TGE terminated by lightning at the maximum of the flux; red disturbances of electrostatic field; blue distance to lightning (~2 km); green small circles are the codes (density of particles) of MAKET-16 array. We expect TGE flux maximum at maximal electric field in cloud and, therefore, at maximal LPCR. Maximal LPCR prevents CG (Nag and Rakov, 2009); thus we expect TGE termination only on beginning and decaying stages, but we have equal events at maximum: so we come to contradiction.
Do lightnings follow EAS path? Neutrons in Atmosphere How to explain TGE termination at maximum of flux (remote lightning at thin LPCR, or EAS-RB effect Gurevich et al., 1999)? Try to detect simultaneously EAS and lightning (need precise timing!) Neutron monitor as EAS core detector; One-second time series of ArNM with 400 ns dead time; Long-leaving particles in NM and Muon detectors; Huge neutrons multiplicities detected at Aragats; Prisma project and its clones; Detection of the EAS core with nanosecond time scales; Neutrons from the lightning bolt? Detection of neutrons from photonuclear reactions in atmosphere and lead.
Model of the thundercloud: occasionally emerging radiation emitting regions in the bottom of the cloud; LPCR play major role in TGE initiation
1 s e c t i o
NM is sensitive also to gamma rays! The resulting detection efficiency of a NM-64 for 6 different particle species including neutrons, protons, positive and negative pions and muons for vertical incident direction. It quite clear from this figure that the detector's response is optimized to measure the hadronic component as muons above 1 GeV is more 3 orders of magnitude less than the hadrons. Energies below 1GeV stopping negative charge muons (or pions) are captured by a lead nucleus into a mesic orbit and absorbed by a nucleus which de-excites of the nucleus through the emission of neutrons which is reflected in the rise in detection efficiency with decreasing energy.
NM operation The Lead Producer, which surrounds the moderator, provides a thick large-nucleus target for incident particles. A large nucleus such as lead is preferred as the neutron production rate per unit mass of a material is roughly proportional to A 0.7. Inelastic interactions can separated into 2 stages: De-excitation phase: Wounded target nucleus ejects neutrons spectrum peaked near 1.0~MeV (evaporation neutrons). Source of counts in the proportional tubes. Thermalized neutrons enter the sensitive volume of the boron counter SNM15 and produce alpha particle by reaction: n( 10 B, 7 Li)α (30% efficiency); the alternate reaction used in helium SNM18 counters is n( 3 He, 3 H)p (80% efficiency)
Secondary Cosmic Rays Shower particles Electromagnetic (electrons, gamma rays) Pions, muons, neutrons, protons Can travel faster than the speed of light in air (they are still slower than the speed of light in vacuum) 150 muons are striking every square meter of the Earth every second You are bombarded with these particles every day! Not all shower particles reach the ground the atmosphere blocks some
A picture from Hayakawa manual (1973): What happens when EAS core hits the It s a nice picture but it contains an error: ground? The question is what will happen in this point??? Yu. V. Stenkin, Baikal'2012
ArNM dead times 0.4μs (black- neutron bursts from EAS); 250μs (blue); 1250μs (red, suppression of EAS, one-to-one relation of incident high energy hadrons and NM counts)
ArNM : 11 operating channels (dead time 400 ns); in 1 ms each tube can count 2500 signals. It can be seen in 1-sec time series (mean value 10-60, sum of 11 300-400).
3 Layers of Muon detector, 3-cm thick scintillator of STAND1 and coincidences of MUON scintillators
Channels of NM demonstrate that EAS hit the detector at 13-14 tube region
Ever largest peak in ArNM (400 ns dead time) Name Mean σ Min Max Dead time 0.4us 381.63 26.1 339 (-1.63σ) 6350 (228.52σ) Dead time 250us 342.54 22.16 297 (-2.05σ) 455 (5.07σ) Dead time 1250us 305.71 17.33 266 (-2.29σ) 358 (3.02σ)
Note large peaks in the failure channels (7,13,16) can t be accepted as genuine event!
Large peak in ArNM, no lightning Name Mean σ Min Max Dead time 0.4us 482.78 32.03 406 (-2.4σ) 1660 (36.69σ) Dead time 250us 431.86 24.48 372 (-2.45σ) 484 (2.13σ) Dead time 1250us 385.81 19.27 336 (-2.58σ) 435 (2.55σ
EAS Table 1 hit 1 section of ArNM (counters 3 and 4) Table 2 Name Mean σ Min Max ArNM #3 45.54 8.78 30 (-1.77σ) 256 (23.98σ) ArNM #4 47.76 8.63 29 (-2.17σ) 230 (21.12σ) ArNM #8 62.64 11.07 35 (-2.5σ) 125 (5.63σ) ArNM #9 64.47 9.47 45 (-2.06σ) 99 (3.64σ) ArNM #13 22.36 5.37 12 (-1.93σ) 44 (4.03σ) ArNM #14 39.61 8.44 25 (-1.73σ) 64 (2.89σ) ArNM #16 25.14 5.13 14 (-2.17σ) 36 (2.12σ) ArNM #17 40 7.52 26 (-1.86σ) 57 (2.26σ) Table 3 Table 4
Coinciding detection of EAS by ArNM. and Muon detector Name Mean σ Min Max Dead time 0.4μs 338.47 27.37 276 (-2.28σ) 2060 (62.72σ) Dead time 250μs 307.03 22.55 250 (-2.53σ) 440 (5.9σ) Dead time 1250μs 278.63 19.19 230 (-2.53σ) 337 (3.04σ) 3cm scint. 7.5cm Lead 261.95 13.58 232 (-2.21σ) 541 (20.56σ) 1cm scint. 9cm Lead 178.97 12.9 156 (-1.78σ) 390 (16.35σ) 1cm scint. 15cm Lead 125.27 11.12 92 (-2.99σ) 313 (16.88σ) 3cm thick scintillator 478.83 18.74 440 (-2.07σ) 479(0.01σ) Coinc. of Muon scint. 4.9 2.36 1 (-1.65σ) 47 (17.87σ) ID Table 1
Knee
Can we confirm EAS-RB model by detected 2 coincidences? Not yet, precise timing required to avoid interferences!
EM interference in MAKET myrio channels gives another time stamp of lightning MAKET Muon detector lightnings at 14:45:07.043 Abrupt increase of near surface electric field 14:45:07.293 Nanosecond pulses from fast wave forms at 7:001 and 7:006 So, Muon detector peaks are coherent with fast waveforms!
A prototype of PRISMA (the ProtoPrisma array) 16 en-detectors Location: on 4th floor inside building in MEPhI, Moscow Yu. V. Stenkin, Baikal'2012
Neutron lateral distribution 100 n e -R/6.7m 10 0 10 20 30 R, m
Tibet (YBJ) Prisma prototype PRISMA YBJ pro (2013)
LHAASO Project: -astronomy and origin of CR LHAASO is very powerful array Large High Altitude Air Shower But, it had no hadron detectors Observatory PRISMA Core Det ect or Array Yu. V. Stenkin, Baikal'2012
Layout of the detectors at the Tian-Shan mountain station Anomalous time structure of EAS particle flows in the knee region of primary cosmic ray spectrum 253
L G Sveshnikova, A P Chubenko, V I Galkin, R A Mukhamedshin, N M Nikolskaya and V I Yakovlev, On absorption of the hadron component of EAS cores in a large lead calorimeter at knee -range energies, J. Phys. G: Nucl. Part. Phys. 35 (2008) Generation probability of the high multiplicity neutron events (M > 1000) by EAS of various sizes Ne. Figure The arrow 4. Correlation marks the plot position between of the the knee total in neutron the shower multiplicity size spectrum. M and The (a) lateral the size an size of core this region distance seems of theto accompanying be of the order EAS. of the (c) distances Generation between probability the monitor of the high units multiplicity in our experiment, events i.e. (M of > the 1000) order by of EAS 3 5 of m. various sizes N e. The arrow marks the position of the kn
EAS core detection by the neutron content EAS core is very poor investigated till now. EM (electron, muons, gamma rays) species of EAS core are excluded from analysis; Hadron calorimeters are expensive and rare; Neutron content of EAS is proxy of hadron content (20-25% of hadron energy is transformed to neutrons); Neutrons is easier to detect; Precise timing of neutron and muon species can provide interesting information on high energy interactions above LHC energies.
EAS core research with 3 channels: neutrons, high energy muons and low energy electrons on nanosecond time scales
Atmospheric neutrons Gulmarg (Himalaya) claim neutrons from the thunderbolts; Tien Shan also claim neutrons from the thunderbolts; Aragats detect neutrons from photonuclear reactions in atmosphere; Tibet demonstrate that photonuclear reaction could be also in the lead of NM.
Huge excess in ArrNM and SEVAN detectors: neutrons and gamma rays!
Detection of TGE neutrons
At 4 October 2010 the lightning activity during TGE was small
Count rate of neutrons, gamma rays and muons (%) 14N ;n 13N. Neutrons born in Atmosphère from the TGE gamma rays 14 N(γ,n) 13 N 10 28 March, 2009 9 8 7 6 5 4 3 2 1 0-1 -2-3 -4 13:30 13:35 13:40 13:45 13:50 UT NAMMM(gamma rays) NAMMM(muons) NANM (neutrons)
H. Tsuchiya, et al., PHYSICAL REVIEW D 85, 092006 (2012) Observation of thundercloud-related gamma rays and neutrons in Tibet Points with 1σ error bars in panels (a) and (b) correspond to the variations in YBJ NM and >40 MeV SNT
Gurevich, A.V., V. P. Antonova, A. P. Chubenko, A. N. Karashtin, G. G. Mitko, M. O. Ptitsyn, V. A. Ryabov, A. L. Shepetov, Yu.V. Shlyugaev, L. I. Vildanova, and K. P. Zybin, Strong Flux of Low-Energy Neutrons Produced by Thunderstorms (2012), Phys. Rev. Lett. 108, 125001. 2H + 2H n + 3He.
Strong Flux of Low-Energy Neutrons Produced by Thunderstorms Commercializing a next-generation source of CLENR energy New evidence for low energy neutron fluxes in lightning - V Data consistent with WLS many-body collective magnetic mechanism Conceptual schematic of Gurevich et al. s experimental setup Neutrons created in lightning channels 2 mm thick roofing iron ceiling Neutrons created in lightning channels 20 cm thick Carbon layer Simple plywood enclosure to protect external TND from elements (15 m away from other two TND detectors) Field mill electrostatic flux meter Capacitor sensor Internal 3 He(n, p)t thermal neutron detector (TND) 18NM64 type neutron supermonitor 4 cm thick wooden floor 3 cm thick rubber Under floor TND April 4, 2012 Copyright 2012, Lattice Energy LLC All Rights Reserved 28 1-minue time series counted in external, internal, and underfloor neutron detectors; the multiplied by 0.001 minutely pulse numbers in the supermonitor NM64; the strength of the local electric field in kv=m. A.V.Gurevich et. Al., PRL 108, 125001 (2012)
Commercializing a next-generation source of CLENR energy Low Energy Nuclear Reactions (LENRs) New neutron data consistent with WLS mechanism in lightning Surprisingly large fluxes of low-energy neutrons well-correlated with thunderstorm EMF fluctuations Multiple Lightning Bolts Technical Overview Lewis Larsen President and CEO Lattice Energy LLC April 4, 2012 It is of the highest importance in the art of detection to be able to recognize, out of a number of facts, which are incidental and which vital. Otherwise your energy and attention must be dissipated instead of being concentrated. Sherlock Holmes, "The Reigate Squires 1893 Single Lightning Bolt e - * + p + n + ν e e - + p + lepton + X Nuclear reactions n + (Z, A) (Z, A+1) (Z, A+1) (Z + 1, A+1) + e - β + ν e Beta - decay of neutron-rich products e - * + p + n + ν e e - + p + lepton + X Nuclear reactions April 4, 2012 Copyright 2012, Lattice Energy LLC All Rights Reserved 1
Origin of TGE neutrons (photonuclear reactions: in lead or in atmosphere) 14 N(γ,n) 13 N Detection efficiency of a NM64 for neutrons, rays, electrons, and positrons, as determined by the GEANT4 simulation.
Babich et al., conclusion Proceeding from the efficiency and size of the external 3He counter and recorded count rates, Chilingarian et al. recovered a flux (1/m 2 min) of thermal neutrons (0.01-1 ev) incident the external counter. Than with the corresponding values of the flux they, using the GEANT4 Monte Carlo code, simulated transport of thermal neutrons through the iron and carbon layers and calculated the flux of neutrons incident the internal 3He counter, which appeared to be 5-11 times less than the flux following from count rates of the internal counter in [Gurevich et al.,chilingarian et al. calculated that the neutron flux at the internal10b(n;4he, )7Li monitor [Gurevich et al., 2012] appeared to be 44-117 times less than the flux following from the count rates reported by Gurevich et al At Aragats [Chilingarian et al. 2010; 2012a; 2012b] the positive result is substantiated by the configuration of the observations, in which high-energy electrons, gamma-rays and neutrons were simultaneously detected. As for the high energies 10-30 MeV, the only work where the flux of the gammaray emission during thunderstorms was measured from the ground is the paper of Chilingarian et al. [2010]; L. P. Babich, E. I. Bochkov, J. R. Dwyer et al., J. Geophys. Res.: Space Phys. 118, 1 (2013).
H.Tsuchiya,K.Hibino,K.Kawata e tal., Phys.Rev.D85, 092006 (2012). Tsuchiya et al., conclusion In other available communications [Shyam and Kaushik, 1999; Kuzhewski, 2004; Bratolyubova-Tsulukidze et al., 2004; Martin et al. 2009a; 2009b; 2010; Gurevich et al., 2012; Starodubtsev et al., 2012] the observations of thunderstorm related neutrons unfortunately are not substantiated at all, because observed increases of neutron detectors count rates could be caused by x - and gamma rays [Tsuchiya et al., 2012]; Tsuchiya et al. [2012] based on results of Monte Carlo simulations of their own high-mountainous (4300 m) experiment claim, that...not neutrons but gamma rays may possibly dominate enhancements detected by the Aragats neutron monitor... [Chilingarian et al., 2010] and their conclusion that...world-wide networks of neutron monitors... and solar neutron telescopes... are useful for observations thunderstorm-related -ray emissions, are fully justified.
Gulmarg conclusion In order to unambiguously establish the neutron enhancement origination in thunder- storm atmosphere by surface detectors, it is rightly believed to have a multivariate data acquisition facility to measure simultaneously all the neutral and charged species of the secondary cosmic rays, x-rays, gamma rays, lightning detection, electrical field parameters, optical monitoring of the skies with fast cameras within an observation time window spreading over several milliseconds on either side of the occurrence of an NALD to reliably infer the source of neutron enhancement. In addition, a monitoring system incorporating mostly optical fibers for transmission of signals can go a long way in helping to eliminate the doubt of pickup due to strong x-rays, gamma rays, EMPs occurring in sync with lightning bolts as neutron signal.
No evidence of lightning neutron production was observed duringin MEPhI, MSU, Obninsk, Baksan and Gran Sasso (V. Alekseenko, et al., PRL 114, 125003 (2015) Neutron signal ZnS(Ag) has several scintillation time constants Charged particle signal Lightning interference 22μs
Amplitude, mv 600 400 200 0-200 -400-600 0 0.5 1 1.5 2 Time relative to trigger, ms Fast Waveforms of atmospheric discharges Nor Amberd Neutron Monitor 1-sec time series; dead time 400 ns