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PROJECT PROPOSAL #

I. Summary Project Information

1. Project Title and Taxonomy Full title: Investigation of the energetic processes in the atmosphere, ionosphere and magnetosphere at the Aragats space-environmental

center

Short title: Energetic processes in the atmosphere, ionosphere and magnetosphere

Technology area: PHY-ANU, INS-DET, ENV-MRA

Category of technology development: Technology Development, Fundamental Research

Key words: Cosmic rays, Thunderstorms, Ground-based detections

2. Project Manager Name: Chilingarian Ashot

Title: Doctor of Phys.- Math. Science Position: Head of the Cosmic Ray Division, AANL.

Street address: 2 Alikhanyan Brothers

City: Yerevan Region: Transcaucasia

ZIP: 375036 Country: Armenia

Tel.: 37410-352041 Fax: 37410-352041

E-mail: chili@aragats.am

3. Participating Institutions

3.1. Leading Institution

Short reference: AANL

Full name: Artem Alikhanyan National Scientific Laboratory

Street address: Alikhanyan Brothers 2

City: Yerevan Region:

ZIP: 375036 Country: Armenia

Name of Signature Authority: Taroian Sargis

Title: Candidate of science (physics mathematics) Position: Deputy Director

Tel.: 37410-34-41-29 Fax: 3741-350030

E-mail: taroian@yerphi.am

Governmental Agency: Ministry of Economy

3.2. Other Participating Institutions None

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4. Foreign Collaborators/Partners

4.1. Collaborators

Institution: Karlsruhe Institute of Technology, (Campus North),Institute for Data Processing and Electronics (IPE)

Street address:

Hermann-von-Helmholtz Platz 1

City: Eggenstein-Leopoldshafen Region/State:

Baden-Wurttemberg

ZIP: 76344 Country: Germany

Person: Hartmut Gemmeke

Title: Professor Position:

Director of the IPE (Emeritus)

Tel.: 0049-7247-82-5635 Fax: 0049-7247-82-5594

E-mail: gemmeke@ipe.fzk.de

Institution: School of Physics and Astronomy, University of Leeds, UK

Street address:

E.C. Stoner Building

City: Leeds, LS2 9JT Region/State:

ZIP: Country: UK

Person: Johannes Knapp

Title: Doctor Position:

Head of High Energy Astrophysics

Tel.: 0044-(0)113-343-3890 Fax: 0044-(0)113-343-3900

E-mail: j.knapp@leeds.ac.uk

4.2. Partners None

5. Project Duration 36 months

6. Project Location and Equipment

Institution Location, Facilities and Equipment

Leading Institution Artem Alikhanyan National Scientific Laboratory, 2 Alikhanyan Brothers, Yerevan, Armenia. Aragats and Nor-Amberd research station, Aragatsotn district, Armenia Particle detectors of the Aragats Space-Environmental Center

7. Total Project Effort

Total number of participants 45

Number of weapon scientists and engineers 23

Total project effort (person*days) 16,700

Total project effort of weapon scientists and engineers (person*days) 9,140

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8. Financial Information

8.1. Estimated Project Costs

Estimated total cost of the project (US $) 973,500

Including:

Payments to Individual Participants 493,500

Equipment 190,000

Materials 100,000

Other Direct Costs 100,000

Travel 65,000

Overhead 25,000

8.2. Funding Sources Estimated total cost of the project (US $) 973,500 Financial Sources:

Requested from the ISTC 973,500 Other financial source 1 0

Other financial source 2 0

Non-Financial Sources:

Non-financial source 1 60,000

Non-financial source 2 2,200, 000

9. Summary of the project The enhanced climatic instability observed recently world-wide, increased frequency of extreme events (floods and droughts, storms, heat and cold waves, fires, etc.) requires developing instruments for the research and forecasting the probability of their occurrence. The Sun is the driving force of processes in the atmosphere, ionosphere and magnetosphere. The full solar-terrestrial system includes the solar wind, the magnetosphere, the ionosphere and the atmosphere. The system is influenced by radiation from the sun and the flux of solar and galactic cosmic rays. The radiation environment near the earth and plasma-geomagnetic field interactions constitutes the space weather conditions. Space weather influences the terrestrial climate and natural hazards; although the mechanisms of space weather effects on the earth are far from being explained and many aspects of the solar activity itself are still unclear. These effects can be understood and quantitatively estimated only by studying the solar-terrestrial system in its entirety: identifying the solar agents affecting the earth, understanding their occurrence and evolution, and understanding the mechanisms of solar energy transfer from the sun all the way to earth. This requires integration of all existing information and specific knowledge now spread in many different scientific areas: solar physics, solar wind, cosmic rays, interplanetary space, magnetosphere, ionosphere, and upper, middle and lower atmosphere.

Sudden, thunderstorm correlated huge fluxes of electrons, positrons, gammas and neutrons detected at Aragats, are undoubtedly newly discovered global physical phenomena that are well-matched to the measured by orbiting gamma observatories fluxes of terrestrial gamma-rays. Particle acceleration and multiplication and broad-band electromagnetic emissions associated with thunderstorms trigger various dynamic processes in the atmosphere-ionosphere chain, causing global effects on earth. Precise muon detectors operating on the Earth surface and in the underground halls could be the first instruments to provide data both for space weather forecasting and meteorology. Extraordinary enhancement of the informative content of measured time series of particle fluxes by making transition from HZ to MHz time scale will open broad possibilities of the physical analysis and forewarning on dangerous consequences of the space and terrestrial weather.

Simultaneous disturbances of the muon flux and of the geomagnetic field point to particle-field interactions in the upper atmosphere. The amplification of the radio frequency electric field signals from EAS during a thunderstorm can lead to the modulation of the EAS size spectra and, consequently, to the possible estimation of the inter-cloud electric fields. Optical monitoring of the upper atmosphere reveals the origin of the transient luminous events huge (TLEs) energy flows (up to several gigajoules in one pulse) from atmosphere to ionosphere and draw attention to the upper atmospheric discharges that possibly could be dangerous for high–altitudes flights. The newly discovered high energy phenomena in the atmosphere undoubtedly can affect the troposphere and ionosphere, and, therefore, the terrestrial climate.

In the framework of the proposed project will be developed an integrated approach for the research of solar-terrestrial connection, the coupling of the solar wind with magnetosphere, space weather issues and fluxes of high energy solar particles, as well as their effects on climate and cloud formations. The newly discovered phenomena – relativistic runaway electron avalanches will be measured by networks of particle detectors at high altitudes. The precise measurements of magnetic and electrical fields, as well as broad bandwidth

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radio emission and lightning detection will help to understand high energy atmospheric phenomena as well as origination of lightning and their influence on climate. The links connected space and terrestrial weather will be investigated and clarified.

These fluxes of the high energy particles (the highest known energies of particles originating in the atmosphere) result in the deposit these particles from the upper atmosphere to the ionosphere and magnetosphere. These phenomena should be considered as an integral component of the solar-terrestrial connections, since thunderstorms are largely driven by solar-induced convection. The investigation of the RREA process may be helpful for understanding the consequences of injection of high-energy radiations into space to the climate, ionosphere and troposphere.

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PROJECT PROPOSAL #

II. Detailed Project Information

1. Introduction and Overview The recently recognized growing influence of the dynamic processes in the atmosphere and the Earth's magnetosphere on human civilization disclosed the risks of climate change and reveals increased frequency and severity of climate anomalies and extreme weather events. On the other hand, the growing importance of satellite and other global technologies in different areas exposed to a variety of phenomena in space and atmosphere requires understanding of space weather and terrestrial weather agents and their reliable forecasting. There is growing understanding that advanced infrastructures of the astroparticle physics experiments should be used also for the research and monitoring of the major geophysical parameters. Thus, the Pierre Auger Observatory has set up a dedicated atmospheric monitoring programme at the site of the observatory in the province Mendoza, Argentina.

The goal of this proposal is the development of a new multivariate approach to the study of geophysical phenomena; the installation of new precise sensors and high-speed networks of particle detectors and field meters with powerful servers; development of the databases and mirror sites providing fast access and visualization possibilities for users; development of users friendly interfaces to multivariate correlation analysis of the time series of major geophysical parameters; issuing warnings and alerts on dangerous consequences of space weather and terrestrial weather. For the first time the Relativistic Runaway Electron Avalanche (RREA) process will be considered with all its manifestations obtained by various experimental techniques including:

• Measurements of the low energy (1 – 50 MeV) electrons, neutrons and gamma rays from the relativistic runaway electron avalanche (RREA) processes, which exhibit themselves as thunderstorm ground enhancements (TGEs);

• Measurements of the solar modulations effects (Forbush decreases (Fd), geomagnetic effects (Ge), ground level enhancements (GLE); issuing warnings and alerts on severe conditions of space weather;

• Precise measurements of the geomagnetic and electrical fields;

• Measuring and storing time series of particle fluxes on the MHz time scale; correlating obtained time series with electrical and magnetic fields, as well as with lightning development;

• Broadband electromagnetic signal detection from thunderstorms;

• Monitoring of the transient luminous effects(TLE) in the upper atmosphere;

• Monitoring of lightings with network of the radio-lightning detectors.

Established in 2000 Aragats Space Environmental Center (ASEC) (Chilingarian et al., 2003a, 2005) is the world’s largest center for monitoring of the cosmic particle fluxes. ASEC facilities measure and estimate intensities of the neutral and charged particle fluxes in the broad energy range from MeV to PeV. The complex of ASEC facilities is a unique combination of particle detectors providing real-time data from many energetic channels, from different directions with good temporal resolution and, thanks to its high altitude, also with high statistical accuracy. ASEC already returned results on the relation of the changing intensities of the cosmic ray fluxes with Space Weather effects. ASEC launched one of the first services of warning of violent radiation storms (Gevorgyan et al., 2006). Several scientific centers are now operating Space Weather portals based on surface particle detector data (Kuwabara et al., 2006, Mavromichalaki et al., 2005, 2006), some of them include the ASEC data in the surveys. ASEC monitors registered almost all severe events of the 23rd solar cycle and report them widely to the scientific community (Proceedings of ICRC, Puna, India, 2005, Lodz, Poland, 209) Proceedings of SEE-2005, Nor Amberd, 2005, Forges-2008, Nor Amberd, 2008, Armenia, Proceedings of COSPAR congresses, China 2006, Montreal, 2008, Bremen, 2010).

In the framework of the new ISTC project, new facilities will be installed at ASEC; the network of the hybrid particle detectors will be expanded in Armenia and worldwide; via new electronics and advanced data analysis systems we will achieve integration of terrestrial and space systems on one Space Weather portal. During the last 10 years at the Cosmic Ray Department a brand new scientific and technical infrastructure was developed, including new particle detectors, modern electronics, powerful computers and networking, advanced data Acquisition (DAQ) and data integrating systems, uninterruptable power supplies, teaching laboratories and other. More

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than 50 papers were published in refereed journals and ~100 reports were presented to International scientific forums and on meetings. CRD experts prepared and delivered undergraduate, master and PhD programs for Yerevan State University (YSU) students, including courses on High Energy Astrophysics, Cosmic Rays, Modeling of Physical process and modern Electronics. 4 PhD thesis and more than 50 undergraduate and graduated theses were defended. The CRD has now adopted a western scheme of employment, broadly including undergraduate and graduate students in research. Scientific cooperation with European, Japanese and USA scientists is organized via joint research projects, scientific visits and joint participation in conferences.

2. Expected Results and Their Application Internet portal with information on current status of solar-terrestrial connections and Space Weather. Running forewarning services based on the solar modulation effects posed on the stable background of the galactic cosmic rays. Forewarnings and alerts will be used by satellite operators, operators of the power plants and gas and oil pipelines. 2.1. Sustainability Implementation Plan

2.1.1. Results to be promoted Fundamental scientific results on the electron acceleration in thunderstorm atmospheres; Development of remote sensing methods for the early recognition of potentially dangerous phenomena in the atmosphere and near-Earth space; Creation of the new instruments for registration, processing and forecasting of space and terrestrial weather based on the flux of particles incident on the Earth’s surface; Using of the astroparticle physics research infrastructures as powerful innovative tools to study, probe, and monitor atmosphere, ionosphere and magnetosphere. Presentation of the research results at international conferences, publication of articles in peer-reviewed journals, organization of topical conferences and seminars.

2.1.2. Uniqueness of results

• Aragats space environmental center provides reliable and precise measurements of the fluxes of the most species of cosmic rays. The energy range of the detected particles is 106 - 1016 eV.

• Monitoring of particle fluxes is performed 24 hours 12 months without any brakes on 3 altitudes 1000, 2000 and 3200 m, (40˚25′N, 44˚15′E; Vertical cutoff rigidity in 2007: 7.1 GV). Within the proposed project we plan to install particle detectors underground in a salt mine where is very low radiation environment. An additional possibility of global cosmic ray monitoring is provided by the SEVAN (Space Environmental Viewing and Analysis Network) world-wide network of particle detectors located in Armenia, Croatia, Bulgaria and India. Further expansion of the network is planned.

• Precise field meters continuously monitor disturbances of the geomagnetic and geo-electrical fields, as well as the emerging electrical field between thunderclouds and earth.

• Networks of antennas for measurements of the radio emissions provide the information on the location and type of lightning; • Measurements of the time series of the particle fluxes with an unprecedented accuracy of the MHz scale will open very broad

possibilities for the physical analysis, including correlations with disturbances in the electrical and geomagnetic field as well as with lightning development, making the particle fluxes a tool for monitoring and researching of the major geophysical parameters.

• A network connects all facilities with powerful servers and databases at CRD headquarters in Yerevan, as well as with mirror servers in USA and Europe; fast and user friendly visualization programs for the on-line data analysis. There is no research center in the world that measures so many different geophysical parameters; located at several high altitudes and providing on-line data worldwide. Participants of the project have expertise in designing and fabricating particle detectors, in designing and commissioning modern electronics; in constructing wireless networks and databases; in developing codes for the data acquisition, data transfer and visualization; in performing simulations of physical processes in the atmosphere and in calculating detector response. A huge advantage of ASEC is its consistency, 24 hours coverage, multi-year operation. In contrast the planned life of the satellites and space station is a few years only, they are affected by the same solar blast that they should alert of, and space-born facilities instead of following the event in progress are put in the stand-by mode. 2.1.3. Demand for results The comprehensive monitoring and prediction of potentially dangerous processes in the magnetosphere and atmosphere of the Earth is important for evaluating the risk in various areas of the economy, in particular, to ensure the safety of existing and emerging large industrial facilities, the destruction of which has a catastrophic impact and long lasting effect on the environment and living conditions. Although the potential impacts of destructive factors are normally taken into consideration however, early warning of any natural cataclysms, which may affect not only the object itself, but also its electronic systems, allows taking timely actions to prevent or reduce possible damage. Another aspect of this problem is various high-tech security information and control systems, destruction of which may lead to the consequences, comparable with the destruction of traditional technological infrastructures such as electric power lines, roads, and oil & gas pipelines. The results of the project are suitable for real-time correlation with meteorological observations. They are also potentially useful for air navigation: adding high energy information to storm-tracking monitoring systems. 2.1.4. Expected income

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Subscription fee for the services, providing on-line information on the geophysical parameters, consulting and other benefit can reach 200,000 USD annually. Planned investigations on the possibility of hail forecasting, if successful, will bring even more profit from Armenian agriculture. 2.1.5. IPR situation Intellectual property rights on results to be developed in the framework of the proposed project will belong to the project team and will follow ISTC rules and regulations. 2.1.6. Additional developments The particle detector network in Armenia will be enlarged by incorporating the new type of detectors (NaI) and locations (salt mine); the world-wide network of particle detectors also will be expanded to new countries. New field meters, networks of antennas and weather stations will be installed. Corporative network will connect all new detectors with servers and data bases; visualization and data analysis/forecasting issuing codes will be developed. 2.1.7. Plan of implementation The business scheme will be tuned according to planned marketing studies. Products and services developed in the project will form an essential part of the planetary global change surveys to be established in the coming years. 2.1.8. Additional licenses or permits Not needed 2.1.9. Business network We are part of the world-wide research networks of particle detectors. We plan to establish working relations with agencies and institutions providing global change research and services.

3. Meeting ISTC Goals and Objectives 1. Supporting the applied, fundamental research and theoretical elaboration for their future usage in the national economy; 2. Integrating of the scientists previously works in the military sphere into international scientific association; 3. Creating the new possibilities for active scientific and business contacts with foreign specialists; 4. Assisting in the solution of the international problem of the global change and space exploration.

4. Scope of Activities

Task 1 Uninterruptable monitoring of the major geophysical parameters, modernization of the main facilities and infrastructures of the ASEC and SEVAN networks

Task description and main milestones Participating Institutions Task 1.1 Continuous operation of the ASEC monitors and SEVAN network; measurement and delivery of the time series of the major geophysical parameters to databases and mirror sites.

Task 1.2 Modernize scientific and technical infrastructures of the ASEC and SEVAN particle detector networks; repair of MAKET surface array, installing new particle detectors, field meters, weather stations, celiometers (lidar based screening devices for mapping the structure of clouds) and radio-antennas.

Task 1.3 Modernization and maintenance of the corporative network; installation of new high speed servers, reliable wireless modems; optical cables and other networking equipment.

Task 1.4 Development and fabrication of the data acquisition electronics based on the FPGs and microcontrollers. Install new precise electronic devices (flash-ADCs for measuring time series on the MHz time scale. Modernize and install new integrated data transfer and storage software. Improve resolution of the timing servers for the local computer networks.

1-AANL

Description of deliverables

1 Time series of particle fluxes; NaI detectors: new lab in underground salt mine; celiometers; weather stations, new servers and networking equipment; reliable and fast data acquisition electronics.

2 Reports and journal publications.

Task 2 Investigation of the Relative Runaway Electron avalanches (RREA) and its influence on cosmic ray fluxes, disturbances of geomagnetic and electrical field.

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Task description and main milestones Participating Institutions Task 2.1Simulations of the high energy particle acceleration/multiplication in the thunderstorm clouds. Modeling of the influence of main geophysical parameters on variations of the energetic and spatial characteristics of the particle fluxes.

Task 2.2 Investigate meteorological and space weather induced disturbances of the geomagnetic field and changes in cosmic ray fluxes. Introduce automatic systems of issuing alerts and warnings.

Task 2.3 Investigate consequences of the RREA process; measure and simulate interconnections between particle fluxes detected at earth surface and in the space, as well as the radio emissions and transient luminous events.

Task 2.4 Investigate processes in the thunderstorm clouds; measure structure of clouds and electrical field; find causal connections between thunderstorm cloud height and structure and emerging enhancements of the particle fluxes.

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Description of deliverables

1 Detected RREA events at Aragats; simulation codes, the automatic system of warnings and alerts;

2 Reports on RREA process, journal publications.

Task 3

Development of the WEB Portal and software for real time analysis of particle flux variations caused by geophysical processes (Solar activity, Disturbances of the geomagnetic field, relativistic runaway electron avalanches, hurricanes, storms, etc…).

Task description and main milestones Participating Institutions Task 3.1Develop sophisticated Global change/Space Weather portal presenting project results, services, scientific and educational materials.

Task 3.2 Development of the methods of the processing of multidimensional experimental information from sensors located on earth and in space.

Task 3.3 Creation of the system of the analysis of meteorological information on the basis of universal software/hardware complex for receiving and processing information from orbital satellites and autonomous weather station.

Task 3.4 Development and maintenance of the databases, multivariate visualization programs, Bayesian and neural network based statistical models on CRD servers and mirror sites.

1-AANL

Description of deliverables

1 WEB Portal, computer codes, meteorological data

2 Publications, reports, WEB materials

5. Role of Foreign Collaborators/Partners • Providing comments to the technical reports and scientific papers; • Support in development of technical equipment and modeling; • Joint publications; • Crosschecks of the developed methods and their implementation; • Providing contacts with national and international organizations interested in global change monitoring and forecasting of

natural catastrophes.

6. Technical Approach and Methodology 1. Multivariate approach to measuring as many geophysical parameters as possible ISTC starting from 1997 sustains investigations of geophysical phenomena using nuclear-particle-physics methods in Artem Alikhanyan National Scientific Laboratory (AANL). ISTC supports space weather research in Cosmic ray division (CRD) of AANL by funding projects A116, A216, A757, A1058, SCP-042 and finally A1554. Implementation of these projects allows developing one of world best facilities for the monitoring of the major geophysical parameters including fluxes of the cosmic rays, geomagnetic and electrical fields, lightning occurrence. Results and achievements from these ISTC projects will be used in new proposed project, i.e. networks of particle detectors, advanced networking equipment, servers and mirror sites, visualization programs, etc… CRD developed brand new scientific and technical infrastructure including new particle detectors, modern electronics, powerful computers and networking, advanced data Acquisition (DAQ) and data integrating systems, systems of uninterruptable power supply, teaching laboratories and others. Developed by CRD methods for the analysis of multi-dimensional experimental data are successfully used in other scientific laboratories, including

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contemporary experimental complexes such as MAGIC, KASCADE. Correlation multivariate analysis of variations of fields, radiation and fluxes can provide new data on the development of thunderstorm anomalies in the atmosphere, including those of catastrophic nature. Analysis of the disturbances of the cosmic ray fluxes over an extended period of time before and during the powerful thunderstorms exhibited the existence of significant correlations between these phenomena, and, as a consequence, a principal possibility of the advance recognition of thunderstorms within a radius of up to 50-100 km.

Figure 1 Main building of Aragats station experimental facilities to be used in project

The Aragats Space Environmental Center (ASEC, see Chilingarian et al., 2003, 2005) of AANL is located on the highland 3250 m above sea level, 5 km from the southern peak of Aragats (3750 m.), near a large lake. The thunderstorm activity on Aragats is extremely strong in May-June and September-October. Sometimes lightning continuously hit the ground in the vicinity of the station during an hour or longer. Thunderstorm clouds are usually below the southern peak (i.e. not higher than 500 m above) and sometimes less than 100 m above the Aragats research station. Along with Solar modulation effects, ASEC detectors register several coherent enhancements associated with thunderstorm activity. Near 50 such events detected in 2007-2009, at solar cycle minimum, unambiguously pointed on the thunderstorm correlated particle acceleration and multiplication. The experimental techniques used, allow for the first time to simultaneously measure fluxes of the electrons, muons, gamma rays and neutrons correlated with thunderstorm activity (Chilingarian, Daryan, et al., 2009). Most of particle detectors and field meters are located in the MAKET building (see Figure 1) and nearby. Along with 16 plastic scintillators belonging to the already canceled MAKET ANI surface array, in operation are Aragats Solar Neutron Telescope (ASNT); Aragats Neutron Monitor (ArNM) of 18NM64 type; and SEVAN particle detectors. In 2010 especially for the detection of low energy electrons and gamma rays from the thunderstorm clouds 2 new detectors were installed outdoor nearby the MAKET building, namely STAND and CUBE scintillation detectors. ArNM is detecting neutrons and ASNT and SEVAN- both neutral and charged species of the fallen secondary cosmic ray flux. Aragats Solar Neutron Telescope is a part of the world-wide network coordinated by the Nagoya University (see details in Chilingarian et al, 2007) aiming primarily to measure the fluxes of the neutrons born in the violent solar flares. In 2006, with the installation of new Data Acquisition electronics (DAQ, Arakelyan et al., 2009) facility was turned to a “deep” calorimeter measuring particle energy release in the range of 7 -120 MeV. Histograms of the energy releases in the thick scintillators, are measured and stored each minute, providing the exact pattern of the energy releases during solar transient events and during thunderstorms by the RREA process. The ASNT consists of 4 up and 4 bottom scintillators, each having the area of 1 m2. The distance between layers is ~ 1.2 m. The data acquisition system can register all coincidences of detector signals from the upper and lower layers, thus, enabling measurements of the arrival of the particles from different directions. The signals ranging from 0.5 mV to 5 V, from each of 8 photomultipliers, are passed to the programmable threshold discriminators. The output signals are fed in parallel to the 8-channel OR gate triggering device and to a buffer. If there is a signal in the channel we will denote it by “1” and the channels that were not fired within the “opening” of the gate (gate duration is ~ 1µsec) – by “0”. The ASNT trigger condition is defined by detecting at least one signal in the 8 data channels. The trigger rate of the entire detector system does not exceed 10 kHz. The duration of the entire data readout and signal processing procedure is less than 10 µsec. There are 23 different possibilities of so called “basic states”. 16 of them carry information about the direction of the incident particle. For example, the state configuration “0010” for the upper layer and “0010” for the lower layer corresponds to the charged particle traversal through the third upper and third lower scintillators (zenith angle between 0 and 30º). Combination “0010” and “1000” corresponds to the traversal through the third upper and the first lower scintillator (zenith angle between 20 and 40º). The other 7 possibilities, give additional valuable information on the particle flux incident on the detector. For instance, the combination “01”, i.e. no signal in the upper and in the lower layer can be attributed to the traversal of a neutral particle. However, due to the small sizes of the anticoincidence shielding several charged particles

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can hit the detector from the side. Nonetheless, if the particle beam is near vertical (it is just the case of electron-gamma avalanche hitting ASNT), we can measure the energy release spectrum of the thunderstorm correlated gamma rays. The combination “01”, selects neutral particles, visa-verse the combination “10”selects low energy charged particles (due to energy losses in the roof the threshold energy is ~15-17MeV). The top scintillators have the thickness of 5 cm (energy release for the vertical electrons and muons is ~ 10 MeV) the combination “11” will select charged particles with energy greater that 25-27 MeV. Advanced Data Analysis System (ADAS) provide registration and storage of all logical combinations of the detector signals for further off-line analysis and for on-line alerts issuing (Chilingaryan, 2006).

The standard Neutron Monitor (NM) of 18NM-64 type (Stoker et al, 2000) operates in Aragats research station. ArNM consists of 18 boron filled proportional chambers, located below 5 cm of lead (producer) and 10 cm of polyethylene (moderator). Secondary protons and neutrons interacting with lead producer give birth to numerous neutrons of smaller energies which release energy in polyethylene (thermalised) and enter the proportional counter filled with gaseous boron. A small fraction of these neutrons (~ 5%), are absorbed by 10B isotope, and generate an alpha-particles detected by the proportional chamber. The neutron monitors are equipped with DAQ electronics, providing 3 different values of the detector dead time - 0.4, 250 and 1250 µsec. Only incident hadrons can be detected by the neutron monitor, the sensitivity of ArNM to electrons, muons and gamma rays is vanishingly small.

The new particle detector system, named SEVAN (Space Environmental Viewing and Analysis Network, Chilingarian and Reymers, 2008, Chilingarian et al., 2009), simultaneously measures fluxes of most species of secondary cosmic rays, thus representing an integrated device used for the exploration of the solar modulation effects. The basic detecting unit of the SEVAN module is assembled from standard slabs of 50x50x5cm3 plastic scintillators. Between two identical assemblies of 100 x 100 x 5 cm3scintillators (4 standard slabs) are located two 100 x 100 x 5 cm3 lead absorbers and thick 50 x 50 x 20 cm3scintillator stack (4 standard slabs). A scintillator light capture cone and PMTs are located on the top, bottom and intermediate layers of the detector. Incoming neutral particles undergo nuclear reactions in the thick 20 cm plastic scintillator and produce protons and other charged particles. In the upper 5cm thick scintillator, charged particles are registered very effectively; however, for the nuclear or photonuclear interactions of neutral particles there is not enough substance. When a neutral particle traverses the top thin (5cm) scintillator, usually no signal is produced. The absence of the signal in the upper scintillators, coinciding with the signal in the middle scintillator, points to neutral particle detection (gamma ray or neutron). The coincidence of signals from the top and bottom scintillators indicates the traversal of high energy muons, traversing 10 cm of lead (minimal energy ~250 MeV).

Two detector assemblies measuring the Extensive Air Showers (EAS) operate on the Aragats research station. The main goal of the GAMMA (Garyaka, Martirosov et al., 2007) and MAKET-ANI (Chilingarian, Hovsepyan et al., 2007) detectors is to measure the energy spectra of cosmic rays to understand their origin and particle acceleration mechanisms. Both detectors use the plastic scintillators overview by photomultipliers to determine the number of electrons in the shower and infer the energy and type of the primary particle. About 300 detecting channels formed from 5 cm thick scintillators with area 1m2 each are located at highland of Mt. Aragats at altitudes 3200 – 3250 m. EAS detectors are triggered arrays; however each detector simultaneously counts all incident particles to detect the time series of the changing fluxes. High count-rate (~30,000 counts per m2 per minute), combined with the large area of the detector assembly makes surface arrays ideal detectors for measuring additional electron flux correlated with thunderstorms. We select several detectors of the surface arrays and implement special trigger conditions for detecting additional fluxes of low energy cosmic rays and large particle bursts in correlation with thunderstorm activity. Twenty six of 1 m2, 5 cm. thick scintillators, located in iron boxes comprise the surface array of the Aragats Multichannel Muon Monitor (AMMM). Another 16 same type scintillators located inside and in the vicinity of the building where most of other particle detectors are located, see Figure 1. AMMM and MAKET detectors measure the low energy charged species of secondary cosmic rays with very high accuracy: the relative error of mean values of the one minute time series is 0.13% and 0.18% correspondingly. Each of MAKET detectors provide the time series of the number of counts per minute and the array on the whole also provides, the so called, EAS trigger (“firing” of more than 8 selected detectors of array within the time window of ~1 µsec). From the triggered events we can select other firing combinations of detector channels (for instance, events with all 16 channel firing). These 2 selections (>8 and all 16 firing channels) at fine weather collect EAS with sizes ~104 and ~2*104 electrons correspondingly.

The STAND detector is a 3-stack of 1 cm thick and 1 m2 area molded plastic scintillators with fiber-glass light shifters purchased from the High Energy Physics Institute, Serpukhov, Russian Federation. Also the same type 3 cm. thick scintillator is located aside. The STAND detector is a 3-stack of 1 cm thick and 1 m2 area molded plastic scintillators with fiber-glass light shifters fabricated by the High Energy Physics Institute, Serpukhov, Russian Federation. Also the same type 3 cm. thick scintillator is located aside. The energy thresholds of the 1 cm thick scintillators are ~1, 3 and 5 MeV correspondingly from top to bottom: energy threshold of the 3cm thick – 3 MeV. The energy thresholds of the rest of ASEC scintillators range from 7 to 18MeV (dependent on the amount of substance above); therefore in 2009 we reconstruct energy spectra of RREA electrons only from 7 MeV. The energy spectra of the 2010 events will be reconstructed from 1MeV. The aim of the CUBE detector is to measure both charged and neutral flux separately with enhanced purity of neutral flux. For it the assembly of two 20 cm thick and 0.25 m2 area plastic scintillators is fully surrounded by the six 1 cm thick 1 m2 area plastic scintillators. The detector will measure count rates of the neutral particles if there is at least one signal from 2 inner scintillators without any signal from outer surrounding thin scintillators. The rejection power of the anticoincidence shielding is ~40. The energy release spectra is registered and stored from each of the thick scintillators every minute. The count rates of the surrounding 6 scintillators are measured and stored as well with all possible double combinations of firing. In the MAKET building in 2010 we install the Magnetoteluric station LEMI-417, designed and commissioned by Lviv center of Space Research Institute of Ukrainian Academy of Science. One-minute time series of the 3-dimensional measurements of the geomagnetic field enter ASEC data base and will highly improve research of correlations of the geomagnetic parameters and changes of the fluxes of

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cosmic rays. The same device is measuring also components of the electric field. Additionally we install the “electrical mill” device for measuring electrical field between clouds and surface and network of lightning locators based on the broad band radio emissions of intercloud, and cloud ground lightning. The time series of the frequency of different 4 types of lightning, measured by the Boltec Storm tracker also enters ASEC monitors data base. The Storm Tracker consists of direction finding antennas and a data acquisition board. In the antenna box two coils oriented North-Southward and West-Eastward are located. The coils detect magnetic fields generated by lightning discharges that occur within a 600 km radius and sends the resulting induced voltages to the processor board. The processor digitizes, analyzes and converts the discharges signals into range and bearing data. It also classifies the kind of strike, is it positive or negative is it intra-cloud, inter-cloud, or cloud–to-ground. If processor unit can’t estimate the bearing direction, the strike is being classified and stored as a noise. The bandwidth of the antenna is meant to be 40-400 kHz. Storm Tracker's direction-finding antenna provides direction information while storm distance is calculated from received signal strength. Special processing in software reduces the effects of strike-to-strike energy variations providing more accurate distance information. All described sensors are operational now and with adding NaI based particle detector, sophisticated weather station and celiometer for screening the inner structure of the thundercloud we’ll be able to achieve all goals of the project in researching all manifestations of the RREA project and understanding the lightning phenomenon itself. The example of new possibilities of the research at Aragats is demonstrated in figure 2.

Figure 1The multiple correlations of electrical, geomagnetic fields and particle flux

In Figure 2 we post the time series of changing fields and particle flux. There were 3 particle flux enhancements at 14-19 September, 2010. We can see a very strong correlation of the particle peaks with electrical field between clouds and ground. Detailed observation of the electrical field on the 1 sec scale reveal very fast oscillations- electrical field abruptly change from positive values up to 30 kV/m to negative values up to 40 kV/m. These oscillations coincide with particle enhancements. Also we can notice in Figure 2 that there we abrupt decreases of the z component of the geomagnetic field before and during particle events. These apparent correlations points on very reach physics opened with new ASEC data measuring as much as possible geomagnetic parameters. However, to measure the shape of TGFs, investigated event-to-event differences, decide if there are different classes of TGF's connected with different models of its origin; and finally to prove a theoretical model of the new physical phenomena we need to measure the microsecond scale signal by flash ADCs. And it is only one of numerous application opened with going to precise temporal measurements of the fallen cosmic ray flux. Cosmic rays are screening magnetosphere, ionosphere, troposphere, atmosphere and fast changing cosmic ray fluxes contain information about the structure and dynamic of these structures. ASEC is equipped already with large fast scintillators and can use them to solve various important physical problems. Stacked in an array 3-cm thick and 1 m2area plastic scintillators will be installed in 4 locations: Yerevan, Nor Amberd, Aragats and salt mine 400 m underground. The micro-millisecond count rate data from these systems will give revolutionary results in several branches of sciences.

1. Ground-based observations of thunderstorm-correlated fluxes of high-energy electrons, gamma-rays and neutrons

Lord Charles Thompson Rees Wilson in 1924 realized that “particle started with suitable velocity in the electrical field of the thundercloud may be expected to continue to acquire kinetic energy at the rate of many thousand volts per cm”. In 1992 Alexander Gurevich, Gennady Milikh and Robert Roussel-Dupre introduced the theory of the generation of fast “runaway “electrons from the MeV electrons of the Extensive Air Showers (EAS) initiated by the energetic proton or nuclei incident on the top of the atmosphere. However, the nature of seed particles is still under debate; alternative source of the seed particles is connected with the lightning leaders (Saleh et al., 2009, Carlson et al., 2009). Although, there are no exact measurements yet of the possible strength of the electric field, in the Moss et al., 2006 was suggested that streamer heads can produce fields up to several tens of million volts per meter. The electrical fields in the thunderstorm atmosphere gave the cosmic-ray shower or/and electrons from the lightning leaders a boost by increasing the number of

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energetic particles through a multiplication process initially called Runaway Breakdown (RB), and now referred as Relativistic Runaway Electron Avalanche (RREA), (Babich et al., 1998, Dwyer, 2007). The RREA mechanism can create large amounts of high-energy electrons and subsequently the gamma rays, as well as X-rays and neutrons. Unfortunately, this model has not yet been able to demonstrate the creation of the hot plasma channel and lightning itself.

Astonishingly, the physical processes in the low atmosphere were observed by the orbiting gamma observatories at 400-600 km above the earth’s surface. Terrestrial Gamma Flashes (TGF), very short (millisecond) bursts of high energy gamma rays, are routinely observed by satellite gamma ray detectors during last 15 years (see Fishman et al, 1994, Smith et al., 2005). Recently the TGF have been observed in correlation with strong thunderstorms in the equatorial regions (Marisaldi et al., 2010). The spectra of the flashes are roughly expressed by power-law function with exponential decaying term; some of them extending up to several tens of MeV. In the reference (Dwyer et al., 2007) these events were interpreted as byproducts of the massive number of runaway electrons being generated within or immediately above thunderclouds. Surface detections of the RREA process, although have long history, are discrepant and rare.Only after detection at Aragats on September 19, 2009 of very large enhancement of count rate detected by all particle monitors the evidence of the RREA process on the earth surface was established undoubtedly. The electron spectrum in the energy range 7-20 MeV is fitted by an exponential function, see Figure 3; the spectral index is -0.18. Electron spectrum abruptly ended at ~30 MeV, as there is no evidence of additional electrons detected by ASNT. The reconstructed energy spectrum of the incident gamma rays described by a power function is steeper than detected electron energy spectrum and continued till ~45MeV. Gamma ray energy spectrum is fitted by a power function in the range 7-30 MeV; in the energy range 30 - 45 MeV gamma ray spectrum is rather well described by the exponential function with slope equals to -0.14 and afterwards abruptly vanished near 45MeV, see Figure 3. The error bars of the gamma ray energy spectrum are statistical ones.

Figure 2Unfolded electron and gamma ray spectra fitted by exponential and power functions.

During the particle event on September 19 huge enhancements of the electrons, gamma-rays and neutrons, as well as short particle bursts, counting millions of the additional particles and distributed over a large area were detected. The observations of ASEC monitors prove the existence of the long lasting electron-photon avalanches developing in the atmosphere during thunderstorms. For the first time we measure the electron and gamma ray energy spectra and made quantitative calculations of the some phenomenological parameters of RREA process. Exponential spectrum of the RREA electrons is in good agreement with expectations based on the simulations (Dwyer, 2004) and gamma ray power energy spectrum do not contradict recent observation of the TGF by orbiting gamma observatories (Marisaldy, 2010). However, we recognize that we measure only high energy tails of the energy spectra of electrons and gamma rays; to measure bulk of particles of lower energies we need new particle detectors with much lower energy thresholds, under operation from August, 2010 at Aragats.

2. Monitoring of the solar-terrestrial connections

The traditional for ASEC research space weather monitoring will be continuing with new aspects of correlations with global climate change. After long period of absolutely calmness (see Figure 4), Sun started to present first signs of activity; although not yet seen in the cosmic ray flux. The cosmic ray flux of major species from C to Fe at the end of 2009 was each 20 – 26% greater than in 1997-1998 (ACE news N 134, October 7, 2010). Interplanetary magnetic field strength was 39% lower; solar wind dynamic pressure was 40% less due to reduced solar wind density. These significant changes in major heliophysical parameters have their reflection in geophysical parameters and, therefore in terrestrial climate. Therefore, the monitoring of the solar activity and first

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solar modulation effects on the ambient population of the galactic cosmic rays is very important for the expected climate changes. At ASEC we detect first in recent years geomagnetic and Forbush effects in 2010.

Figure 3The Intensity of the cosmic ray flux (secondary neutrons registered by the Nor Amberd and Izmiran neutron monitors) during exceptionally long 23rd solar activity cycle. There are no signs yet of decreasing of cosmic ray flux – an indicator of the start of new solar cycle.

The first Geomagnetic Effect was detected at Aragats in spring 2010. The geomagnetic storm began at 08:55 UT on Monday, April 5, 2010. Space weather storm level reached Strong (G3) level according to the NOAA geomagnetic storms space weather scale. The source of the storming is an Earth-directed coronal mass ejection (CME) associated with a weak solar flare that occurred in active region AR 1059 on April 3 at 08:54 UT. The severity of the geomagnetic storm was Kp = 7 on the 0-to-9 Kp index scale of magnetic disturbances.

Figure 4The 2.5% count rate increase of the Nor Amberd neutron Monitor inverse correlated in time with the minimum of the geomagnetic field strength measured by the Nor Amberd magnetometer.

As we can see in the Figure 5 during minimum of the geomagnetic field strength (measured by '' LEMI-018 magnetometer) additional Galactic Cosmic Rays enter the atmosphere producing some extra protons and neutrons in interactions with terrestrial atmosphere. Some of these secondary nucleons reach mountain altitudes and falling on the Nor-Amberd Neutron Monitor (NM) enlarging the count rate by 2.5%.A bit bigger peak was detected by the Aragats NM, at altitude 3200 m, 1200 m above the Nor Amberd NM. Other ASEC detectors are sensitive to the higher energies of primary particles and decrease of the geomagnetic field did not change their count rate. The NMs are sensitive to energies just above the cutoff rigidity; therefore decrease of cutoff rigidity leads to increase of count rate Another sign of renewed solar activity was detected at 3 August. A shock detected by the Ace Spacecraft indicated the arrival of at least one CME caused by the long duration C3 flare on August 1.

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Figure 5Geomagnetic storm (planetary DST index) and count rates of Aragats and Alma-Ati (AATB) Neutron Monitors

Arrived magnetised plazma cloud unleash a Forbush decrese (Fd) detected by Aragats and Nor Amberd NMs as well as by Alma-Ati NM (see Figure 6, the “deepness” of Fd is 1.5 – 2.5%) located at approximately same latitude and altitude as Aragts monitors. Figures 4-6 illustrates that ASEC monitors are ready to register all solar modulation events of started 24th solar activity cycle. During long lasting quiet sun the parameters of the ASEC detectors were calculated and checked. Recently (Interactions News Wire #02-09, 21 January 2009, http://www.interactions.org) the major particle physics experiment MINOS (managed by the Fermi National Accelerator Laboratory) in a disused iron-mine in the Minnesota observed strong correlation of the high energy muon flux and stratospheric temperature. In turn the stratospheric temperature correlates with a major weather event, known as a Sudden Stratospheric Warming. On average, these occur every other year and are notoriously unpredictable. This study has shown, for the first time that cosmic-ray data can be used effectively to identify these events. For exploring the connections between muon flux and temperature in the stratosphere for both climate and space weather studies we plan to install muon detectors in the low-background laboratory of YerPhI, located at the depth of 660 m water equivalent in Yerevan salt mine. This laboratory has such an important advantage, compared to known underground laboratories, as it is located in the precincts of a large city with corresponding infrastructure and communication system. It should be mentioned also, that the natural conditions in the mine (the humidity is about 35%, temperature 20-21 C) are very comfortable both for people and electronic devices. It’s well known also, that the natural background in salt mines is exceptionally low. Reference

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