The secondary radiation of the Earth's ionosphere
The modernization of the KLAUDIA radiotelescope, used for the detection of the Earth ionosphere's secondary radiation at 40 kHz±200 Hz waves, is presented in the paper. In particular, the scope of the Very Low Frequency receiver's modernization and the construction of the high frequency gr...
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Advances in astronomy and space physics
2011
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| Цитувати: | The secondary radiation of the Earth's ionosphere / M. Szczesniak, R. Szczesniak, A.P. Durajski, M.W. Jarosik // Advances in Astronomy and Space Physics. — 2011. — Т. 1., вип. 1-2. — С. 65-68. — Бібліогр.: 5 назв. — англ. |
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nasplib_isofts_kiev_ua-123456789-1189752025-02-10T00:17:12Z The secondary radiation of the Earth's ionosphere Szczesniak, M. Szczesniak, R. Durajsk, A.P. Jarosik, M.W. The modernization of the KLAUDIA radiotelescope, used for the detection of the Earth ionosphere's secondary radiation at 40 kHz±200 Hz waves, is presented in the paper. In particular, the scope of the Very Low Frequency receiver's modernization and the construction of the high frequency grounding module is briefly discussed. The most typical features of the radio radiation of the Earth's ionosphere at 40 kHz frequency waves are presented and discussed in detail in the second part of the paper. 2011 Article The secondary radiation of the Earth's ionosphere / M. Szczesniak, R. Szczesniak, A.P. Durajski, M.W. Jarosik // Advances in Astronomy and Space Physics. — 2011. — Т. 1., вип. 1-2. — С. 65-68. — Бібліогр.: 5 назв. — англ. 987-966-439-367-3 https://nasplib.isofts.kiev.ua/handle/123456789/118975 en Advances in Astronomy and Space Physics application/pdf Advances in astronomy and space physics |
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Digital Library of Periodicals of National Academy of Sciences of Ukraine |
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The modernization of the KLAUDIA radiotelescope, used for the detection of the Earth ionosphere's secondary radiation at 40 kHz±200 Hz waves, is presented in the paper. In particular, the scope of the Very Low Frequency receiver's modernization and the construction of the high frequency grounding module is briefly discussed. The most typical features of the radio radiation of the Earth's ionosphere at 40 kHz frequency waves are presented and discussed in detail in the second part of the paper. |
| format |
Article |
| author |
Szczesniak, M. Szczesniak, R. Durajsk, A.P. Jarosik, M.W. |
| spellingShingle |
Szczesniak, M. Szczesniak, R. Durajsk, A.P. Jarosik, M.W. The secondary radiation of the Earth's ionosphere Advances in Astronomy and Space Physics |
| author_facet |
Szczesniak, M. Szczesniak, R. Durajsk, A.P. Jarosik, M.W. |
| author_sort |
Szczesniak, M. |
| title |
The secondary radiation of the Earth's ionosphere |
| title_short |
The secondary radiation of the Earth's ionosphere |
| title_full |
The secondary radiation of the Earth's ionosphere |
| title_fullStr |
The secondary radiation of the Earth's ionosphere |
| title_full_unstemmed |
The secondary radiation of the Earth's ionosphere |
| title_sort |
secondary radiation of the earth's ionosphere |
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Advances in astronomy and space physics |
| publishDate |
2011 |
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https://nasplib.isofts.kiev.ua/handle/123456789/118975 |
| citation_txt |
The secondary radiation of the Earth's ionosphere / M. Szczesniak, R. Szczesniak, A.P. Durajski, M.W. Jarosik // Advances in Astronomy and Space Physics. — 2011. — Т. 1., вип. 1-2. — С. 65-68. — Бібліогр.: 5 назв. — англ. |
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Advances in Astronomy and Space Physics |
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2025-12-02T02:15:56Z |
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2025-12-02T02:15:56Z |
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| fulltext |
The secondary radiation of the Earth's ionosphere
M. Szcz�e�sniak1, R. Szcz�e�sniak2, A. P. Durajski2, M. W. Jarosik2
1Ul. Sªoneczna 44, 34-700 Rabka-Zdrój, Poland
2Institute of Physics, Cz�estochowa University of Technology, Al. Armii Krajowej 19, 42-200 Cz�estochowa, Poland
szczesni@mim.pcz.czest.pl
The modernization of the KLAUDIA radiotelescope, used for the detection of the Earth ionosphere's
secondary radiation at 40 kHz±200 Hz waves, is presented in the paper. In particular, the scope of the
Very Low Frequency receiver's modernization and the construction of the high frequency grounding module
is brie�y discussed. The most typical features of the radio radiation of the Earth's ionosphere at 40 kHz
frequency waves are presented and discussed in detail in the second part of the paper.
The construction and the modernization of the radiotelescope
The radiotelescope KLAUDIA consists of a Very Low Frequency (VLF) receiver supplied with the antenna,
a high frequency grounding module, a stabilized power supply adapter and two PC computers, with a special
software utility named Radio�SkyPipe. It is developed for collecting, processing and visualization of the
collected data.
Produced in the USA, the VLF receiver was designed as a device to work with a Long�Wire (LW) type
antenna [5]. The LW antenna which is non-symmetric and receives the signal at its whole length, is made
up as a single wire, hung in space with one end connected directly to the grounded receiver. The antenna,
made from a non-screened wire, negatively in�uences the quality of the received signal. The part of the
antenna which is inside the building, introduces the distortions that come from the electric and electronic
installations present in the building. The same situation is related to the grounding, which as a second
part of the antenna, receives the signal with all its length too. In order to eliminate harmful disturbances
introduced to the receiver by the antenna and the grounding, the decision to modernize the antenna, the
grounding line and the receiver was made.
At the frequencies below 30 MHz, the so called �skin e�ect� is not important. For that reason, the
antenna which is designed for receiving 40 kHz frequencies, can be generally built from any kind of the
wire. In our case, the receiving part of the antenna, 7.5 m in length, was made up from the steel cord,
1 mm in diameter, brazen in a PCV braid and ended with the ceramic insulators at the binding places. The
antenna guys were made of the silk�polypropylene cord, 4 mm in diameter. The antenna was hung under
the angle of 30 degrees to the ground level for more circular characteristic and increasing its sensitivity to
the signals with horizontal and vertical polarization. The higher end of the antenna was connected to the
voltage symmetrizer, which (without using the antenna tuner) enables the connection of the wired antenna
to receiver with an instrumentation of a RG 6/U coaxial cable (75 Ω wave resistance). The symmetrizer
(balun 9:1), which �ts the high impedance of the antenna to the low impedance of the coaxial cable, was
made up by trilinear reeling of 11 coils of wire 0.3 wire covered with the gloss paint onto a ferrite ring, type
Amidon T 105�2. The whole construction was put into a hermetically closed and screened case, with the
mounted F socket. The symmetrizer also creates a galvanic connection of the LW antenna with the coaxial
cable's screen, which is connected with the grounding in the receiver, and allows the electrostatic charges,
induced in the antenna during the passing of the clouds above it, to be led into the ground. The grounding
was made of the galvanized steel pipe, 1.5 m in length, thrust into the ground, to which the 4 mm in diameter
cooper lead was connected. The second end was linked with the ground clamp in the grounding tune-up
system. Such system composes a balance for the non-symmetric LW antenna. For the high frequency electric
currents the grounding wire forms not only the resistance caused by the material resistivity, but also the
wave resistance, which is much greater and dependable even on the way of the wire placement. In order to
decrease the impedance of the grounding wire, the �tting system consisting of the tuned serial circuit and
the meter of the high frequency current, was made. The air coil of the tuned circuit was reeled with the DNE
2.0 wire, 24 reels in total, with detaches between every 2 reels. The air capacitor, of a capacity 500 pF, was
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Advances in Astronomy and Space Physics M. Szcz�e�sniak, R. Szcz�e�sniak, A. P. Durajski, M. W. Jarosik
isolated from the case. The toroidal transformer, which connects the tuned circuit with the meter circuit,
was reeled on the RP 20× 12× 8 ferrite ring, made up of F81 material. The whole system was placed into
a screened case. The introduction of a tuned resonance circuit into the grounding line and tuning it at a
previously determined frequency, becomes a very e�ective grounding for the high frequency currents. The
tuning of the grounding is based on the selection (with an use of a switch) of the proper detachment on a
coil and then tuning up the system with an alternating capacitor on a maximum de�ection of a meter.
The VLF receiver was factory constructed on a printed circuit board, and the entire system was closed
in a metal case, which serves as an anti-distortion screen. Such solution was not completely proven to be
useful in practice, because in order to tune the receiver, one should, �rstly, remove the upper cover of the
receiver (hence the system is left without the screening) and then, using the 50 kΩ set-up potentiometer tune
the receiver. In the case of such receiver design, its regulation would be less accurate and very annoying.
During the tuning of the system the biggest sources of distortions were the operator's hands, the computer,
the monitor and an ambient illumination [2]. To improve the regulation process and in order to reduce the
in�uence of the harmful signal on the quality and the course of the regulation, the case of the receiver was
replaced, double screened of the system was used and other constructional changes were introduced. Due
to the relatively large inertia of the system, the set-up potentiometer was replaced with the multi-round
potentiometer, which enables the precise tuning of the system.
The VLF receiver is originally provided with the analog / digital converter, which allows to transmit the
digital signal into the computer via the RS-232 serial port. During the modernization process the receiver
was additionally provided with the analog low frequency output, with a help of which the analog signal can
be transmitted into the computer via the sound card. The switch of the analog-digital output together with
the power switch and the multi-round potentiometer were placed on the front panel of the case. The selected
mode of the receiver work is signaled by the proper diodes.
The antenna socket, the power socket, the RS-232 socket, two jack-type sockets and the grounding socket
were mounted on the rear panel of the case. This solution has improved the maintenance of the receiver.
Typical changes in the radio radiation's intensity of the Earth's ionosphere
The most typical radio states of the Earth's ionosphere recorded with using the VLF 40 kHz receiver are
presented and discussed in the following chapter.
In particular, the changes of the ionosphere's radiation intensity caused by the changes of the solar activity
during the period between sunrise and sunset and registered on January, 17 and 21, 2010, are presented in
Figures. 1 and 3. It is worth to notice, that the in�uence of the Sun on the ionosphere is the largest in the
morning and in hours before midday, the ionization process takes an advantage in these hours (the density
of electrons in D layer is increasing) [3]. The recombination process, that leads to disappearance of the D
layer in the night, becomes dominating in hours after noon. The phenomena of ionization, related to the
sunrise and the sunset, are presented in Figures 1 and 3 as the increase and the decrease of the intensity of
received radio signal.
Figures 2 and 4 present the most interesting details from plots 1 and 3 and are generally explained with
the sudden distortion of the ionosphere caused by the solar �ashes and the Gamma Ray Bursts (GRB) type
�ashes. It is worth to underline, that the solar �ashes last from few minutes to about one and half hour.
Those phenomena are evoked by the rapid replacement of the magnetic �eld's energy of the Sun by the other
types of energy (mostly by the radiant energy, the thermal energy and the kinetic energy of the solar coronae
particles). Let us notice, that during the solar �ashes, the sunlit side of the Earth's ionosphere is being swept
by the ultraviolet radiation and the hard X-ray radiation. This type of radiation penetrates the D layer with
easily, thus increasing the rate of ionization process. In the case of the sudden distortion of the ionosphere as
a result of the solar �ash, the ionization process is observed with a small delay. This delay is equal to about
several minutes when counting from the beginning of the �ash. The �ash duration depends on many factors,
which can be: the magnitude of the solar �ash, the radiation intensity and the temporary electron density in
the ionosphere. The plot presented in Figure 2 shows the recombination process occurring in the ionosphere
after the solar �ash and persisting for more than 1 hour; the plot in Figure 4 presents slow recombination
process occurring in the ionosphere, with the duration equal to about 3 hours.
The GRB �ashes last from the few milliseconds to about an hour, occur more or less once per day,
originate from out of the galaxy [4]. Such phenomenon is accompanied by the sudden increasing of the
gamma radiation intensity on the small area of the sky. Let us notice, that the Earth's atmosphere absorbs
the gamma radiation, thus the GRB �ashes cannot be directly observed. From the Earth's surface the
observation is possible only through the monitoring of the second radiation of ionosphere. In Figures 3 and 4
one can see an �event�, which is very short, but energetic enough to signi�cantly change the signal intensity.
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Advances in Astronomy and Space Physics M. Szcz�e�sniak, R. Szcz�e�sniak, A. P. Durajski, M. W. Jarosik
[d
B
]
Figure 1: The changes in the ionosphere related to the sunrise and sunset and the changes evoked by the
solar �ash.
[d
B
]
Figure 2: The recombination phase after the solar �ash, that lasts for above an hour.
[d
B
]
Figure 3: The changes in the ionosphere related to the sunrise and the sunset, and the changes evoked by
the solar �ash. The characteristic, sharp peak is being also visible on the �gure, the most probably it is
induced by the strong GRB �ash.
[d
B
]
Figure 4: Slow recombination phase, lasting for few hours.
67
Advances in Astronomy and Space Physics M. Szcz�e�sniak, R. Szcz�e�sniak, A. P. Durajski, M. W. Jarosik
That phenomenon was recorded at 11:31:00 UT, with duration of 0.02 s. Short duration time suggests, that,
most possibly, the GRB �ash was registered [1].
Summary
The modernization of the KLAUDIA radiotelescope, which serves to register the Earth ionosphere's
radiation at 40 kHz frequency, was discussed in detail in the present paper. The investments, that were
made, enabled the signi�cant improvement of the quality of the received signal. In the second part of the
paper the typical changes in the intensity of the radio radiation evoked by the daily change of the solar
activity, unpredictable radio blasts generated by our star and the GRB �ash, were presented. The results
prove, that the KLAUDIA radiotelescope works correctly after modernization and, in the near future, will
serve for the permanent monitoring of the radio activity of the Sun.
References
[1] Band D., Matteson J., Ford L. et al. Astrophys. J., V. 413, pp. 281 (1993)
[2] Jarosik M. W., Starzy«ski S., Szcz�e±niak M., Szcz�e±niak R., Ceglarek A. E. YSC'14 Proc. of Contributed Papers, eds.:
Ivashchenko G., Golovin A., Kyivskyi Universytet, Kyiv, pp. 73-76 (2007)
[3] Pal P., De B.K. Proc. of the XXVIIIth URSI General Assembly in New Delhi, GP1.36 (0709) (2005)
[4] Smith F. G. `Radioastronomia', PWN Warszawa (1966)
[5] http://www.nitehawk.com
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