Operation of the Space Environmental viewing and Analysis Network (Sevan) in 24-th Solar Activity Cycle A. Chilingarian A. Chilingarian Yerevan Physics.

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Presentation transcript:

Operation of the Space Environmental viewing and Analysis Network (Sevan) in 24-th Solar Activity Cycle A. Chilingarian A. Chilingarian Yerevan Physics Institute, Yerevan, Armenia, Alikhanyan Brothers 2, Yerevan , Armenia,

100 – traversal of the low energy charged particle (<100MeV); 010 – traversal of the neutral particle; 111, 101 – traversal of the high energy muon (>250, 200MeV); Design of the SEVAN basic unit

SEVAN home page:

Starting of SEVANs in Bulgaria and Croatia

Modulation of Galactic Cosmic Rays

Selection of Secondary Cosmic Rays

Purity-Efficiency Diagram

SEVAN Count Rates Aragats 3200 a.s.l. ArNM 18NM64 SEVAN [100] SEVAN [010] SEVAN [111] Relative Error /sqrt(N) YerPhI (1200m)NorAmberd (2000m)Aragats (3200m) Zagreb, Croatia (130m) Moussala, Bulgaria, (2925 m) Type of secondary particle Measured count rate Simulated count rate Measured count rate Simul. Measured count rate Simulated count rate Measured Count rate Measured count rate Low energy charged particles (100) 8862± ± ± ± ±136 Neutral particles (010) 363± ± ± ±181115±38 High energy muon (111 & 101) 4337± ± ± ±646315±78

Barometric coefficients, count rates and relative errors of SEVAN monitors Monitor Altitude (m) Rc (Gv) Barometric Coeff. %/mb Correlation Coefficient Count rate [min] Relative error Aragats SEVAN Low energy charged particles (Coincidence 100) ± Aragats SEVAN High energy muons (Coincidence 111+ Coincidence 101) ± Aragats SEVAN neutrons (Coincidence 010) ± Nor Amberd SEVAN Low energy charged particles (Coincidence 100) ± Nor Amberd SEVAN High energy muons (Coincidence 111+ Coincidence 101) ± Nor Amberd SEVAN neutrons (Coincidence 010) ± Yerevan SEVAN Low energy charged particles (Coincidence 100) ± SEVAN High energy muons (Coincidence 111+ Coincidence 101) ± Yerevan SEVAN neutrons (Coincidence 010) ±

2 types of GLE detected by the SEVAN basic unit (simulation) Detector LayerSolar ProtonsSolar Neutrons Upper 5cm scintillator4.8σ2.6σ Middle 25 cm scintillator1.7σ6.4σ 5min simulated enhancements in the Upper and Middle layers of the SEVAN basic unit.

Space Weather alerts: SEVAN can estimate on-line Spectral “knees” of Solar CR

High Solar Activity in March 2012

March 2012 Fd: on-line data from all SEVANs and all NMs in:

SEVAN calibration with gamma rays from Thunderstorm Ground Enhancements (TGEs): Electrons born gamma rays and gamma rays – neutrons.

Deficit of high energy muons- positive muons stop: evidence of large potential drop in thundercloud ~5% deficit in muon flux prove existence of large potential drop in thundercloud accelerated electrons in the direction to Earth surface

SEVAN Advantages The hybrid particle detectors, measuring neutral and charged fluxes provide following advantages upon existing detector networks measuring single species of secondary CR: Cheap and simple operation; Probe different populations of primary cosmic rays with rigidities from few GV (neutrons) up to GV (muons); Reconstruct SCR spectra and determine position of the spectral “knees”; Classify GLEs in “neutron” or “proton” initiated events; Significantly enlarge the reliability of Space Weather alerts due to detection of 3 particle fluxes instead of only one in existing neutron monitor and muon telescope world-wide networks. Detect Thunderstorm Ground Enhancements – both electron and gamma ray fluxes