QUICKLOOK of the observational data
Hourly meteor echo rate by the MU radar
Hourly meteor echo rate will be reported here every hour on Nov. 17/18,
and every 6 hours for the rest of the observation period.
Time-range cross section of the radar echo
Meteor echo distribution in time and range is reported.
PSMOS of SCOSTEP
PSMOS/JAPAN hope page
Radar Group of RASC (Radio Atmospheric Science Center), Kyoto Univ.
updated on November 17, 1998.