ИСТИНА

Neutron monitors Baksan (Northern Caucasus, 42 N), Apatity (67 N) and Barentsburg (arch. Spitsbergen, 78 N) have an advanced data acquisition system. The system records each neutron monitor’s (NM) pulse: which tube produced the pulse and what time, with one microsecond accuracy. The system is used to study multiplicity events on NM. The multiplicity is characterized by the number of M pulses (neutrons). A multiplicity event is clearly distinct: at an average interval between pulses is ~22 ms on an NM the intervals between pulses inside an M event are 10-200 mcs and number of pulses M = 5-200. The multiplicity is two kinds: multiplicity into NM (M = 5-10) and in the atmosphere (M = 10-200). The second kind corresponds to coming in the atmosphere a particle with very high energy from hundreds GeV and more. After upgrading the acquisition system of the monitors are connected to the universal time with accuracy less than 1 mcs. Now three NMs are like one distributed detector. It is found a long sequence of multiplicity events (15-40 events during ~20 seconds) after processing the data. An average time profile and spectrum of multiplicity are derived. Time profile shows a gap before and after the sequence with low number of multiplicity events. Frequency of such sequences is two orders more than usual fluctuation. Furthermore, a part of the long sequences of multiplicity are simultaneously on two or three NMs. We consider it to be detected by the neutron monitors quick surges (or clusters) of density in the high-energy particle flux. Larmour radius of 1 TeV particle in the interplanetary magnetic field is compatible to heliosphere size. In this case large scale irregularities of the interplanetary magnetic field could produce such surges. Using a wide net of NMs and solving inversed problem one could derive large scale structure of heliosphere.