UDC 537.591
Sokurov
V.F.
Research of a stream of cosmic rays
a radar-tracking method
Getting in an atmosphere of
the Earth, space beams generate a stream of secondary radiation, investigating
which, it is possible to receive the objective information on a spectrum of
primary radiation.
• The purpose of work: Studying of a stream of electromagnetic
flashes in an atmosphere from particles ultrahigh ýíåðãèé.
• Research problems:
To analyse
effective methods of registration of particles ultrahigh ýíåðãèé.
In work [1] the method of radar-tracking sounding trace EAS is applied. Range of a
location allows to create the area of registration exceeding the area of
existing largest installations of the world, i.e. from above than on the order
to expand a power range of measurement of a spectrum of primary particles.
However, a plenty of electric categories in an atmosphere have not allowed to
apply this method.
In the present work radar-tracking sounding relativistic disk EAS is considered. Selection of the reflected pulse is
carried out on Doppler-shift of frequency of the
signal reflected from a disk. The size of shift is characterized by the
projection of a vector of speed of a disk directed on the observer: v =
│V•sin θ│ (1).
In laboratory system of readout frequency of electromagnetic
fluctuations on an input of the reception device is received from
transformations Lorrenc for time coordinate
of a four-vector: , (2).
Where f ' - frequency in system of the center of weights; φ - an azimuthal
corner. Having substituted (1) in (2) and taking into account, that v~c, we
shall receive
. (3)
Dependence of the attitude(relation) f/f ' from an azimuthal
corner has been designed for various antiaircraft corners. As a result of the
analysis of the settlement data the conclusion is made, that the probability of
selection of a pulse - handicap, for example, from meteoric front of
ionization, exists for antiaircraft corners ØÀË θ ≈ 10-2-10-3
degrees and makes Ð ≈
10-4-10-6.
At calculation of äîïïëåð-shift the factor of
reflection was accepted equal ≈ 1.
Where ωý = 5,6•104 • plasma frequency e- disk EAS (nå - concentration e- in a disk); ω - angular
frequency of radiation of an electromagnetic signal.
Performance of this equality is possible at a choice of the certain
frequency of radiation f/f ' for some threshold of plasma frequency ωý.
Apparently from (4), plasma frequency ωý depends on
concentration e- in disk. Let's
analyse change of concentration ýëåêòðîíîâ in disk EAS with energy of a primary particle and we shall
establish its threshold energy at which equality (4) would be carried out.
Concentration ýëåêòðîíîâ in
disk EAS with change of distance from an axis is definedby
spatial distribution ýëåêòðîíîâ EAS and can be received from expression: (5).
Where I size of linear ionization of a relativistic particle; f (r)
function of spatial distribution of particles EAS.
Let's consider change of factor of reflection of a disk a primary
particle and various frequencies of electromagnetic radiation of a locator.
As a result of a variation of frequencies of radiation of a locator the
optimal appeared value of frequency a signal . For this value
change of factor of reflection is received depending on concentration e- disk EAS.
As a result of the lead calculations the conclusion is made, that for
the set frequency of radiation value of factor of reflection is close to unit
for downpours with . It enables to
calculate amplitude of the reflected signal from a relativistic disk of a
downpour of the specified energy.
Density of a stream of the electromagnetic energy reflected from disk
EAS:
,
Where - density of a stream of the radiated energy,
Ω - a solid angle of the purpose, sr; Sîòð - the effective area of reflection, m2; r -
distance from the purpose, m; Ω ’ - a corner of the review of the aerial, ñð; R - factor of
reflection.
As the density of particles ØÀË on the fixed
distance is proportional to full number of particles EAS, and consequently, and
energy of a primary particle [2,3] the
effective area of reflection will characterize energy of a primary particle on
dependence . From here it is visible, that energy of a
primary particle is proportional to the module of intensity of an electric
field of the reflected wave: E0~EV. .
1.Suga TO Methods for Observing Extremely Large Extensive Air
Showers // Proc. Fifth Intern. Seminar on Cosmic Rays.-1962.-Vol. 2.-P. 49.
2. Åôèìîâ Í.Í., Ïðàâäèí Ì.È., Õðèñòèàíñåí Ã.Á. Ïðè÷èíû ðàñõîæäåíèÿ ñïåêòðîâ ρ6îî , èçìåðåííûõ â ßêóòñêå è Õàâåðà Ïàðêå //
Èññëåäîâàíèÿ ïî ôè çèêå êîñìè÷åñêèõ ëó÷åé.—ßêóòñê: ßÔ ÑÎ ÀÍ
ÑÑÑÐ, 1985.—Ñ. 19—23.
3. Ñîêóðîâ Â.Ô. Ýêñïåðèìåíòàëüíûå
èññëåäîâàíèÿ ðàäèàöèîííûõ ïðîöåññîâ â àòìîñôåðå Çåìëè. Ìîíîãðàôèÿ // – Ðîñòîâ íà Äîíó: Èçä. ÞÔÓ.
2009, 239ñ.