Transcript V. Morozenko, Night Atmosphere Radiation in

Night Atmosphere Radiation in 240-400 and
600-800 nm Wavelengths Ranges, Measured by
“Universitetsky-Tatiana-2” Satellite
G.K. Garipov1, B.A. Khrenov1, P.A. Klimov1, V.S. Morozenko1, M.I.
Panasyuk1, V.I. Tulupov1, V.M. Shahparonov1, S.A. Sharakin1, S.I.
Svertilov1, N.N. Vedenkin1, I.V. Yashin1, H.I Salazar2, O.B. Martinez2,
E.L. Ponce2, J.P. Cotsomi2, I.H. Park3.
1-D.V. Skobeltsyn Institute of Nuclear Physics, Moscow State University, Russia.
2-University of Puebla (BUAP), Puebla, Mexico.
3-Research Center of MEMS Space Telescope, Ewha Womans University, Seoul,
Korea.
September 6-11, 2010
Nor Amberd, Armenia
“Universitetsky-Tatiana-2”
scientific payload
(launched on September 17, 2009 to orbit of 830 km height and
98.8˚ inclination)
Detector of UV (240-400 nm) and RedIR radiation (600-800 nm).
Electron flux detector of area 400 cm2
UV and Red-IR
detector:
1-entrance collimators,
2- PMT for UV,
3-PMT for Red,
4-electronics.
CP (charged particle)
detector:
1- scintillation plate,
2- light guide-convertor,
3- PM tube.
“Digital oscilloscope” time sample is 1 ms
Oscilloscope race duration is 128 ms. Event selection integration time is
1 ms. The brightest event in 1 minute is finally recorded.
Universitetsky-Tatiana-2 night atmosphere UV
radiation monitoring data
At moonless nights the darkest
places on Earth in UV light are
Sahara desert, Siberia, Southern
regions of Pacific and Atlantic
oceans (UV intensity 3-5 107 ph/cm2
s sr).
The brightest are the aurora oval
regions (UV intensity up to 2 109
ph/cm2 s sr – “Tatiana-1” data) and
regions above large cities or
industrial regions (up to 1-2 108
ph/cm2 s sr).
Those data are important for
planning the Extreme Energy
Cosmic Ray measurements from
Satellites.
Night cities lights
Universitetsky-Tatiana-2 night atmosphere IR
radiation monitoring data
• The industrial regions are also well seen in IR wavelength.
• The enhancement of measured intensity is observed in the South
Atlantic Anomaly region. Probably it is connected with light, produced by
charged particles in detector (filter, entrance PMT window)
Universitetsky-Tatiana-2 charge particles monitoring data
• CP detector is designed for measurements of msec pulses. It is
not sensitive to average low flux of charged particles. On the world
map, obtained by “Tatiana-2” satellite only the particle flux at
South Atlantic Anomaly is clearly seen (> 102 el/cm2 s).
• In aurora regions the particle flux is near detector sensitivity
threshold.
•There is no signals of charged particles synchronous to UV flashes.
World maps of UV flash events.
Flashes classification based on temporal profile features.
Class
1
2
3
4
Number of flashes, %
26
31
33
10
Serials of flashes
UV-R-IR detector frequently measured serials of flashes
along the night orbit . Number of flashes (N) in serial
varied from 3 to 11 (one flash per minute). In 1 months
56 serials were recorded. Most of serials were observed
above land.
Flashes in one serial are of various types
N
3
4
5
6
7
11
Above land
13
14
4
-
2
1
Above ocean
6
1
1
-
-
-
Above coast
6
4
1
3
-
-
Serials of flashes and the geomagnetic equator. Part of serials
is symmetrical to equator and could be related to electrons
trapped by geomagnetic field. The Southern Hemisphere
latitudes >30o are at the day side. Sahara is evidently region
restricted to flash events.
Serials of flashes and clouds.
Many flashes occurs above clouds and can be related to
thunderstorms, but frequently there are no clouds under measured
flashes. Pictures above show two such event examples.
Further statistical analysis of all events will be done.
Conclusions
1.
2.
3.
4.
5.
The detailed map of UV average intensity is obtained by “Tatiana-2” data.
This map is important for planning orbital high energy cosmic rays
measurements.
Map of charge particles signal was also obtained. Measurements of CP
flux in SAA have shown that charge particle detector works properly. The
CP signal synchronous to UV flashes was not detected .
Measured flashes have various temporal profiles. Two types of flashes: 1)
events with clear structure of short (1-3 ms) pulses and events with
longer structure are separated as different in energy release to UV
photons and different in world distribution.
The serials of flashes are measured with number of flashes within one
serial (number of flashes in one serial: from 3 to 11). Serial contain flashes
of various types and occur more frequently above land.
There are flashes not connected with lightning (no clouds under the flash).
The origin of those flashes is under analysis.