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.

1.MSU Micro satellite TATIANA UV Detector and Results of measurements

2.MSU Micro satellite TATIANA-2 UV, IR and Charged Particles detectors and First Results of measurements

3. ISR of RAS Micro satellite CHIBIS-M UV and IR detectors

4. UV and IR detectors for Ararat's Cosmic Station for Study Elementary Particle Acceleration in Thunderstorm Electric Field.

5. Conclusion TEPA 2010

Parameters of the ‘‘Tatiana’’ satellite

Mass, kg 25Power, Wt 7

Ground track of TATIANA satelliteAltitude 1000kmInclination 820

TATIANA

Parameters of the UV detector

Mass, kg 0.5Field of view, degree ±7Power, Wt 0.6PMT R1463

The scientific instruments were prepared and constructed by D.V. Skobeltsyn

Institute of Nuclear Physics.

Mass of scientific instrument, kg 7Power, 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

84

3

1

2

U74

3

1

2

U69

MAX

797

AD73

03

1V

CC

O

10

1IO

10

2IO

_V

RE

F1

03

IO1

04

IO_

VR

EF

10

5IO

10

6IO

10

7IO

108 M2

109 VCCO

11IO

110 M0112 M1

113 IO114 IO115 IO116 IO_VREF117 IO118 IO_VREF119 IO

12

IO

121 IO122 IO123 IO_VREF124 IO125 IO

127 IO

128 VCCO

13

IO_

VR

EF

130 IO131 IO132 IO133 IO_VREF134 IO135 IO

137 IO138 IO_VREF139 IO

14

IO

140 IO_VREF141 IO142 IO

143TMS

16

GC

K3

17

VC

CO

19

GC

K2

2TCK

20

IO2

1IO

22

IO_

VR

EF

23

IO2

4IO

27

IO2

8IO

_V

RE

F2

9IO

3IO

30

IO_

VR

EF

31

IO3

2IO

_W

RIT

E3

3IO

_C

S

34TDI36TDO

37VCCO

38CCLK

39IO_DOUT_BUSY

4IO

40IO_DIN_D041IO42IO_VREF43IO44IO_VREF45IO_D1

47IO_D248IO49IO

5IO

_V

RE

F

50IO_VREF51IO_D352IO53IO

55VCCO

56IO58IO59IO_D4

6IO

60IO_VREF61IO62IO63IO_D5

65IO_D666IO_VREF67IO68IO_VREF69IO

7IO

_V

RE

F

70IO_D771IO_INIT

72 PROGRAM

73

VC

CO

74 DONE

76

IO7

7IO

78

IO7

9IO

_V

RE

F

8IO

80

IO8

1IO

_V

RE

F8

2IO

85

IO8

6IO

87

IO_

VR

EF

88

IO8

9IO

90

GC

K0

92

VC

CO

93

GC

K1

95

IO9

6IO

_V

RE

F9

7IO

98

IO

Electronics diagram

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 moon and full moon in reference to the Earth and the Sun.

UV transient event number as a function of lunar phase

Correlation between the transient UV event rates

Energy distribution of UV TLE radiation recorded by DUV

Carrier rocket: “Soyuz-2” Upper-stage rocket “Fregat”

Operating orbit: Polar Sun synchronous Altitude : 800 – 850km Inclination 98.80

Mass: 100kg Power: 100W

Assembling of the satellite and scientific equipment

Ground track of TATIANA-2 satellite

Altitude 850km Inclination 98.80

Block-diagram of UV, IR and CPD detectors at the MSU “Tatiana 2” satellite

Thickness 0.5cmSensitive 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 WWLLNEvery 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 cloudsdistribution.

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 40kgServes equipment 12,6kgScientific payload 10,8kgPower 50WtOrbit 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

UV 240-400nmRed 610-800nmSensitive area ~ 0.5cm2Field of view ~ 150Mass ~ 0.65kGPower < 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

CONCLUSIONS

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.