High-frequency trend during intense solar activity in September 2017: equatorial studies

Author(s):  
Sabirin Abdullah ◽  
Johari Talib
Space Weather ◽  
2019 ◽  
Vol 17 (1) ◽  
pp. 118-132 ◽  
Author(s):  
Nathaniel A. Frissell ◽  
Joshua S. Vega ◽  
Evan Markowitz ◽  
Andrew J. Gerrard ◽  
William D. Engelke ◽  
...  

2018 ◽  
Vol 2 (2) ◽  
pp. 85-91
Author(s):  
Husni Husni ◽  
Ali Warsito ◽  
Asnawi Husin

ABSTRAK Variasi perubahan frekuensi kritis lapisan F2 (foF2) dan ketinggian lapisan F2 (h'F2) di atas Kupang selama tahun 2014 mengalami perubahan yang bervariasi dimana hal ini bergantung pada aktivitas matahari, semakin tinggi tingkat aktivitas matahari semakin tinggi pula tingkat variasi pada foF2 dan h'F2, sebaliknya semakin rendah tingkat aktivitas matahari semakin berkurang pula tingkat variasi foF2 dan h'F2 variasi perubahan terhadap lapisan F diindikasikan dengan penurunan dan peningkatan nilai foF2 dan h'F2. Peningkatan nilai foF2 rata-rata terjadi pada pukul  07.00 WITA mencapai maksimumnya pada pukul 12.00-14.00 WITA siang hari dan dikuti dengan penurunan nilai foF2 pada malam hari yang mencapai minimumnya pada pukul 05.00-06.00 WITA pagi. Selama tahun 2014, ketinggian lapisan F2 memiliki tiga pola peningkatan yang berbeda, (1) peningkatan ketinggian pada jam tengah hari seperti yang terjadi pada bulan Januari – April, (2) peningkatan pada jam tengah malam hingga menjelang matahari terbit, jam-jam tengah hari dan  sore hingga malam hari terjadi pada bulan Mei – Agustus (3) peningkatan pada pada jam tengah malam hingga menjelang matahari terbit dan jam-jam tengah hari seperti pada bulan September – Desember. Dalam pemanfaatannya sebagai media pantul gelombang komunikasi radio frekuensi tinggi (HF), karakteristik ionosfer di atas Kupang selama tahun 2014, memiliki kemampuan memantulkan gelombang frekuensi tinggi berada pada rentang 2-19.2 MHz dengan ketinggian yang berada pada rentang 179 – 550 Km. Akan mengakibatkan gagalnya komunikasi radio frekuensi tinggi, apabila menggunakan frekuensi lebih besar atau lebih kecil dari frekuensi yang dapat bekerja tersebut. Kata Kunci : Aktivitas matahari, Frekuensi kritis F2, ketinggian lapisan F2, komunikasi radio, frekuensi tinggi. ABSTRACT The ionospheric critical frequency (foF2) and the F2 layer height (h'F2) variation over Kupang during 2014 period unchanged varied where it is dependent on solar activity, the higher the level of solar activity the higher the level of variation in foF2 and h'F2, conversely the lower level of sun activity diminishing the level of variation foF2 and h'F2 variation changes to the F layer is indicated by a decrease and an increase in the value of foF2 and h'F2. Increasing the value of the average foF2 occurred at 07:00 pm reaching it's maximum at noon and 12:00 to 14:00 pm followed by impairment foF2 at night, which reached it's minimum at morning 5:00 to 6:00 pm. During 2014, the altitude of the F2 has three patterns different upgrade, (1) an increase in height on the hour midday as happened in January-April, (2) an increase in the hours of midnight until before sunrise, hours noon and afternoon until the evening occurred in May-August (3) an increase in the hours of midnight until near sunrise and midday hours as in September-December. In the media utilization as reflected waves of high frequency radio communications (HF), characteristics of the ionosphere above Kupang during 2014, has the ability to reflect high frequency waves that are in the range of 2 - 19.2 MHz with a height that is in the range 179-550 Km. Will lead to high frequency radio communication failure, when using a frequency of greater or smaller than the frequency that can work. Keywords: solar activity, the critical frequency of F2, F2 layer heights, radio communications, high frequency.


2016 ◽  
Vol 6 (1) ◽  
pp. 24-27 ◽  
Author(s):  
Ya. Volvach ◽  
A. Stanislavsky ◽  
A. Konovalenko ◽  
A. Koval ◽  
V. Dorovskyy

We report about new observations of solar 'drift pair' (DP) bursts by means of the UTR-2 radio telescope at frequencies 10-30 MHz. Our experimental data include both 'forward' and 'reverse' bursts with high frequency and time resolution. The records of 301 bursts, observed in 10-12 July of 2015, are investigated. The main properties of these bursts (frequency bandwidth, central frequency and others) have been analysed. In this report our main attention is paid to the comparison of our observations with the similar observations of decametre DPs performed earlier during 13-15 July of 2002 in the same frequency range. Common features of DPs in the two different pieces of data samples have been found. This may indicate the possible presence of stability in the frequency-time properties of decametre DPs from one cycle of solar activity to another.


2020 ◽  
pp. 3434-3444
Author(s):  
Ala'a A. Al-Shallal ◽  
Najat M. R. Al-Ubaidi

High frequency (HF) radio wave propagation depends on the ionosphere status which is changed with the time of day, season, and solar activity conditions. In this research, ionosonde observations were used to calculate the values of maximum usable frequency (MUF) the ionospheric F2- layer during strong geomagnetic storms (Dst ≤ -100 nT) which were compared with the predicted MUF for the same layer by using IRI-16 model. Data from years 2015 and 2017, during which five strong geomagnetic storms occurred, were selected from two Japanese ionosonde stations (Kokubunji and Wakkanai) located at the mid-latitude region. The results of the present work do not show a good correlation between the observed and predicted MUF values for F2- layer during the selected events of strong geomagnetic storms at these stations. Thus, there is a further need to improve the IRI-16 model for better matching with the observations during strong geomagnetic storms.


1977 ◽  
Vol 36 ◽  
pp. 143-180 ◽  
Author(s):  
J.O. Stenflo

It is well-known that solar activity is basically caused by the Interaction of magnetic fields with convection and solar rotation, resulting in a great variety of dynamic phenomena, like flares, surges, sunspots, prominences, etc. Many conferences have been devoted to solar activity, including the role of magnetic fields. Similar attention has not been paid to the role of magnetic fields for the overall dynamics and energy balance of the solar atmosphere, related to the general problem of chromospheric and coronal heating. To penetrate this problem we have to focus our attention more on the physical conditions in the ‘quiet’ regions than on the conspicuous phenomena in active regions.


1979 ◽  
Vol 44 ◽  
pp. 357-372
Author(s):  
Z. Švestka

The following subjects were discussed:(1)Filament activation(2)Post-flare loops.(3)Surges and sprays.(4)Coronal transients.(5)Disk vs. limb observations.(6)Solar cycle variations of prominence occurrence.(7)Active prominences patrol service.Of all these items, (1) and (2) were discussed in most detail and we also pay most attention to them in this report. Items (3) and (4) did not bring anything new when compared with the earlier invited presentations given by RUST and ZIRIN and therefore, we omit them.


Author(s):  
W. E. Lee ◽  
A. H. Heuer

IntroductionTraditional steatite ceramics, made by firing (vitrifying) hydrous magnesium silicate, have long been used as insulators for high frequency applications due to their excellent mechanical and electrical properties. Early x-ray and optical analysis of steatites showed that they were composed largely of protoenstatite (MgSiO3) in a glassy matrix. Recent studies of enstatite-containing glass ceramics have revived interest in the polymorphism of enstatite. Three polymorphs exist, two with orthorhombic and one with monoclinic symmetry (ortho, proto and clino enstatite, respectively). Steatite ceramics are of particular interest a they contain the normally unstable high-temperature polymorph, protoenstatite.Experimental3mm diameter discs cut from steatite rods (∼10” long and 0.5” dia.) were ground, polished, dimpled, and ion-thinned to electron transparency using 6KV Argon ions at a beam current of 1 x 10-3 A and a 12° angle of incidence. The discs were coated with carbon prior to TEM examination to minimize charging effects.


Author(s):  
G. Y. Fan ◽  
J. M. Cowley

It is well known that the structure information on the specimen is not always faithfully transferred through the electron microscope. Firstly, the spatial frequency spectrum is modulated by the transfer function (TF) at the focal plane. Secondly, the spectrum suffers high frequency cut-off by the aperture (or effectively damping terms such as chromatic aberration). While these do not have essential effect on imaging crystal periodicity as long as the low order Bragg spots are inside the aperture, although the contrast may be reversed, they may change the appearance of images of amorphous materials completely. Because the spectrum of amorphous materials is continuous, modulation of it emphasizes some components while weakening others. Especially the cut-off of high frequency components, which contribute to amorphous image just as strongly as low frequency components can have a fundamental effect. This can be illustrated through computer simulation. Imaging of a whitenoise object with an electron microscope without TF limitation gives Fig. 1a, which is obtained by Fourier transformation of a constant amplitude combined with random phases generated by computer.


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