Department of Space PhysicsInstitute of Experimental Physics, SAS

Slovak & Czech Horizon 2020 Space Information dayBratislava, 13. december 2013

Prof. Juraj Dubinský Prof. Karel Kudela

RNDr. Ladislav Just, CScIng. Jozef Rojko, CSc

Founder, leadingand most influential,persons inDepartment history

ShortLookTo History

36 yearsSinceFirstDetectorin space(2013)

1977SelectedMissions/resultsFrom history

1996SelectedMissions/resultsFrom history

1999

2004SelectedMissions/resultsFrom history

SelectedMissions/results

2014

55 yearsmeasurements

history

Online at http://neutronmonitor.ta3.sk

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

● Extreme Universe Space Observatory

● JAXA+ESA+NASA+ROSKOSMOS 14 countries

● Slovakia official member since 2008

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

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

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

1m

1m

Lenses

Electronics Detector

Laser and IR Camera Simulations

EUSO ballonCNES

March2014

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

~ 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%

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%∼

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.

Analysis of fake trigger events background in JEM-EUSO experiment

Patterns from backgroud can not be mistaken with real event

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.

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 ?

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)

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

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

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

Simulations / Models

● Cosmic rays trajectories and ditribution in Earth's magnetosphere

Models developed~ 20 years of development and

publication activity

GeoMag – www.geomagsphere.org

Particles motion in magnetosphere model

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

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

HelMod - www.helmod.org Web version of model (ver. HelMod 1.5.) Model description + bibliography

Spectra of protons at 1AU catalog

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

HelMod online - www.helmod.orgSimulator

beta

ECRS – twice organized in Kosice by DSP IEP SAS

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, ...

Thank you

Contact:

More information atSpace.saske.skJem-euso.skHelMod.orgGeoMagnetosphere.org

Pavol Bobikbobik@saske.skInstitute of Experimental PhysicsSlovak Academy of SciencesDepartment of Space PhysicsWatsonova 47040 01 KošiceSlovakia

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