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Title. Yu. D. Kotov and CORONAS-PHOTON team. Scientific objectives and observational capabilities of "Coronas-Photon" project. Federal Space Agency Russian Academy of Science Principal Organization: Moscow Engineering Physics Institute (Technical University). - PowerPoint PPT PresentationTRANSCRIPT
Yu. D. Kotov and CORONAS-PHOTON team
Scientific objectives and observational capabilities
of "Coronas-Photon" project
Federal Space AgencyRussian Academy of Science
Principal Organization: Moscow Engineering Physics Institute
(Technical University)
Title
Russian program CORONAS
КОРОНАС Комплексные ОРбитальные Околоземные Наблюдения Активности Солнца
CORONAS Complex ORbital ObservatioN of Activity of Sun
CORONASCORONAS--II с с 03.03.19941994 по по 12.12.20002000 ((IZMIRAN, IZMIRAN, CB“Yuznoe”CB“Yuznoe”))
CORONASCORONAS--FF с с 07.2001 07.2001 по по 12.200512.2005 ---- ----||----||----
CORONAS-PHOTONCORONAS-PHOTON 2008 2008 (Astrophysics Institute (Astrophysics Institute of MEPhIof MEPhI, , NIIEM NIIEM, , VNIIEM VNIIEM))
CORONAS-PHOTON mission is the third satellite of the Russian CORONAS program on the Solar activity observations.
The main goal of the CORONAS-PHOTON mission is the study of the Solar flare hard electromagnetic radiation in the wide energy range from Extreme UV up to high energy gamma - radiation (~2000MeV)
Magnetic field
dominates plasma
creates intricate
structure/heats
Magnetic structure as it is seen in UV
TRACE
Generation of gamma-rays in the solar atmosphere be accelerated particles
Electromagnetic radiation spectrumfrom intense solar flare
Cycle 24 Maximum
• The panel is split down the middle on whether it will be bigger than average or smaller than average, namely:
• Will peak at a sunspot number of 140(±20) in October, 2011
Or• Will peak at a sunspot number of 90(±10) in
August, 2012– An average solar cycle peaks at 114– The next cycle will be neither extreme, nor average
CONSENSUS STATEMENT OF THE SOLAR CYCLE 24 PREDICTION PANEL
March 20, 2007• The Solar Cycle 24 Prediction Panel anticipates the solar minimum marking the onset of
Cycle 24 will occur in March, 2008 (±6 months). The panel reached this conclusion due to the absence of expected signatures of minimum-like conditions on the Sun at the time of the panel meeting in March, 2007: there have been no high-latitude sunspots observed with the expected Cycle 24 polarity; the configuration of the large scale white-light corona has not yet relaxed to a simple dipole; the heliospheric current sheet has not yet flattened; and activity measures, such as cosmic ray flux, radio flux, and sunspot number, have not yet reached typical solar minimum values.
• In light of the expected long interval until the onset of Cycle 24, the Prediction Panel has been unable to resolve a sufficient number of questions to reach a single, consensus prediction for the amplitude of the cycle. The deliberations of the panel supported two possible peak amplitudes for the smoothed International Sunspot Number (Ri): Ri = 140 ±20 and Ri = 90 ±10. Important questions to be resolved in the year following solar minimum will lead to a consensus decision by the panel.
• The panel agrees solar maximum will occur near October, 2011 for the large cycle (Ri=140) case and August, 2012 for the small cycle (Ri=90) prediction.
A National Solar Observatory map of observed magnetic fields correlates closely with the NCAR model of the fields. Both images show the longitudinal averages of the fields. (Courtesy Mausumi Dikpati, Giuliana de Toma, Peter Gilman, Oran White, and Charles Arge).
Scientists for years have known about the current of plasma, or the meridional flow, which moves at about 20 meters (66 feet) per second near the surface. But they had not previously connected it to sunspot activity.
New model Mausumi Dikpati and colleagues (Geophys. Research Letters, March 3,2007)
Latitude distribution of the flares
As the plasma current approaches the poles, it sinks about 200,000 kilometers down into the Sun’s interior and starts its return journey back to the equator
The Great Conveyor Belt is a massive circulating current of fire (hot plasma) within the Sun. It has two branches, north and south, each taking about 40 years to perform one complete circuit. Researchers believe the turning of the belt controls the sunspot cycle, and that's why the slowdown is important.
"Normally, the conveyor belt moves about 1 meter per second-walking pace," says Hathaway. "That's how it has been since the late 19th century." In recent years, however, the belt has decelerated to 0.75 m/sec in the north and 0.35 m/sec in the south. "We've never seen speeds so low."According to theory and observation, the speed of the belt foretells the intensity of sunspot activity about 20 years in the future. A slow belt means lower solar activity; a fast belt means stronger activity. "The slowdown we see now means that Solar Cycle 25, peaking around the year 2022, could be one of the weakest in centuries," says Hathaway
Предсказания: Активность на 50% больше, чем в 23 цикле. Начало цикла в конце
2007 или начале 2008. Максимум в 2012
BUT! Phys. Rev. Lett. 98 131101 Arnab Rai Choudhuri and colleagues from the Indian Institute of Science in Bangalore and the Chinese Academy of Sciences in Beijing calculate that the next cycle (known as cycle 24) will be about 35% weaker than cycle 23 (11 April 2007)
F10.7 Observations and Predicts
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Observations Predicted in Advance
#23 #24#22#21
Schatten et al. Predicted in advance
Observations
F10.7 Observations and Predicts
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1940 1950 1960 1970 1980 1990 2000 2010 2020 2030
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Observations Predicted in Advance
#23 #24#22#21
Schatten et al. Predicted in advance
Observations
W.Dean Persell, April 2007
Satellite CORONAS – PHOTON (METEOR type)Weight <2250kg
Launcher: Cyclon-3MCosmodrome: Plesetsk
Orbit: Circular 550±10 km. Inclination 82.5 deg
Nominal mission lifetime 3 years extended 5 years
Telemetry 8.2 GHz; Onboard memory 1.0Gbyte
Launching date at the summer season of the 2008
Orbit and Launcher
CORONAS-PHOTON Spacecraft
Orientation of longitudinal axis to the Sun direction
(day part of orbit)
Pointing accuracy 10' (nominal)*
Posteriori pointing accuracy 1.5'
Destabilization of the longitudinal axis during the shadow part of the orbit
0.3'/sec Angular disturbance is less than 0.005 deg/s
* Signals from instrument TESIS will be used to get: transverse axes stabilization longitudinal axis stabilization
≤0.5 deg ≤3′
Accuracy of time registration
1 msec
Scientific payload
Instruments for registration of gamma-radiation and neutrons
Seven Full Solar disk UV & soft X-ray monitors
TESIS assembly of instruments for XUV imaging spectroscopy of the Sun
Instruments for charge particle measurements
Simi-imagingRT-2 X-ray monitor
+ Magnetometer
Российские участники Российские участники проекта «КОРОНАС-ФОТОНпроекта «КОРОНАС-ФОТОН»»(создание научной аппаратуры)(создание научной аппаратуры)
Московский инженерно-физический институт (МИФИ), Москва - головной
Научно-исследовательский институт ядерной физики МГУ (НИИЯФ МГУ), Москва
Физико-технический институт РАН (ФТИ РАН), Санкт-Петербург
Физический институт РАН (ФИ РАН), МоскваИнститут земного магнетизма, ионосферы и
распространения радиоволн РАН (ИЗМИРАН), Троицк
Институт космических исследований РАН (ИКИ РАН), Москва
Зарубежные участники Зарубежные участники проекта «КОРОНАС-ФОТОНпроекта «КОРОНАС-ФОТОН»»
(создание научной аппаратуры)(создание научной аппаратуры)
Харьковский национальный университет (ХНУ), Харьковский национальный университет (ХНУ), Харьков, Харьков, УкраинаУкраина
TTaaттa a институт фундаментальных исследований (ТИФР), институт фундаментальных исследований (ТИФР), Мумбай, ИндияМумбай, ИндияСцинтилляционные детекторы США
Полупроводниковые детекторы CZT Израиль
Многоканальная электроника Норвегия
Центр космических исследований Польской академии наук Центр космических исследований Польской академии наук (ЦКИ ПАН), (ЦКИ ПАН), Вроцлав, ПольшаВроцлав, Польша
Полупроводниковый детектор США
Instruments for registration of gamma-radiation and neutrons
Instrument Measured radiation Organizations Weight kg High energy
radiation spectrometer
NATALYA-2M
Gamma-rays spectroscopy 0.3 – 2000MeV;
Neutrons 20 – 300MeV
Moscow Engineering-
Physics Institute (MEPhI)
PI Yu.D.Kotov
360.0
Solar flare and GRB
spectrometer KONUS-RF
Hard X-ray & gamma-ray spectroscopy with high temporal resolution (0.0112) MeV
Ioffe Physical-Technical Institute,
PI E.P.Mazets
31.5
Hard X-ray polarimeter
PENGUIN-M
Soft X-rays 1 – 10keV Hard-X-ray polarization 20–150keV Spectroscopy 0.15 – 5MeV;
Ioffe Physical-Technical Institute,
MEPhI PI A.S.Glyanenko
29.5
Fast X-ray monitor FXM
Hard X-ray with sub-msec temporal resolution 20 – 500keV
MEPhI PI V.N.Yurov
10.5
Low energy gamma-ray
spectrometer RT - 2
Hard X-ray spectroscopy: Phoswich NaI(Tl)/CsI(Na) 15 – 150keV; 100–2000keV CZT - detector 10-100keV
TATA Institute of Fundamental
Research (TIFR), ISRO and others
PI. A.R.Rao
68.0
Full Solar disk UV & soft X-ray monitorsInstrument Radiation bands Temporal resolution Detector type
SphinXSpace Res. Center,PolandPI J. Sylwester P.N. Lebedev PI, Russia MEPhI, Russia
Soft X-rays0.5 keV– 15 keV
Solar disk radiation monitoring up to 10 msec
Pure Si PIN-diode 500μm thick, aperture 19.96, 0.397 and 0.0785 mm2 (Amptek, USA)
PHOKARussia MEPhI, PI A.Kochemasov
4 channels (nm) Visible, FUV & XUV <1100; 116-125; 27-37 & <11
Solar disk radiation monitoring 2 secOccultation mode 0.1 sec
AXUV-100G 10mmx10mm(International Radiation Detectors, CA, USA)
SOKOLRussia,IZMIRAN, PI V.D.Kuznetsov
7 Visible & NUV channels (nm)1500, 1100, 850, 650, 500, 350, 280 (bandwidth <10%)
Solar disk radiation monitoring 30 sec
Photodiodes with filter (effect. square
TESIS assembly of instrumentsTESIS assembly of instruments for XUV imaging spectroscopy of the Sun
Name of channel
Parameter
FeXX XUV
telescope
HeII XUV
telescope-coronagraph
WF XUVwide
field telescope-
coronagraph
Mg XII spectro-
heliometer
XUV spectro-
heliometer
SphinX Solar
Photometer in X-rays
Spectral band, Å
131-133 295-315 8.418-8.423 280-335 1- 10 keV
Field of view
Full disk: 60
60 in the field of 2.5
Corona up to 5 radii - 2.5
Full disk: 60
1.6 (cross to dispertion)
Spatial resolution, arcsec
1,7 4.4 2 3 (cross to dispertion)
256 channel
Spectral resolution
/~70 /~20 /~20 2*10-4 Å/pix 2*10-2 Å/pix Full Sun
It is advanced version of the SPIRIT instrument
Kuzin S. et al; Cospar meeting 2006 talk E2.1 009 - 06
Instrument Measured radiation Organizations Weigh, kg
Energetic particle analyzer
ELECTRON-M
e : 0.2 – 2MeV p : 1.0 – 150MeV He: 1.5 – 50MeV/nucleon
Institute of nuclear physics of Moscow
State University; PI S.N.Kuznetsov
16.0
Energetic particle telescope STEP-F
e : 0.15 – 10MeV p : 4.0 – 62MeV He: 15.5 – 245.5MeV
Kharkov State University
PI I.I.Zalubovsky
7.5
Instruments for charge particle measurements
Magnetometer
SM-8M
three components of magnetic field in the range of –55 T … +55 T
FGU NPP “Geologorazvedka”, St-Petersburg, Russia;
MEPhI, Russia
PI V.N.Yurov
3-axis magnetometer
RT-2/G
RT-2/S
RT-2/GA
PINGUIN
KONUS-RF
PHOKA
TESIS STEP-F
Magnetometer
pressure vessel
N-2M
KONUS-RF-anti
Ground segment CORONAS-PHOTON project
NATALYA-2M
Energy channels of Natalya-2M instrument (defined by trigger mode)
ChannelChannel Energy regionEnergy region, , MeVMeV
Effective Effective areaarea, , cmcm22
Energy Energy resolutionresolution
ΔΔEE//EE
TimingTiming
X-ray and gamma-raysR 0,3 – 2 920 10% (662 keV)
measured1 ms
L 2 – 10 900 5% (2,5 MeV)measured 1 sec
M 7 – 200 800 6% (10 MeV) calculated
1 sec
H 50 – 2000 750 32% (500 MeV) calculated
1 sec
NeutronsN (neutrons) 20 – 300 37 – 120 – 32 sec
Data readoutfrom the high-energy radiation spectrometer
NATALYA-2M
Routine Energy range, MeV
Spectral data
Timing
Number of ADC channels
Collection time, sec
Number of energy channels
Collection time, sec
0.2-2.0 4 x 1024 (four
independent detectors)
1 4 x 2 (two channels for
each detector)
0.1 (0.001 – 1 sec by command)
1.0 – 10 1024 1 1 0.1 7-200 256 16 sec/ each event tagging
70-2000 256 16 sec / each event tagging n / 2-200
MeV Matrix 256x256 channels
each event tagging
Data readout from spectrometer KONUS-RF
Two detectors based on NaI(Tl) scintillator Ø127x76.2 mm
Measurement mode
Timing Spectral Routine Flare Routine Flare
Ene
rgy
rang
e
Num
ber
of
chan
nels
Collection time, sec
Duration, sec
Collection time,
msec
Num
ber
of
chan
nels
Collection time
Duration after
trigger, sec
Spectrum
collection time,
sec 10 -1000 keV
12 (quasi-
log)
112 (quasi-
log)
0.25 – 10 MeV
10 (quasi-
log)
1
0 – 3 2
3 – 35 16
35 – 165 64 154
(quasi-log)
No measure-ments
0 – 3 0.1
3 – 67 0.5
67 – 163 4.0
Gamma-line response
1 2 3 4 5 6 7101
102
103
104
105
Cou
nts/
MeV
Energy (MeV)1 2 3 4 5 6 7
102
103
104
2x104
24Mg
20Ne 28Si20Ne
16O12C
2H
(Cou
nts/
MeV
)*M
eV2
Energy(MeV)
NATALYA-2M L-mode 1.0-10.0 MeV
neutron/gammapulse shape
discrimination3D diagram ofenergy output verses pulse shape parameter in CsI(Tl) detector
14 MeV neutron beam calibration
Anticoincidence counter
NaI(Tl) detector of scattering X-rays
PTF counter to scatter X-rays
Proportional counters
Anticoincidence counter
Pinguin-M (disassembled)
Three RT-2 detectors
The Tantalum Coded Mask is coded by open and close pattern of squares of size 2.5mm. Its dimensions are 180 x180 x0.5mm.
Mechanical slat collimator made up of Tantalum surrounded by a graded shield with viewing angles of 4º x 4º and 6º x 6º respectively.
Four CDZ modules
Two phoswich detectors One CZT detector
Coded Mask Imaging Concept
Multiple pin-hole MASK
Mask casts shadow on detector plane
Shift of shadow pattern encodes source location
Cross correlation of mask pattern with shadow recovers shift and locates sources
Design characteristics of RT-2.
Type Phoswich
NaI(Tl)+CsI(Na)CZT
Thickness (mm) 3+25 5
Size (mm) 117.6 dia40 X 40
(4 numbers)
Readout PMT1024 pixels
(ASIC)
Effective area (cm2)(@60 keV)
100 64
Energy resolution(@60 keV)
18% 8 %
Energy range15 – 150 keV(extended 2
MeV)
10 – 100 keV
Time Resolution (ms)
10 10
Specifications of CZT detector
Area 64 cm 2
Pixels 1024
Pixel size 2.5 mm X 2.5 mm (5 mm thick)
Read-out ASIC based (8 chips of 128 channels)
Imaging method Coded Aperture Mask (CAM)/ FZP
Field of View 6 o X 6 o CAM
3 o X 1.5 oFZP
Angular resolution 30 arcmin/ 30 arcsec
Energy resolution 5% @ 100 keV (< 8%)
Energy range 10 – 100 keV
Up to 1 MeV (Photometric)
CZT: Hard X-ray detector of the future …..
Good energy resolutionGood efficiencyPixelated : Moderate imaging Background estimation Avoids source confusionBackground reductionGood spectroscopic detector
Note: Used up to now only as a gamma-ray imager
Fresnel’s Zone Plate• It is made up of Tantalum of 1 mm
thickness and alternate solid and hollow regions with 4 flanges to support the overall structure.It is fabricated using MEMS.
• The deconvolution of source is done from the interference fringes formed by two zone plates.The radii of the annulus are governed by:
rn = (n)1/2 x r1
where, r1 = radius of innermost disc
It has following advantages over contemporary decoding methods:
(i) Very high order of precision of source location.
(ii) Highly economical in terms of volume.
FXM
YАlO3(Ce)
YAP(Ce): Yttrium Aluminum Perovskite doped with Cerium (chemical formula YAlO3:Ce) is a non-hygroscopic, glasslike, inorganic scintillator with a high density, but a relatively low effective atomic number (36). The wavelength of maximum emission is 35 nm, the decay time is short, 27 ns, the light output is typically 40% of that of NaI(Tl) and the material is relatively stable over a wide temperature range.
In intense flare temporal In intense flare temporal resolution up to 1msresolution up to 1ms
dimensions of 13 mm in height and 68 mm in diameter
Multi-channel solar photometer SOKOL
Continuous observations of the solar radiation intensity variations in range 280 - 1500 nm,
relative intensity resolution 2х10-6 of total solar intensity, observation angle - 2°.
Technical parameters:•radiation intensity is measured simultaneously in 7 optical spectrum bands by 8 photosensors: 280, 350, 500, 650, 850, 1100 and 1500 nanometers with the measuring bandwidth below 10% of the value of central wavelength. •relative intensity resolution is 2х10-6 of the total solar radiation intensity. •temporal resolution of intensity measurements - 30 sec. •spacial resolution is not available. •photometer observation angle - 2°. •precision of the photometer orientation towards the center of the solar disk is 5 arc. min. •the photometer consists of the photosensors unit PU and electronics unit EU. Dimensions: PU - 130х130х510 mm. Weight: 5.2 kg.
View of instrument
PHOKA bands Channel
## Type of deposit filter Filter
thickness, nm
wave-length, nm
Remarks
Working channels 1 No filter - <1100 Visual
channel 2 Ti/Pd 200/100 <11 3 Cr/Al 100/200 27-37 4 2 external filters
Acton 122-XN-0.5D 116-125 Ly-α
channel Reserve channels
5 Ti/Pd 200/100 <11 6 Cr/Al 100/200 27-37 7 2 external filters
Acton 122-XN-0.5D 116-125 Ly-α
channel
STEP-F instrument is able to register fluxes of:electrons 0.4 – 14.3 MeV;protons of 9.8 – 61.0 MeV;alpha-particles of 37.0 – 246.0 MeV.
The detector block includes two identical silicon position-sensitive
detectors and two scintillation detectors. Each silicon detector has the size
of 45×45 mm and 350 μm thickness. Scintillation detectors are based on
CsI(Tl) crystals and viewed by large area photodiodes. The average
telescope field of view is 97×97°. The size of each of 36 matrix square
elements of semiconductor detector is 7.3×7.3 mm, which allows to receive
the average angular resolution in telescope total field of view about 8°.
The effective area of each semiconductor detector is 20 сm2, scintillation
detectors is 36 and 49 сm2. Geometric factor of STEP-F instrument is 20
сm2·str.
STEP-F
D1: Si, h = 0.03 cm 45×45 mm
D2: Si, h = 0.03 cm 45×45 mm
D3: CsI(Tl), h = 1.3 cm60×60 mm
D4: CsI(Tl), h = 1.0 cm70×70 mm
D1, D2 – silicon position-sensitive totally depleted pin-detectors;D3, D4 – scintillation detectors.