69 research outputs found
Lateral distribution of radio signal measured in showers with energy 5*10^16-10^18 eV at the Yakutsk EAS array
We present of measurements of radio emission from EAS at the frequency 32 MHz
performed in 2008-2012. Showers were selected by zenith and azimuth directions,
sampled by energy. A mean lateral distribution function was fitted to the data
each interval. The paper presents unied approximation formula for all three
energy intervals of lateral distribution, using connection between equation (1)
and (2) coefficients with energy and geomagnetic angle. Here we analyze the
connection between the shape of lateral distribution and the depth of the
maximum shower development Xmax too.Comment: 33rd International Cosmic Ray Conference, Rio de Janeiro, Brazil,
July 201
Correlation of AOT with Relative Frequency of Air Showers with energy 10^{15} - 10^{16} eV by Yakutsk Data
Long-term series of measurement of spectral transparency of the atmosphere
(\lambda = 430 nm) and atmospheric optical thickness (AOT) measured by
multimode photometer CE 318 in the region of Yakutsk array are analyzed.
Correlation of AOT with intensity of air showers with small energies 10^{15} -
10^{16} eV is found. The variability of aerosol composition of the atmosphere
during the registration period of the Cherenkov light should be taken into
account since it may affect the quality of determining characteristics of air
showers.Comment: XXV ECRS 2016 Proceedings - eConf C16-09-04.
The depth of maximum shower development and its fluctuations: cosmic ray mass composition at E_0 >= 10^17 eV
We present new data on Cherenkov light observations obtained during the
period 1994-2009, after a modernization of the Yakutsk EAS array. A complex
analysis of \xmax and its fluctuations \sigma(\xmax) was performed over a
wide energy range. With the new data, according to QGSJet II model, an
estimation was made of the cosmic ray mass composition for \E \sim 10^{17} - 3
\times 10^{19} eV. The result points towards a mixed composition with a large
portion of heavy nuclei at \E \sim 10^{17} eV and the dominance of light
nuclei at \E \sim 10^{19} eV. The analysis of \sigma(\xmax) energy
dependence for the same energies qualitatively confirms this result. The shape
of the \xmax distribution at fixed energy eV is analysed to make
more precise conclusions on cosmic ray mass composition.Comment: Contributed paper to the XVI International Symposium on Very High
Energy Cosmic Ray Interactions ISVHECRI 2010, Batavia, IL, USA (28 June - 2
July 2010). 4 pages, 5 figure
Spectrum and mass composition of cosmic rays in the energy range 10^15-10^18 eV derived from the Yakutsk array data
A spectrum of cosmic rays within energy range 10^15 - 3x10^17 eV was derived
from the data of the small Cherenkov setup, which is a part of the Yakutsk
complex EAS array. In this, work a new series of observation is covered. These
observations lasted from 2000 till 2010 and resulted in increased number of
registered events within interval 10^16 - 10^18 eV, which in turn made it
possible to reproduce cosmic ray spectrum in this energy domain with better
precision. A sign of a thin structure is observed in the shape of the spectrum.
It could be related to the escape of heavy nuclei from our Galaxy. Cosmic ray
mass composition was obtained for the energy region 10^16 - 10^18 eV. A joint
analysis of spectrum and mass composition of cosmic rays was performed.
Obtained results are considered in the context of theoretical computations that
were performed with the use of hypothesis of galactic and meta-galactic origin
of cosmic rays.Comment: Proc. 32nd ICRC, Aug.11-18, Beijing, Chin
The nature of pulses delayed by 5 mcs in scintillation detectors from showers with the energy above 1E17 eV
Here we consider EAS events with energy above 1E17 eV with recorded pulses
delayed by t>=5 mcs in scintillation detectors with different thresholds: 10, 5
and 1.8 MeV. In order to identify pulses from electrons, muons and neutrons,
experimental data were compared to computational results performed within the
framework of QGSJET01d model. Preliminary, one may speculate of registration of
low-energy electrons arisen from moderation of neutrons in a detector or a
medium surrounding a detector or in the snow cover and frozen crust (albedo
particles). The fact that such pulses were registered mostly in low-threshold
detectors confirms this hypothesis.Comment: Proc. of the 33rd ICRC (2013), Rio de Janeiro, Brazi
Air shower registration algorithm and mathematical processing of showers with radio signal at the Yakutsk array
The paper describes the techniques and method of registration of air shower
radio emission at the Yakutsk array of extensive air showers at a frequency of
32 MHz. At this stage, emission registration involves two set of antennas, the
distance between them is 500m. One set involves 8 antennas, second - 4
antennas. The antennas are perpendicularly crossed dipoles with radiation
pattern North South,West East and raised 1.5 m above the ground. Each set of
antennas connected to an industrial PC. The registration requires one of two
triggers. First trigger are generated by scintillation detectors of Yakutsk
array. Scintillation detectors cover area of 12 km^2 and registers air showers
with energy more than 10^17 eV. The second trigger is generated by Small
Cherenkov Array that covers area of 1 km^2 and registers air showers with
energy 10^15 - 5*10^17 eV. Small Cherenkov Array is part of Yakutsk array and
involve Cherenkov detectors located at a distance of 50, 100, 250 m. For
further selection we are using an additional criterion the radio pulse must be
localized in the area corresponding to the delay time on first and second
triggers. In addition, descriptions of the algorithm and the flowcharts of the
program for the air shower selection and further analysis are given. This
method registers EAS radio emission with energy 10^16 - 10^19 eV. With the
absolute calibration, the amplitudes of all antennas converted to a single
value. Air shower radio emission dependences from zenith angle and shower
energy are plotted.Comment: Contributions to the 33rd International Cosmic Ray Conference, Rio de
Janeiro, Brazil, July 201
Radio emission of air showers with extremely high energy measured by the Yakutsk radio array
The Yakutsk Array is designed to study cosmic rays at energy
10-10 eV. It consists several independent arrays that register
charged particles, muons with energy E1 GeV, Cherenkov light and radio
emission. The paper presents a technical description of the Yakutsk Radio Array
and some preliminary results obtained from measurements of radio emission at
30-35 MHz frequency induced by air shower particles with energy
110 eV. The data obtained at the Yakutsk array in
1986-1989 (first set of measurements) and 2009-2014 (new set of measurements).
Based on the obtained results we determined:
Lateral distribution function (LDF) of air showers radio emission with energy
10 eV. Radio emission amplitude empirical connection with air
shower energy. Determination of depth of maximum by the ratio of amplitude at
different distances from the shower axis. For the first time, at the Yakutsk
array, radio emission from the air shower with energy 10 eV was
registered including the shower with the highest energy ever registered at the
Yakutsk array with energy 2 10 eV.Comment: 11 pages, 20 figures, 2 tables, accepted for publication in NIM A.
arXiv admin note: text overlap with arXiv:1609.0327
The energy spectrum of cosmic rays above 10^15 eV as derived from air Cherenkov light measurements in Yakutsk
The Yakutsk array observes the Cherenkov light emitted by UHECR in
atmosphere. Recently, an autonomous subarray is added consisting of
photomultipliers to measure the showers in the knee region. Our aim is to
analyze the combined data set in order to derive the cosmic ray spectrum in the
energy range as wide as possible using the same technique.
The advantage of the air Cherenkov light measurement is the model independent
estimation of the EAS primary energy using the total light flux emitted in the
atmosphere. A set of the light lateral distributions observed in the extended
energy range is presented also.Comment: 11 pages, 5 figures, submitted to Nuclear Physics B (Proceedings
Supplements
Behavior of some characteristics of EAS in the region of knee and ankle of spectrum
The energy dependence of such characteristics as a ratio of the total number
of charged particles to the total flux of EAS Cherenkov radiation, a ratio of
E(thr)>=1GeV muon flux density at the distance of 600m from a shower core to
charged particle flux density, a ratio of the energy transferred to the
electromagnetic component of EAS to the primary particle energy is presented.
Their comparison with two-component mass composition of cosmic rays (p-Fe) in
the framework of calculations by a QGSJET model is given.Comment: 6 pages, 9 figure
Fluctuations of the depth of maximum in extensive air showers and cross-section of p-air inelastic interaction for energy range 10^15-10^17 eV
We present estimation of proton-air inelastic interaction cross-section
obtained for different energy values are. Results are compared with different
hadron interaction models.Comment: Proc. 32nd ICRC, Aug. 11-18, Beijing, Chin
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