Investigation of radio-emission from extensive air shower at high mountain cosmic ray station at an altitude of 3340 m above sea level

M Nassurlla,A.I Zhumabayev,A.D Beisenova,T.Kh Sadykov,T Idrisova,A Haungs,B.A Iskakov,N.M Salikhov,O.A Novolodskaya,M.B Khabargeldina

doi:10.29317/ejpfm.2019030305

Abstract

The complex EAS installation of the Tien Shan mountain cosmic ray station which is situated at a height of 3340 m above sea level includes the scintillation and Cherenkov detectors of charged shower particles, an ionization calorimeter and a set of neutron detectors for registering the hadronic component of the shower, and a number of underground detectors of the penetrative EAS component. Now it is intended to expand this installation with a promising method for detecting the radio-emission generated by the particles of the developing shower. The facility for radio-emission detection consists of a three crossed dipole antennae, one being set vertically, and another two - mutually perpendicularly in a horizontal plane, all of them being connected to a three-channel radio-frequency ampliﬁer of German production. By the passage of an extensive air shower, which is deﬁned by a scintillation shower detector system, the output signal of antenna ampliﬁer is digitized by a fast multichannel DT5720 ADC of Italian production, and kept within computer memory. The further analysis of the detected signal anticipates its operation according to a special algorithm and a search for the pulse of radio-emission from the shower. A functional test of the radio-installation is made with artiﬁcial signals which imitate those of the shower, and with the use of a N1996A type wave analyzer of Agilent Technologies production. We present preliminary results on the registration of extensive air shower emission at the Tien Shan installation which were collected during test measurements.

Highlights

The registration of radio-emission generated by particles of high-energy extensive air showers (EAS) has a number of advantages over other methods of primary cosmic ray investigation, both of which are based on direct registration of shower particles, and the methods connected with the registration of Cherenkov and fluorescent EAS emissions in ultraviolet and optic diapasons
Every one of the shown distributions is registered with a 4 ns temporal resolution and consists of 10000 sequential measurements of signal intensity which correspond to the full duration of the measured time series of 40 μs
All distributions are centered relative to the arrival time of the EAS trigger which came from the scintillation shower system; the leading 20 μs in every time series corresponds to the ’prehistory’ of the radio-signal which precedes the EAS time, and the 20 μs describe the time behavior of the radio-signal after the passage of the shower front through the antennae system

Summary

Introduction

The registration of radio-emission generated by particles of high-energy extensive air showers (EAS) has a number of advantages over other methods of primary cosmic ray investigation, both of which are based on direct registration of shower particles (a relative simple and cheap radio-detector system compared with wide-spread electronic detector systems, the large spatial volume of the space controlled by a single radio antenna, a sensitivity to the characteristics of longitudinal EAS development), and the methods connected with the registration of Cherenkov and fluorescent EAS emissions in ultraviolet and optic diapasons (an unrestricted duty cycle of radio installation which is independent of daytime and weather conditions). A convenient place for the development of the radio-method of EAS particle registration is the Tien Shan mountain cosmic ray station (43 ◦ 15‘ N, 76 ◦ 57‘ E, 3340 m above sea level) whose installations for the complex EAS investigation in the range of primary energies of (10 14 - 10 18 ) eV permit both a direct detection of the charged shower particles [6] at the station’s level, and registration of Cherenkov light emitted above in atmosphere [7].

Results

Conclusion