Detector of UV and IR Radiation on Board “Tatiana” and- “Tatiana-2” Satellites and Applications for Future Experiments and in Complex Detector for TLE Study at Aragats Cosmic Station” G.K . Garipov Skobeltsyn Institute of Nuclear Physics, Moscow State University, Russia Content.
Parameters of the
Mass, kg 25
Power, Wt 7
Ground track of TATIANA satellite
Parameters of the
Mass, kg 0.5
Field of view, degree ±7
Power, Wt 0.6
The scientific instruments were preparedand constructed by D.V. Skobeltsyn Instituteof Nuclear Physics.
Mass of scientific
Power, Wt 4.2
Block-diagram of the UV detector at the MSU “Tatiana” satellite
UV detector comprises 2 PMT tubes and electronics block.
(first tube measures an optical radiation, second measures the charge particle background)
Two code are recorded and used in measurements:
M- PMT gain DAC code and N- the PMT anode current ADC code
(1) collimator, (2) UV-1 filter, (3)cover, MX—multiplexor, HV—voltage supply for PM tubes,ADC and DAC—analog-digital and digital-analog convertors, Logic Unit-FPGA.
UV & blinded PMT electronics block- diagram
Gain control circuit or detector
Digital integrator and Signal finder circuit.
The ‘‘flash’’ event finding algorithm
Example of the measured oscillogram of the airglow signal on the day side,
satellite is illuminated by the Sun
ground track of the orbit
Stability of the PMT performance. Moon was used as source of calibrated light
Examples of UV intensity and AURORA and near equatorial ovals recording on – route at South latitudes in moonless night in two circulations.
Registering of the TLE.
It performed by 2 oscilloscopes: with trace length 4 ms and time sample 16μs, and trace length 64 ms and time sample 256μs.
Examples of UV flashes of energy 1011 – 1012 erg in 1-64 ms intervals were detected.
Global map of UV flashes
Positions of the UV detector at new moonand full moon
in reference to the Earth and the Sun.
UV transient event number as a function of lunar phase
Correlation between the transient UVevent rates
Energy distribution of UV TLE radiation recorded by DUV
Carrier rocket: “Soyuz-2” Upper-stage rocket “Fregat”
Polar Sun synchronous
Altitude: 800 – 850km
Assembling of the satelliteand scientific equipment
Ground track of TATIANA-2 satellite
Block-diagram of UV, IR and CPD detectors at the MSU “Tatiana 2” satellite
Sensitive aria 350 cm2
Energy threshold 1 Mev
UV & CPD detectors electronics block- diagram
Example of UV intensity recording on-orbits.
Examples of UV, IR and CP temporal distribution by TATIANA-2 above SAA
One day TLE distribution recorded by TATIANA-2
above cloud word map
Part of flash events are observed in cloudless regions and was not detected by WWLLN
Every orbit with close longitudes have been observed the same picture-long series
of flash events. Length of such series reach 10 thousand kilometers which is much more
longer then thunderstorm or clouds area crossed by satellite.
Lighting flashes density
above land ~ 5·10-5 min-1km-2
above water ~ 5·10-7 min-1km-2
Flash events density recorded by TATIANA-2
above land ~ 5·10-5 min-1km-2
above water ~ 5·10-5 min-1km-2
Typical lighting geographical distribution in winter and summer
All recorded thunderstorm cloud to ground lightings are in good correlation with clouds
Low energy flash events distributed uniformly at the globe map, at least at the night site of orbit observed by UV detector during TATIANA-2 mission.
Low energy flash event Global distribution statistics
Distribution of registered flash events on the map in pixels 300300
Main number of flashes distributed above continents at the regions with high lighting activity. We believe main part of flashes have ionospheric origin.
DUV on the board CHIBIS micro satellite of Institute for Space Research
of Russian Academy of Sciences
Total mass 40kg
Serves equipment 12,6kg
Scientific payload 10,8kg
Orbit altitude 480km
The launch of the CHIBIS micro satellite is planned to celebrate the 50-years of the launching of the first man in space in USSA
Sensitive area ~ 0.5cm2
Field of view ~ 150
Mass ~ 0.65kG
Power < 2.5Wt
UV and IR detector for Aragats cosmic station
Structure of the set up for lighting observation at Aragats Cosmic Station
Aragats UV and IR detector testing in Nor Amberd laboratory with lamp
Aragats UV and IR detector testing in Nor Amberd laboratory with LED sours
1.The background radiation of light from charged particles in the optical components of the detector is negligibly small as compared with the airglow on the darkest nights.
2.It is confirmed by experiments that the PMT can operate with a regulated high-voltage power supply in the transition mode from a large illumination on the day side of the Earth to a small one on the night side.
3.The afterglow effect of the PMT proves to be small as compared with the airglow even on the darkest nights. In ultraviolet intensity measurements by one detector, a wide dynamic range of ~105 was reached.
4. For observation of bursts, the digital oscilloscope method was successfully applied. Bursts with an ultraviolet radiant energy of hundreds of kJ were recorded
5, Ground base UV and IR detector successfully was tested in Nor Amberd Cosmic Ray Laboratory with LED flash source
1. PMT is able to operate in period of several years in the orbit in the day and night regime.
2. The regime of the PMT operation with variable gain following by the UV light intensity increase detector duty cycle.