department of space physics
TRANSCRIPT
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Department of Space PhysicsInstitute of Experimental Physics, SAS
Slovak & Czech Horizon 2020 Space Information dayBratislava, 13. december 2013
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Prof. Juraj Dubinský Prof. Karel Kudela
RNDr. Ladislav Just, CScIng. Jozef Rojko, CSc
Founder, leadingand most influential,persons inDepartment history
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ShortLookTo History
36 yearsSinceFirstDetectorin space(2013)
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1977SelectedMissions/resultsFrom history
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1996SelectedMissions/resultsFrom history
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1999
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2004SelectedMissions/resultsFrom history
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SelectedMissions/results
2014
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55 yearsmeasurements
history
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Online at http://neutronmonitor.ta3.sk
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Actual projects BepiColombo (ESA mission to Mercury) – participation on PICAM development
Double Star TC2-NUADU
JEM-EUSO – Slovakia official member since december 2008, 4th International JEM-EUSO Collaboration Meeting in Torino
Luna Glob (spectrometer ASPECT – in development phase)
Neutron monitor Lomnický štít
Resonance (spektrometer DOK-M – in development phase)
Rosetta - ESA mission to comet 67P/Churyumov–Gerasimenko
Simulations / particles in Magnetosphere and Heliosphere
Spektrum Radioastron / MEP2 (start 18.7.2011)
Venus Express – participation on data analysis
theory-models / already measured missions / missions in development-preparations
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● Extreme Universe Space Observatory
● JAXA+ESA+NASA+ROSKOSMOS 14 countries
● Slovakia official member since 2008
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JEM-EUSO - Main Scientific Objectives
• Main Objective: Astronomy and Astrophysics through the particle channel – Identification of sources by high-statistics arrival
direction analysis – Measurement of the energy spectra of
individual sources (spectral shape, flux, power)
Understand and constrain acceleration and emission mechanisms
Physics and Astrophysics at E > 5×1019eV
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JEM-EUSO - Exploratory Scientific Objectives
• Exploratory Objectives: new messengers– Discovery of UHE neutrinos – Discovery of UHE Gammas
High discovery potential; tests of new physics models
• Exploratory Objectives: magnetic fields– Constrains on the galactic and local
extragalactic fields
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JEM-EUSOPrecursor experiments
● Tellescope Array EUSO● ~Apríl 2014, Utah TA
● callibration
● trigger scheme
verification
● MiniEUSO ● inside ISS – view through UV
transparent windows
● ESA astronaut Samantha Cristoforetti, 42 ISS crew, November 2014
● Map of UV background in 300-400 nm
Window – american segment
Window - russian partWeight : 30 kgDimension : 350×350×600 mmPower : 30 W
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1m
1m
Lenses
Electronics Detector
Laser and IR Camera Simulations
EUSO ballonCNES
March2014
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JEM-EUSO - SK participation
● Since 4th International JEM-EUSO Collaboration Meeting in Torino, Italy 2008
● Main tasks
1) The estimation of the UV background on the night side of the Earth
Sources of the background are Moon, stars, airglow, man made lights, lightnings, auroras etc..
2) The determination of the JEM-EUSO operational efficiency
Fraction of time when monitoring UV compared to full time on orbit. Above mentioned UV background sources together with ISS operation schedule had to be taken into account in the model of JEM-EUSO operational efficiency
3) The fake trigger event simulations and analysis
The goal of the trigger system is to detect the occurrence of scientifically valuable signal among very huge background noise detected by JEM-EUSO. The UV background registered by JEM-EUSO is randomly distributed. We study if these random processes produce fake pattern, which could be mistakenly interpreted as EECRs events.
www.jem-euso.sk
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~ 21-22 %
Duty cycle estimationUV light sourcesIf background 1500 ph/(m2 ns sr) is allowed [in % of total time on orbit]
- sun
- moon
- airglow/nightglow
- zodiacal light
- integrated faint star light
- Boreal/austral auroras
- South Atlantic anomaly
- Lightning and TLEs
- artificial sources (Anthropogenic / city light)
} ~ 20-21%
}
~ 1%
small
~ 2%
~ 9%
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Duty cycle estimationAuroras effect on JEM-EUSO operational efficiency
2017–2019 probably again deep solar minimum – effect of auroral light to restrain EAS measurements 1%∼
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Duty cycle estimationSAA effect
Evaluated upper limit ~4 ph/(m2 ns) is approximatelly in order of 1% in comparison to photons which pass the detector and reach the FS from the standard UV BG of 500 ph/(m2 ns sr).
This leads to conclusion that electrons trapped in non disturbed magnetosphere do not affect the JEM-EUSO operational duty cycle significantly.
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Analysis of fake trigger events background in JEM-EUSO experiment
Patterns from backgroud can not be mistaken with real event
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ESA-BepiColombo / PICAM
Planetary Ion CAMera will provide the mass composition, energy and angular distribution of low energy ions up to 3 keV in the environment of planet Mercury.
The Department of Space physics IEP-SAS contributes to PICAM construction in the frame of scientific-technical cooperation with The National University of Ireland, Maynooth, Ireland.
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Resonance DOK-M
● The project RESONANCE is a magnetospheric space exploration mission dedicated for advanced study of the wave – particle interactions in the Earth's magnetosphere. The project RESONANCE is conducted by Space Research Institute (IKI-RAN) in Moscow, Russian Federation.
● The DOK-M spectrometer is equipped with four passive cooled silicon solid state detectors, two of them are dedicated for detection of the energetic ions, another two detect the energetic electrons.
● Start: 2014 ?
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RadioAstron - Spektrum R / MEP-2
MEP-2 - Monitor of Energetic Particles
Start: 18. july 2011 First data: august 2011 fluxes and spektra of electrons
(30 keV–350 keV) and ions (30 keV–3.2 MeV)
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Data analysis: Venus express
● Little or no solar wind enters Venus' atmosphere at solar minimum
● Zhang T. L., Delva M., Baumjohann W., Auster H.-U., Carr C., Russell C. T., Barabash S., Balikhin M., Kudela K., Berghofer G., Biernat H. K., Lammer H., Lichtenegger H., Magnes W., Nakamura R., Schwingenschuh K., Volwerk M., Vörös Z., Zambelli W., Fornacon K.-H., Glassmeier K.-H., Richter I., Balogh A., Schwarzl H., Pope S. A., Shi J. K., Wang, C., Motschmann U., Lebreton J.-P.
● Venus has no significant internal magnetic field, which allows the solar wind to interact directly with its atmosphere. A field is induced in this interaction, which partially shields the atmosphere, but we have no knowledge of how effective that shield is at solar minimum.
The bow shock is close to the planet, meaning that it is possible that some solar wind could be absorbed by the atmosphere and contribute to the evolution of the atmosphere. Here we report magnetic field measurements from the Venus Express spacecraft in the plasma environment surrounding Venus. The bow shock under low solar activity conditions seems to be in the position that would be expected from a complete deflection by a magnetized ionosphere. Therefore little solar wind enters the Venus ionosphere even at solar minimum.
● Nature, Volume 450, Issue 7170, pp. 654, 11/2007
IF 26.681
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Data analysis / Space weather
● Erlykin, A. D.; Gyalai, G.; Kudela, K.; Sloan, T.; Wolfendale, A. W., On the correlation between cosmic ray intensity and cloud cover, eprint arXiv:0906.4442, 30 pages, 10 figures, accepted for publication in Journal of Atmospheric and Solar-Terrestrial Physics, acknowledgements replaced, Journal of Atmospheric and Solar-Terrestiral Physics , 71,17-18, 1794-1806, 2009
● Papailiou M., Mavromichalaki H., Kudela K., Stetiarova J., Dimitrova S.V., Effect of geomagnetic disturbances on physiological parameters: An investigation on aviators, Advances in Space Research, Volume 48, Issue 9, p. 1545-1550, 2011
● Papailiou M., Mavromichalaki H., Kudela K., Stetiarova J., Dimitrova S.V., Cosmic radiation influence on the physiological state of aviators, Natural Hazards
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Data analysis / Magnetosphere
● Vainio R., Desorgher L., Heynderickx D., Storini M., Flückiger E., Horne R, B., Kovaltsov G, A., Kudela K., Laurenza M., McKenna-Lawlor S., Rothkaehl H., Usoskin I. G., Dynamics of the Earth's Particle Radiation Environment, Space Science Reviews, Volume 147, Issue 3-4, pp. 187-231, 2009
● McKenna-Lawlor S., Li Lu, Dandouras I., Brandt Pontus C., Zheng Y., Barabash S., Bucik R., Kudela K., Balaz J., Strharsky I., Moderate geomagnetic storm (21-22 January 2005) triggered by an outstanding coronal mass ejection viewed via energetic neutral atoms, Journal of Geophysical Research, Volume 115, Issue A8, CiteID A08213, 2010
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Simulations / Models
● Cosmic rays trajectories and ditribution in Earth's magnetosphere
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Models developed~ 20 years of development and
publication activity
GeoMag – www.geomagsphere.org
Particles motion in magnetosphere model
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HelMod - www.helmod.org
Heliosphere Modulation Monte Carlo Code: HelMod
More than 10 years development
Selected articles:
Della Torre et al., AdvSR 2012, 49, 11, 1587
Bobik et al. Ap.J. 2012, 745:132
www.helmod.org
2012 – catalog of HelMod results
2013 – HelMod OnlineBETA
– first public model in the field
2014 – public code
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HelMod – selected results
Table 2 and 4
error-weighted root mean square of the relative difference between experimental dataand those resulting from simulated differential intensities
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HelMod - www.helmod.org Web version of model (ver. HelMod 1.5.) Model description + bibliography
Spectra of protons at 1AU catalog
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HelMod online - www.helmod.org
HelMod online – beta version- already opened to use
- after registrationat http://www.helmod.org/online
- and Login at http://www.helmod.org/online/prihlasenie.php
User can use
- HelMod Calculator - to find intensity of protons at 1AU for different LIS - fast
- HelMod Simulator - HelMod v2.01 run - to evaluate spectrum of protons, antiprotons, electrons, positrons at any distance from the Sun, with possibility set also user defined LIS - long/overnight simulation with results received ~12 hours after submitting job
beta
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ECRS – twice organized in Kosice by DSP IEP SAS
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Popularization / outreach Web: space.saske.sk/popul
TV: STV, TA3, TV Naša
Radio: Slovenský rozhlas, FUN Rádio, Lumen, ...
Press: SME, Pravda, Trend, Hospodárske noviny, Quark, Plus1deň, Košický večer, Korzár, Nový čas, ...
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Thank you
Contact:
More information atSpace.saske.skJem-euso.skHelMod.orgGeoMagnetosphere.org
Pavol [email protected] of Experimental PhysicsSlovak Academy of SciencesDepartment of Space PhysicsWatsonova 47040 01 KošiceSlovakia
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Hot-Pay / PEEL● Project HotPay is a Norwegian sounding rocket
mission to atmosphere and ionosphere organized by Andoya Rocket Range ARR and associated ALOMAR Observatory.
The project consists of two sounding rocket experiments, the HotPay-1 (summer launch), and HotPay-2 (winter launch). The full name of the project is: ALOMAR eARI (enhanced Access to Research Infrastructure), the Rocket Launch opportunity is called "HotPay Services".
The PEEL experiment (Precipitation of Energetic Electrons at high Latitude ) has been developed at DSP-IEP-SAS in cooperation with Democritus University of Thrace in Xanthi, Greece and Andoya Rocket Range for sounding rocket HotPay-2.
● Start 31.1.2008