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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F10.7 Observations and Predicts

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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.