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    Tytuł:
    Chronology of Formation of Solar Radio Burst Types III and V Associated with Solar Flare Phenomenon on 19th September 2011
    Autorzy:
    Hamidi, Z. S.
    Shariff, N. N. M.
    Powiązania:
    https://bibliotekanauki.pl/articles/411656.pdf
    Data publikacji:
    2014
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    solar radio burst
    solar flare
    type III
    type V
    CALLISTO
    Opis:
    The formation of two different solar bursts, type III and V in one solar flare event is presented. Both bursts are found on 19th September 2011 associated with C-class flares on active region 1295. From the observation, we believed that the mechanism of evolution the bursts play an important role in the event. It is found that type V burst appeared in five minutes after type III. There are a few active regions on the solar disk but most are magnetically simple and have remained rather quiet. An interpretation of this new result depends critically on the number of sunspots and the role of active region 1295. Sunspot number is increased up to 144 with seven sunspots can be observed. During that event, the speed of solar wind exceeds 433.8 km/second with 2.0 g/cm3 density of protons in the solar corona. Currently, radio flux is also high up to 150 SFU. The solar flare type C6 is continuously being observed in the X-ray region for 24 hours since 1541 UT and a maximum C1 is detected on 1847 UT. Although the sources of both bursts are same, the direction and ejection explode differ.
    Źródło:
    International Letters of Chemistry, Physics and Astronomy; 2014, 5; 32-42
    2299-3843
    Pojawia się w:
    International Letters of Chemistry, Physics and Astronomy
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Production of Coronal Mass Ejections in Relation With Complex Solar Radio Burst Type III Correlated With Single Solar Radio Burst Type III
    Autorzy:
    Hussien, Nurul Hazwani
    Hamidi, Z. S.
    Ali, M. O.
    Sabri, S. N. U.
    Zainol, N. H.
    Shariff, N. N. M.
    Moinstein, C
    Powiązania:
    https://bibliotekanauki.pl/articles/1192988.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Sun
    Solar radio burst
    type III
    single Solar Radio Burst Type (SRBT) III
    complex Solar Radio Burst Type (SRBT) III
    Coronal Mass Ejection (CMEs)
    magnetic reconnection
    Opis:
    The complex solar radio burst type III is very related to generation of Coronal Mass Ejections (CMEs). In a previous study, they deduced that the burst was produced by electron beams accelerated in blast wave shocks and injected along open magnetic field lines, similar to the herringbone bursts at metric wavelengths. Usually, if there is another solar flare recorded during complex solar radio burst type III it should be type II burst. Different for this event, the single solar radio burst recorded occur 8 minutes 30 seconds before the complex solar radio burst type III. The Coronal Mass Ejections also recorded occurred 7 hours before the single and complex solar radio burst type III. It is noted that CMEs occurred several hours before this event recorded by the SOHO websites.It is proved that the production of coronal mass ejection contributed to the production of complex solar radio burst type III.
    Źródło:
    World Scientific News; 2016, 36; 96-108
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Observations of Different Type of Bursts Associated with M 6.3 Solar Flares
    Autorzy:
    Hamidi, Z. S.
    Shariff, N. N. M.
    Powiązania:
    https://bibliotekanauki.pl/articles/412558.pdf
    Data publikacji:
    2014
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    sun
    low frequency
    solar radio
    burst
    type III
    type U
    e-CALLISTO
    Opis:
    Variation of solar bursts due to solar flares such as type an isolated type III , a complex type III, U is being highlighted. These bursts occurred on 9th March 2012 at the National Space Centre, Sg. Lang, Selangor, Malaysia Here, we study a unique case with a combination of two types burst associated with solar flare and CMEs. Our observation is focused on the low frequency region starting from 150 MHz till 400 MHz. We found that a solar flare type solar flare type M 6.3 which occurred in active region AR 1429 starting from 3:32 UT and ending at 05:00 UT. The flare has been confirmed to be the largest flare since 2005. Some physical parameters will be measured. We then compared our results with X-ray data from NOAA Space Weather Prediction Centre (SWPC).
    Źródło:
    International Letters of Chemistry, Physics and Astronomy; 2014, 4; 29-36
    2299-3843
    Pojawia się w:
    International Letters of Chemistry, Physics and Astronomy
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    The Tendencies and Timeline of the Solar Burst Type II Fragmented
    Autorzy:
    Hamidi, Z. S.
    Shariff, N. N. M.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/412634.pdf
    Data publikacji:
    2014
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    sun
    low frequency
    solar radio
    burst
    type II
    type III
    e-CALLISTO
    Opis:
    We report the timeline of the solar radio burst Type II that formed but fragmented at certain point based on the eruption of the solar flare on 13th November 2012 at 2:04:20 UT. The active region AR 1613 is one of the most active region in 2012. It is well known that the magnetic energy in the solar corona is explosively released before converted into the thermal and kinetic energy in solar flares. In this work, the Compound Astronomical Low-frequency, Low-cost Instrument for Spectroscopy Transportable Observatories (CALLIISTO) system is used in obtaining a dynamic spectrum of solar radio burst data. There are eight active regions and this is the indicator that the Sun is currently active. Most the active regions radiate a Beta radiation. The active regions 1610, 1611 and 1614 are currently the largest sunspots on the visible solar disk. There is an increasing chance for an isolated M-Class solar flare event. It is also expected that there will be a chance of an M flare, especially from AR 1614 and 1610. Although these two observations (radio and X-rays) seem to be dominant on the observational analysis, we could not directly confirmed that this is the only possibility, and we need to consider other processes to explain in detailed the injection, energy loss and the mechanism of the acceleration of the particles. In conclusion, the percentage of energy of solar flare becomes more dominant rather than the acceleration of particles through the Coronal Mass Ejections (CMEs) and that will be the main reason why does the harmonic structure of type II burst is not formed. This event is one fine example of tendencies solar radio burst type III, which makes the harmonic structure of solar radio burst type II fragmented.
    Źródło:
    International Letters of Chemistry, Physics and Astronomy; 2014, 12; 84-102
    2299-3843
    Pojawia się w:
    International Letters of Chemistry, Physics and Astronomy
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Investigation on a Broken Solar Burst Type II during High Activities in AR1613 on 13th November 2012
    Autorzy:
    Hamidi, Z. S.
    Shariff, N. N. M.
    Monstein, C.
    Zulkifli, W. N. A. W.
    Ibrahim, M. B.
    Arifin, N. S.
    Amran, N. A.
    Powiązania:
    https://bibliotekanauki.pl/articles/411666.pdf
    Data publikacji:
    2014
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    sun
    low frequency
    solar radio
    burst
    type II
    type III
    e-CALLISTO
    Opis:
    The present article is an attempt to analyze the solar burst Type II observations based on solar flare and Coronal Mass Ejections (CMEs) events. We choose an intriguing type II radio burst with a velocity of 1193 kms-1 that occurred on 2012 November 13 at 2:04:20 UT. In this case, the study of solar radio burst type III is of paramount importance because of the fact that it helps to gain an insight of generation mechanisms of solar flare and Coronal Mass Ejections (CMEs) phenomena. Here, we have got a reasonably clear idea of the various forms under which the type III continuum emission may appear and potentially form a type II burst. However, in this case, the Type II solar burst only successfully forms a fundamental structure within the first few minute period, but broken suddenly before evolve a harmonic structure. This phenomenon is very interesting to be tackled and study. How the burst suddenly broken is still ongoing research seems the event is very rare and hard to be proved. There are a few questions that cause this unique situation which related to: (i) the intensity and duration of type III burst which also related to the classification of solar flare (ii) the probabilities CMEs to occur during that time and also the factor of the total amount of massive burst that exploded, Thus, we can conclude that the solar burst type III event still tells us an enigmatic characteristic from time to time due to the relationship of energetic particles and streams of particles with coronal magnetic fields and the pattern of Sun activity due to the 24th solar cycle. It might an interesting to study in detail the main factor that caused the Type II solar burst broken. Indirectly, it might because of the very intense of solar flares that make the percentage of energy of solar flare become more dominant rather than the acceleration of particles through the Coronal Mass Ejections. Thus, we realize that the potential energy during this event is higher than the kinetic energy of the particles.
    Źródło:
    International Letters of Chemistry, Physics and Astronomy; 2014, 9; 8-15
    2299-3843
    Pojawia się w:
    International Letters of Chemistry, Physics and Astronomy
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    An Alternating of Solar Radio Burst Type III and IV of Thermal and Non-Thermal Plasma Radiation
    Autorzy:
    Hamidi, Z. S.
    Husien, Nurul Hazwani
    Shariff, N. N. M.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/1193005.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Sun
    burst
    low frequency
    solar radio
    type III
    type IV e-CALLISTO
    Opis:
    A preliminary correlation study of the solar burst type III with a type Iv solar burst of has been made. On the basis of this study and in combination with the observation in radio emission, an interpretation of the mechanism of the occurrence of this event has been proposed. We have noted that an individual type III burst also can be observed at 13:54-13:58 UT from 500 MHz. Based on 3 days observation beginning from 31st March 2015, the solar activity is gradual increased. The highest solar flare can be observed is only a class of M8 flare. There was a CMEs event that directed to the Earth is detected. From the selected event, although theoretically solar radio burst type III is alternating with type IV solar burst. This huge explosion generated the M-class flare which can affect the Earth and satellites. The solar wind velocity recorded is 384.2 km/second while the density of protons is 3.6 protons/cm3. The total magnetic field during this event also quite big which is 4.6nT. The alternating of solar burst type III and IV would probably depends on the tendencies to form the CMEs event. The morphology of thermal and non-thermal flare plasma is of particular significance because it holds many important signatures of the energy release process.
    Źródło:
    World Scientific News; 2016, 31; 88-99
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Statistical Study of Nine Months Distribution of Solar Flares
    Autorzy:
    Hamidi, Z. S.
    Shariff, N. N. M.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/412246.pdf
    Data publikacji:
    2014
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    sun
    solar eclipse
    solar radio
    burst
    type III
    e-CALLISTO
    Opis:
    Solar flare is one of the solar activities that take place in the outermost layer of the corona. Solar flares can heat the material to several million degrees in just a few minutes and at the same time they release the numerous amount of energy. It is believed that a change of magnetic field lines potentially creates the solar flares. The objectives of the study are to identify and compare the types of solar flares (in X-Ray) region and to improve understanding of solar flares. Data are taken from the NOAA website, from the United States Department of Commerce, NOAA, Space Weather Prediction Center (SPWC). Solar radio flux readings were merged together with the three classes and a total of nine graphs were plotted. In illustrating the relationship of solar radio flux and solar flares, it can be explained by studying the range values of flux corresponding to flares values. From this case study, it was found that the minimum value of solar radio flux in order for the flares to occur is equivalent 68 x 10-22Wm-2Hz-1. Thus, whenever the values of solar radio flux are high, there should be a higher number of flares produced by the sun. The overall range of solar radio flux recorded in this study ranging from 68 x 10-22 Wm-2Hz-1 to 96 x 10-22 Wm-2Hz-1. Observing and collecting data from the Sun and develop our very own new prediction methods will leads the accuracy of the prediction of the behavior of the Sun more precisely.
    Źródło:
    International Letters of Chemistry, Physics and Astronomy; 2014, 14, 1; 1-11
    2299-3843
    Pojawia się w:
    International Letters of Chemistry, Physics and Astronomy
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    The Propagation of An Impulsive Coronal Mass Ejections (CMEs) due to the High Solar Flares and Moreton Waves
    Autorzy:
    Hamidi, Z. S.
    Shariff, N. N. M.
    Powiązania:
    https://bibliotekanauki.pl/articles/412288.pdf
    Data publikacji:
    2014
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    sun
    solar eclipse
    solar radio
    burst
    type III
    e-CALLISTO
    Opis:
    This paper provides a short review of some of the basic concepts related to the origin of Coronal Mass Ejections (CMEs). The numerous ideas which have been put forward to elucidate the initiation of CMEs are categorized in terms of whether this event is a gradual CME or impulsive CME. In this case, an earth-directed Coronal Mass Ejection (CME) was observed on April 2, 2014 by the Large Angle Spectrometric Coronagraph (LASCO) C2. This recent observations obtained a large impulsive CMEs. The CME, originating from the active region AR2027. The speed of CMEs is 1600 kms-1. A halo CME, a bright expanding ring at the North-West region is exploded beginning at about 14:36 UT, and the process of departing, expansion and propagation are highlighted. We discuss the correspondence of this event with the structure of the CME in the LASCO data. It is believed that the high solar flare and a Moreton waves initiate this kind of CMEs.
    Źródło:
    International Letters of Chemistry, Physics and Astronomy; 2014, 14, 1; 118-126
    2299-3843
    Pojawia się w:
    International Letters of Chemistry, Physics and Astronomy
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Scenario of Solar Radio Burst Type III During Solar Eclipse on 14th November 2012
    Autorzy:
    Hamidi, Z. S.
    Shariff, N. N. M.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/411752.pdf
    Data publikacji:
    2014
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    sun
    solar eclipse
    solar radio
    burst
    type III
    e-CALLISTO
    Opis:
    A compact solar flare was observed during a total solar eclipse event on 13-14 November 2012. This phenomenon is beginning in local time on November 14 west of the date line over northern Australia, and ended in local time on November 13 east of the date line near the west coast of South America. During the eclipse, the highest magnitude was 1.0500, occurring only 12 hours before perigee, with the maximum eclipse totality lasting just over four minutes. Considering the observational facts, the solar radio burst type III can be detected from the National Space Centre Malaysia by the Compound Low Cost Low Frequency Transportable Observatory (CALLISTO) system from 00:00 UT –1:30 UT. The group and individual solar burst type III can be detected in the region of 150-400 MHz. However, the eclipse cannot be observed from our site. From the observation, it was found that the eruption in the active region is becoming more active with a tens of groups solar radio burst type III can be observed. It continuing bursting within the first one hour. The sunspot number exceeds to 108 and solar wind speed 454.9 km/sec. Still the Sun remains active and we need to consider other processes to explain in detailed the injection, energy loss and the mechanism of the acceleration of the particles.
    Źródło:
    International Letters of Chemistry, Physics and Astronomy; 2014, 13, 2; 135-143
    2299-3843
    Pojawia się w:
    International Letters of Chemistry, Physics and Astronomy
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    The Development of Solar Prominence on 4th September 2015 and the Solar Burst Type III and IV
    Autorzy:
    Norsham, N. A.
    Hamidi, Z. S.
    Mazlan, Muzamir
    Shariff, N. N. M.
    Yusofl, N. S.
    Jafni, A. I.
    Khalib, N. M. F.
    Hamdan, M. N.
    Kamaruddin, Farahana
    Tahar, Muhammad Redzuan
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/1192156.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Solar prominences
    active region (AR)
    solar burst
    type III
    type IV
    e CALLISTO
    Opis:
    This article will focus on the solar prominences that occur during the 4th September 2015. On that day, there were two sunspots on the surface of the sun, which were AR2409 and AR2410. These two active regions did not produce any threat for strong flare and thus the solar activity was very low. The prominences that will be focused were both occurred at 0353 UT and 0427 UT respectively. There were minor (G1) geomagnetic storm observed on that day. For solar prominences that occurred at 0353 UT, solar radio burst type (SRBT) IV was detected by CALLISTO spectrometer. From the CALLISTO, two bursts at low intensities with the duration of about 7 minutes for the first burst of 280-320 MHz and 6 minutes for the second burst of 360-430 MHz were observed. For the first burst, energy calculated was between 1.855 x 10 -25 J and 2.12 x 10 -25 J with the drift rate of 0.095 MHz/s. For second burst, the energy obtained was between 2.385 x 10 -25 J and 2.849 x 10 -25 J with the drift rate of 0.194 MHz/s. At 0427 UT, SRBT III was recorded with a frequency of 240-350 MHz with the energy which was obtained between 1.590 x 10 -25 J and 2.319 x 10 -25 J. The drift rate of this type of burst was 0.61 MHz/s. During this event, the solar wind value was 499.3 km/Sec with the proton density of 15.1 protons/cm3.
    Źródło:
    World Scientific News; 2016, 45, 2; 264-275
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Probability of Solar Flares Turn Out to Form a Coronal Mass Ejections Events Due to the Characterization of Solar Radio Burst Type II and III
    Autorzy:
    Hamidi, Z. S.
    Powiązania:
    https://bibliotekanauki.pl/articles/412360.pdf
    Data publikacji:
    2014
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    solar flare
    Coronal Mass Ejection
    solar burst
    type II
    type III
    space Feather
    Opis:
    The solar flare and Coronal Mass Ejections (CMEs) are well known as one of the most massive eruptions which potentially create major disturbances in the interplanetary medium and initiate severe magnetic storms when they collide with the Earth‟s magnetosphere. However, how far the solar flare can contribute to the formation of the CMEs is still not easy to be understood. These phenomena are associated with II and III burst it also divided by sub-type of burst depending on the physical characteristics and different mechanisms. In this work, we used a Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy in Transportable Observatories (CALLISTO) system. The aim of the present study is to reveal dynamical properties of solar burst type II and III due to several mechanisms. Most of the cases of both solar radio bursts can be found in the range less that 400 MHz. Based on solar flare monitoring within 24 hours, the CMEs that has the potential to explode will dominantly be a class of M1 solar flare. Overall, the tendencies of SRBT III burst form the solar radio burst type III at 187 MHz to 449 MHz. Based on solar observations, it is evident that the explosive, short time-scale energy release during flares and the long term, gradual energy release expressed by CMEs can be reasonably understood only if both processes are taken as common and probably not independent signatures of a destabilization of pre-existing coronal magnetic field structures. The configurations of several active regions can be sourced regions of CMEs formation. The study of the formation, acceleration and propagation of CMEs requires advanced and powerful observational tools in different spectral ranges as many „stages‟ as possible between the photosphere of the Sun and magnetosphere of the Sun and magnetosphere of the Earth. In conclusion, this range is a current regime of solar radio bursts during CMEs events.
    Źródło:
    International Letters of Chemistry, Physics and Astronomy; 2014, 16; 1-85
    2299-3843
    Pojawia się w:
    International Letters of Chemistry, Physics and Astronomy
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Comparison of the Optical Image of the Solar Prominence with the Formation of Solar Radio Burst Type III on 3rd September 2015
    Autorzy:
    Hamidi, Z. S.
    Norsham, N. A.
    Mazlan, Muzamir
    Yusof, N. S.
    Jafni, A. I.
    Kahlid, N. M.
    Hamdan, M. N.
    Kamaruddin, Farahana
    Tahar, Muhammad Redzuan
    Monstein, C.
    Shariff, N. N. M.
    Powiązania:
    https://bibliotekanauki.pl/articles/1192670.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    solar prominences
    solar radio burst
    type III
    AR2407
    e CALLISTO
    Opis:
    Solar radio burst in the range of 220 - 400 MHz have been correlated with the optical solar prominence phenomena covering the presence sunspot minimum. In combination of the observation in radio emission and the basis of this study, the occurrence of the event has been proposed. The active region of the prominence was AR2407. An individual type III burst was observed at 08:21 UT. The burst lasts for 20 seconds with a drift rate of 4.25 MHz/s. This burst was recorded by the Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy and Transportable Observatory (CALLISTO) at Switzerland. The CALLISTO spectrometer is a spectrometer system that has been installed all around the world to observe the activity of the sun for 24 hours. The activation may be caused by shock waves issuing from prominences and solar flares. The loop prominences can be observed by using the optical telescope and is the initiates points of the following important flare that exist for 6 hours. The active region on the Sun experience the gradual build up of the magnetic field which gives rise to the sunspots, prominences and loops in the corona and produce the powerful outburst explosions.
    Źródło:
    World Scientific News; 2016, 47, 2; 230-240
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Emergence of an Impulsive CMEs Related To Solar Radio Burst Type III Due To Magnetic Filament Eruption
    Autorzy:
    Ali, M. Omar
    Shariff, N. N. M.
    Hamidi, Z. S.
    Husien, Nurul Hazwani
    Sabri, S. N. U.
    Zainol, N. H.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/1192085.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Sun
    Coronal Mass Ejections (CMEs)
    solar burst type III
    magnetic filament
    Opis:
    During solar activity the energy particles of the sun released due to solar flare, Coronal Mass Ejections (CMEs), coronal heating as well as sunspot. Solar radio burst will be observed in the presence of solar activity such solar flare, CMEs and solar prominence as the indicator for those events to happen. During the peak of solar cycle, the filaments are present due to the active magnetic field and solar storm’s explosion. This type of solar radio burst normally can be seen in the phase of impulsive solar flare. Therefore, it is crucial to understand field line connectivity in flare and the access of flare accelerated particle to the earth. In this study, we highlighted on the observation of solar radio burst type III on 9th of May at 05:31 UT till 05:44 UT. The event was successfully recoded by e-CALLISTO using BLEINSW radio telescope. The Solar Radio Burst Type III that had been observed was related to the Coronal Mass Ejections and the mechanisms that trigger the events have been discussed. It is shown that the CMEs is believed to happen because of the magnetic filament that connected to active region (AR) 2339 was erupted, and combination of two wild filament produced a bright CMEs. Fortunately, the expanding cloud does not appear to be heading for earth.
    Źródło:
    World Scientific News; 2016, 37; 168-178
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Comparison of the Radio Frequency Interference (RFI) in the Region of Solar Burst Type III Data At Selected CALLISTO Network
    Autorzy:
    Hamidi, Z. S.
    Shariff, N. N. M.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/412319.pdf
    Data publikacji:
    2014
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    CALLISTO
    low frequency
    solar burst type III
    Radio Frequency Interference (RFI)
    Opis:
    Compact Astronomical Low-frequency, Low-cost Instrument for Spectroscopy in Transportable Observatories (CALLISTO) is a global network of spectrometer system with the purpose to observe the Sun’s activities. There are 25 stations that are used for this purpose. Radio Frequency Interference (RFI) is a major obstacle when performing observation with CALLISTO. We have confirmed at least 2 stations out of 10 stations with a complete overview spectral (OVS) made available to us showed clear detection of these consistent types of RFI for each specific region. In Malaysia, these RFI are also clearly detected. The major RFI affecting CALLISTO within radio astronomical windows below 1 GHz are local electronic system specifically radio navigation (at 73.1 MHz and 75.2 MHz), broadcasting (at (i) 151 MHz, (ii) 151.8 MHz and 152 MHz), aeronautical navigation (at (i) 245.5 MHz, (ii) 248.7 MHz and (iii) 249 MHz and fixed mobile at (i) 605 MHz, (ii) 608.3 MHz, (iii) 612.2 MHz, (iv) 613.3 MHz). It is obviously showed that all sites within this region are free from interference at 320-330 MHz and is the best specific region to be considered for solar burst monitoring. We also investigate the effect of RFI on detection of solar burst. We have considered type III solar bursts on 9th March 2012 in order to measure the percentage of RFI level during the solar burst. The RFI level is as low as 6.512 % to 80.769 % above solar burst detection.
    Źródło:
    International Letters of Chemistry, Physics and Astronomy; 2014, 10; 38-45
    2299-3843
    Pojawia się w:
    International Letters of Chemistry, Physics and Astronomy
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    First Light Detection of A Single Solar Radio Burst Type III Due To Solar Flare Event
    Autorzy:
    Hamidi, Z. S.
    Shariff, N. N. M.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/411677.pdf
    Data publikacji:
    2014
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Solar flare
    low frequency
    radio wavelength
    solar burst
    type III
    CALLISTO
    Opis:
    The eruption mechanism of solar flares and type III are currently an extremely active area of research, especially during the solar cycle is towards maximum. In this case, the total energy of solar burst type III is of the order of solar flare with the explosion of the energy can up to 1015 ergs. The solar flare event is one of the most spectacular explosions that still be on-going study in the solar physics world. This event occurred at 2:000 UT on 15th April 2012 is due to the explosion of the magnetic energy in from the chromosphere and converted into the heating, mass motion and particle acceleration which can be detected by solar radio burst type III. In this work, we will highlight our first light detection of very tiny solar radio burst type III, which has been observed at the National Space Centre, Banting, Selangor detected by the Compound Low Cost Low Frequency Transportable Observatories (CALLISTO) system at 5:53:23. The region of the data is from 150 − 400 MHz in radio region. This burst is drifted from 150 MHz till 260 MHz. It represents a total energy of 6.2035 × 10-7 eV − 1.0753 × 10-6 eV. This fast drift burst is a continuity of the acceleration of the particles which is intermittent, and can be observed since the explosion of the solar flare. Although the burst is very tiny, it is still significant because this burst is the first detection of a single type III burst from our site. Still, the acceleration of the particles can be detected from Earth in the radio region within 3 hours period of observation at the post stage of solar flare.
    Źródło:
    International Letters of Chemistry, Physics and Astronomy; 2014, 11, 1; 51-58
    2299-3843
    Pojawia się w:
    International Letters of Chemistry, Physics and Astronomy
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Characterization of Selected Solar Radio Bursts Based on Solar Activity Detected by e- CALLISTO (Malaysia)
    Autorzy:
    Hamidi, Z. S.
    Shariff, N. N. M.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/412630.pdf
    Data publikacji:
    2014
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    sun
    low frequency
    solar radio
    burst
    type II
    type III
    type IV
    type V
    type U
    e-CALLISTO
    Opis:
    One of the main reasons to study more about the dynamics of solar radio bursts is because solar these bursts can interfere with the Global Positioning System (GPS) and communications systems. More importantly, these bursts are a key to understand the space weather condition. Recent work on the interpretation of the low frequency region of a main solar burst is discussed. Continuum radio bursts are often related to the solar activities such as an indication of the formation of sunspot, impulsive phase of solar flares and Coronal Mass Ejections (CMEs) and their frequencies correspond to the densities supposed to exist in the primary energy release volume. Specifically, solar burst in low frequency play an important role in interpretation of Sun activities. In this work, we have selected few solar bursts that successfully detected by our station at the National Space Centre, Banting Selangor. Our objective is to correlate the solar burst with Sun activities by looking at the main sources that responsibility with the trigger of solar burst. It is found that type II burst is dominant with Coronal Mass Ejections (CMEs), type III burst associated with solar flare, IV burst with the formation of active region and type U burst high solar flare. We believed that this work is a good start to monitor Sun’s activities in Malaysia as equatorial country.
    Źródło:
    International Letters of Chemistry, Physics and Astronomy; 2014, 13, 2; 144-159
    2299-3843
    Pojawia się w:
    International Letters of Chemistry, Physics and Astronomy
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    The Progression of Active Region with the Formation of Group and Complex Solar Radio Burst Type III on 31st August 2015
    Autorzy:
    Hamidi, Z. S.
    Norsham, N. A.
    Mazlan, Muzamir
    Yusof, N. S.
    Jafni, A. I.
    Kahlid, N. M.
    Hamdan, M. N.
    Kamaruddin, Farahana
    Tahar, Muhammad Redzuan
    Monstein, C.
    Shariff, N. N. M.
    Powiązania:
    https://bibliotekanauki.pl/articles/1182942.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    solar prominences
    complex solar radio burst
    type iii
    ar2403
    e callisto
    Opis:
    In this event, a solar radio burst in the range of 45-165 MHz with energy of 〖2.982 x 10〗^(-26) to 〖1.093 x 10〗^(-25) Joule with 0.8 MHz/ second have been correlated with the optical solar prominence. In combination of the optical, radio and X-ray observation, the occurrence of the event has been proposed. The active region of the prominence was AR2403. An individual type III burst was observed at 19:40 UT. The burst lasts for 15 minutes with a drift rate of 0.8 MHz/s. This burst was recorded by the Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy and Transportable Observatory (CALLISTO) at Almaty Site. From 29th August 2015 onwards, the total magnetic flux increases gradually to over four-fold the initial value during development and levels off around 29th August 2015. It was found that B3 solar flare, followed by a slow coronal mass ejection (CME), is released from NOAA 2403 on 31st August 2015. The region is beyond -30 longitude at the time of the flare, making it impossible to reliably measure any magnetic properties involving gradients. The overall increase of Beff prior to the flare is indicative of an increase in polarity mixing within the AR, which has been shown to be related to flaring. Understanding of the exact nature of the initiation of these events is still incomplete.
    Źródło:
    World Scientific News; 2016, 49, 2; 272-282
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Expression of IFN-λ1 from Congjiang pigs and its effect on anti-PRRSV proliferation
    Autorzy:
    Xin-qin, J.
    Biao, W.
    Zhi-qiang, D.
    Yong, R.
    Yan, H.
    Meng-qiu, H.
    Shan-shan, D.
    Yu-jie, T.
    Powiązania:
    https://bibliotekanauki.pl/articles/2087291.pdf
    Data publikacji:
    2020
    Wydawca:
    Polska Akademia Nauk. Czytelnia Czasopism PAN
    Tematy:
    porcine ifn-λ1
    porcine type III interferon
    eukaryotic expression
    anti-proliferation
    Źródło:
    Polish Journal of Veterinary Sciences; 2020, 23, 3; 423-430
    1505-1773
    Pojawia się w:
    Polish Journal of Veterinary Sciences
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Occurrences Rate of Type II and III Solar Radio Bursts at Low Frequency Radio Region 45 − 870 MHz
    Autorzy:
    Hamidi, Z. S.
    Shariff, N. N. M.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/412187.pdf
    Data publikacji:
    2014
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    CALLISTO
    low frequency
    solar burst
    type II
    type III
    solar flare
    Coronal Mass Ejections
    CMEs
    Opis:
    Observations of type II and III solar bursts indicate that while type III bursts may appear at any altitude, from the very low corona into interplanetary space, type II solar bursts do not act the same way. This work focuses on recent observations in the radio region on the low frequency region from 45 MHz to 870 MHz. Our analysis employed the accuracy of the daily solar burst measurements of e-CALLISTO network. It was found that solar burst type II explode quite minimum with 1-2 events from 2006 - 2010. However, the data 2011 for solar burst type II increases drastically with 16 events has been recorded. The occurrences of Coronal Mass Ejections (CMEs) events are also increasing up to four times in 2011. Most of the both events can be observed in the range of 150 MHz till 500 MHz. Overall, we can say that the range of photon energy for solar burst type III is between 7.737 x 10-7 eV to 1.569 x 10-6 eV. In the case of solar burst type II, the distribution of energy is much smaller with 1.596 x 10-6 eV to 6.906 x 10-6 eV. Detailed investigation of solar burst will concern the 2011 data seem to show a significant trend for both types. We showed that the increasing of both solar burst events via years implies directing an increasing of solar activities including sunspot number, solar flare and Coronal Mass Ejections (CMEs) events. It is expected that both types will increase gradually in the beginning of 2014.
    Źródło:
    International Letters of Chemistry, Physics and Astronomy; 2014, 18; 103-112
    2299-3843
    Pojawia się w:
    International Letters of Chemistry, Physics and Astronomy
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Some remarks of type III error for directional two-tailed test
    Uwagi o błędzie iii rodzaju dla kierunkowych testów o dwustronnym obszarze krytycznym
    Autorzy:
    Trzpiot, Grażyna
    Powiązania:
    https://bibliotekanauki.pl/articles/586490.pdf
    Data publikacji:
    2015
    Wydawca:
    Uniwersytet Ekonomiczny w Katowicach
    Tematy:
    Power of test
    Type I error rates
    Type III error rates
    Błąd I rodzaju
    Błąd III rodzaju
    Moc testu
    Opis:
    The major objective of this study was to investigate the effects of non-normality on Type III error rates for ANOVA F and its commonly recommended parametric counterparts namely Alexander-Govern test. The major objective of this study was to investigate the effects of non-normality on Type III error rates for ANOVA. Therefore these tests were compared in terms of Type III error rates across the variety of population distributions, mean difference (effect size), and sample sizes
    Główny cel tej pracy to zbadanie konsekwencji braku normalności rozkładu dla błędu III rodzaju w teście ANOVA F oraz jego parametrycznym odpowiedniku, mianowicie w teście znanym jako Alexander Govern. Testy zostały porównane pod względem poziomu błędów III rodzaju przez wybór różnych rozkładów zmiennych losowych, o różnych średnich oraz wariancjach (wielkość efektu) oraz różnych (małych) wielkościach próby
    Źródło:
    Studia Ekonomiczne; 2015, 219; 5-16
    2083-8611
    Pojawia się w:
    Studia Ekonomiczne
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    An Analysis of Antenna Temperature and Radar Cross Section of Log Periodic Dipole Antenna
    Autorzy:
    Hamidi, Z. S.
    Saad, M. Azren Mat
    Shariff, N. N. M.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/1192599.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Sun
    Log Periodic Dipole Antenna
    type III
    radio region
    antenna temperature radar cross section
    Opis:
    The LPDA antenna because it is very suitable and economic amount the types of antennas. It consists of an array of dipoles in which their lengths and spacing are arranged in a log periodic manner, but not all elements in the system are active on a single frequency of operation. The temperature or Antenna Noise Temperature depends on its gain pattern and the thermal environment that it is placed in. We need to design an antenna that can detect the data and monitor the solar burst type III in radio region. It must be sensitive to a broad frequency range and angular distribution of the incident radio pulse and capable to handle the noise issue that is necessary to gain the pure signal. With large instantaneous bandwidths and high spectral resolutions, these instruments will provide increased imaging sensitivity and enable detailed measurements of the dynamic solar burst. For standardized the time, GPS clock is used to control the sampling time of the spectrometer and a tracking controller control the antenna direction. In conclusion, LPDA is the most practical antennas provide general broadband transmission and reception in a wide range of frequency.
    Źródło:
    World Scientific News; 2016, 55; 126-136
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    The Tendencies Group Type III Burst Form Type II Burst During Low activity
    Autorzy:
    Hamidi, Z. S.
    Mokthtar, Fatin Nabila
    Shariff, N. N. M.
    Ali, Marhana Omar
    Husien, Nurulhazwani
    Sabri, S. N. U.
    Zainol, N. H.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/1191365.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Coronal Mass Ejections (CMEs)
    X-ray region
    radio region
    solar burst
    sun
    sun type II
    sun type III
    Opis:
    Using the e-CALLISTO network radio observations on 1st June 2015, we present an analysis of the complex type III and type II solar radio bursts during low activity. This event occurred on 1st July 2015 at 13:52 UT (complex solar burst type III) and 13:40 UT - 13:44 UT (solar burst type II). Solar burst type detected at (i) BIR, (ii) BLENSW, (iii) Essen, (iv) Glascow (v) Osra, (vi) Rwanda. The spectral shape consists of high flux densities at meter wavelengths. The energy going into plasma heating during each flare was estimated by computing the time evolution of the energy content of the thermal plasma and obtaining the peak value. This constitutes a lower limit to the thermal energy, since it does not account for the cooling of the plasma prior to this time nor to any heating at later times. It is also believed that the meter wavelength branch of the this type III spectrum may be attributable to second-phase accelerated electrons to form type II burst. There are four sunspots of the active regions (AR2355, AR2356, AR2357, and AR2358) during this event. The solar wind recorded during the event is 342.4 km/s and the density of the proton recorded is 4.1 protons/cm3. Moreover, the are some evidence that radio-quiet CMEs mostly came from the edges of the sun. The main goal of this study was to determine whether is there any possibilities that the radio burst can be formed even the Sun is at low activity and this event is one of the candidate events.
    Źródło:
    World Scientific News; 2016, 34; 121-134
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Disturbances of Solar Eruption From Active Region AR1613
    Autorzy:
    Hamidi, Z. S.
    Shariff, N. N. M.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/411713.pdf
    Data publikacji:
    2014
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    solar radio emission
    solar burst type III
    e-CALLISTO
    solar flare
    Active Region AR1613
    Opis:
    The paper describes an investigation of the solar radio bursts of spectral type III due to disturbances of the active region AR 1613. A solar flare occurred on 2012 November 15, between 2:00 UT to 3:30 UT. The sequence images from a burst from our site revealed that although the solar flare is considered moderate, it is still possible to obtain the solar burst type III in a single and group forms within one and half hour. It can easily produce misleading results in terms of non-thermal electron density and magnetic field strength. The burst is originated in the same active region of the solar corona. The C-6 level enhancement was detected in GOES 1.8 a soft X-ray. Based on the results, we suggest that radio wave source motion manifests the displacement of particle sites caused by plasma eruptions. Time variability in the emission may due to the changes in the electron density. The group and individual solar burst type III can be related to the distance travelled before an electron beam becomes unstable to Langmuir waves. In conclusion, the interactions non-thermal electron and magnetic trapping can influence the transporting of electrons and this is still a subject of interest of intense investigation.
    Źródło:
    International Letters of Chemistry, Physics and Astronomy; 2014, 13, 1; 77-87
    2299-3843
    Pojawia się w:
    International Letters of Chemistry, Physics and Astronomy
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Design of small molecule inhibitors of type III secretion system ATPase EscN from enteropathogenic Escherichia coli
    Autorzy:
    Bzdzion, Lukasz
    Krezel, Hanna
    Wrzeszcz, Karol
    Grzegorek, Irmina
    Nowinska, Katarzyna
    Chodaczek, Grzegorz
    Swietnicki, Wieslaw
    Powiązania:
    https://bibliotekanauki.pl/articles/1038684.pdf
    Data publikacji:
    2017
    Wydawca:
    Polskie Towarzystwo Biochemiczne
    Tematy:
    Escherichia coli (E. coli)
    type III secretion system (T3SS)
    enzyme inhibitor
    small molecule
    Opis:
    Enteropathogenic E. coli (EPEC) is a human pathogen using type III secretion system for delivery of proteins directly into the human host. The system contains a single ATPase, EscN, which is essential for uncoupling of proteins from their complexes with chaperones before the delivery. The structure of EscN ATPase (PDB code: 2obm) was used to screen computationally for small molecule inhibitors blocking its active site. Two lead candidates were examined but only one, Compound 54, was selected for further optimization. After extended QSAR optimization, two derivatives were found to be competitive inhibitors of EscN capable of blocking ATPase activity with a Ki below 50 µM. One candidate, WEN05-03, with a Ki=16±2 µM, was also minimally toxic to mammalian cells as determined by other assays. In the cell infection model of HeLa cells with EPEC, Compound WEN05-03 completely blocked actin cluster formation at 100 µM concentration, when analyzed by confocal microscopy. The second best inhibitor of EscN ATPase activity was WEN04-34 with a Ki=46±2 µM. However, the compound was highly toxic to the BALB/3T3 cell line. In summary, the work identifies a compound blocking bacterial ATPase in its active site without causing cellular toxicity to the host cells. It is the first report showing feasibility of using bacterial virulence system ATPase as a target for safe, non-toxic compounds and offering a proof-of-concept for non-antibiotic alternatives.
    Źródło:
    Acta Biochimica Polonica; 2017, 64, 1; 49-63
    0001-527X
    Pojawia się w:
    Acta Biochimica Polonica
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    An Analysis of the Electron Density and Drift Rate of Solar Burst Type III During 13th of May 2015
    Autorzy:
    Ali, M. O.
    Hamidi, Z. S.
    Shariff, N. N. M.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/1192997.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Coronal Mass Ejections (CMEs)
    Sun
    X-ray region
    radio region
    solar burst
    solar flare
    type III
    Opis:
    During 13th of May 2015, the solar wind is very high velocity, which is 733 kms-1 as compared to 367.5 kms-1. It is believed that the plasma–magnetic field interactions in the solar corona can produce suprathermal electron populations over periods from tens of minutes to several hours, and the interactions of wave-particle and wave-wave lead to characteristic fine structures of the emission. An intense and broad solar radio burst type II was recorded by CALLISTO spectrometer from 20-85 MHz. Using data from a the Blein observatory, the complex structure of solar burst type III can also be found in the early stage of the formation of type III solar burst type event due to active region AR 12339. The drift rate of solar burst type III exceeds 1.0 MHz/s with 6.318 x1012 e/m3 a density of electron in the solar corona. There were also 2 groups of solar radio burst type III were observed. This CME was detected at 08:36 UT which is 1and ½ hour after the solar burst detected. This event shows a strong radiation in radio region, but not in X-ray region.
    Źródło:
    World Scientific News; 2016, 31; 1-11
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Implementation and Analysis of Mathematical Modeled Drive Train System in Type III Wind Turbines Using Computational Fluid Dynamics
    Autorzy:
    Kabat, Subash Ranjan
    Panigrahi, Chinmoy Kumar
    Ganthia, Bibhu Prasad
    Barik, Subrat Kumar
    Nayak, Byamakesh
    Powiązania:
    https://bibliotekanauki.pl/articles/2022489.pdf
    Data publikacji:
    2022
    Wydawca:
    Stowarzyszenie Inżynierów i Techników Mechaników Polskich
    Tematy:
    type III wind turbines
    gear train
    pitch control
    gear ratio
    pitch angle
    yaw system
    angular velocity
    CFD
    Opis:
    This paper is based on designing a modified rotor for a drivetrain in a Type-III wind turbine system for maximum power generation to work effectively under low and high wind speed and its variation. In this paper three drive trains are designed for the gearbox to provide regulated torque and thrust force. For time to time variation in wind speed the voltage sag and during over speed condition voltage swell problem can be solved by using this modified design. The pitch control, gear box and yaw of the wind turbine basically focused for modification. Mainly the gear box for the rotor causes sluggish motion of the rotor during low wind speed. This paper explained the design of modified rotor control for the gear box in DFIG based (Type-III) wind turbine. Also in this paper how the modified rotor system can be helpful for reactive power control highlighted with comparison with existing models. For designing MATLAB Simulink platform is taken and validated using CFD mechanical design analysis. Using these types of modified drive trains maximum power for the wind turbines is enhanced by 40–60% of its reference value.
    Źródło:
    Advances in Science and Technology. Research Journal; 2022, 16, 1; 180-189
    2299-8624
    Pojawia się w:
    Advances in Science and Technology. Research Journal
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Statistical Analysis of Some Meteorological Variables Data for Sokoto and its Vicinity
    Autorzy:
    Hassan, Z.
    Ajibola, T. B.
    Powiązania:
    https://bibliotekanauki.pl/articles/1193862.pdf
    Data publikacji:
    2015
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Gumbel
    Meteorological variables
    Normal
    Pearson and Log-pearson type III
    Statistical Analysis
    relative humidity
    solar radiation
    some meteorological variables
    Opis:
    This study aims at studying the characteristics of some meteorological variables in Sokoto and its vicinity using probability distribution models. The thirty one (31) years data (i.e 1980-2010) were collected at Nigerian Meteorological Agency (Nimet) Oshodi and the data were subjected to various probability distribution analyses in order to resolute the best fit probability functions for each meteorological variables. The variables measured consist of Relative humidity, Rainfall, Temperature, Sunshine hours, Solar radiation, wind speed and Evaporation pitche. Whereas the probability distribution models adopt were Normal, Gumbel, Pearson type III and Log-Pearson type III distribution functions. Numerical equation were recognized and used to forecast the variables. Goodness of fit tests such as chi-square, correlation coefficient and coefficient of determination were carried out to obtain the reliability of the forecasted values. The model that satisfies the statistical tests conditions mostly was selected as the best fit model. The study revealed that Rainfall, wind speed, evaporation pitche are best fitted by Log-pearson type III probability distribution model, whereas the Relative humidity, solar radiation, sunshine hours and temperature the best model is Gumbel probability distribution.
    Źródło:
    World Scientific News; 2015, 24; 8-17
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    A Fatigue Fracture Study on TDCB Aluminum Foam Specimen of Type Mode III Bonded with Adhesive
    Autorzy:
    Lee, J. H.
    Cho, J. U.
    Powiązania:
    https://bibliotekanauki.pl/articles/356731.pdf
    Data publikacji:
    2017
    Wydawca:
    Polska Akademia Nauk. Czytelnia Czasopism PAN
    Tematy:
    aluminum foam
    fatigue fracture
    fatigue analysis
    load
    Mode III type
    specimen thickness
    Opis:
    This paper studies the characteristics of junction structure of closed-cell type aluminum foam, which is generally used as a shock absorber. TDCB specimens were designed for mode III type with thickness as a variable and performed a fatigue experiment on them by thickness. As the result, the load value of all specimens peaks under 0 to 25 cycles and decreases as the cycles increase. As the specimen thickens by 10 mm, the maximum load value is 1.2 times. When the thickness increases by 20 mm, the maximum value increases by 1.5 times. This study result can be utilized by investigating the mechanical characteristics of TDCB specimens for mode III type under fatigue loading conditions systematically and efficiently.
    Źródło:
    Archives of Metallurgy and Materials; 2017, 62, 2B; 1359-1362
    1733-3490
    Pojawia się w:
    Archives of Metallurgy and Materials
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    An Analysis of Solar Burst Type II, III, and IV and Determination of a Drift Rate of a Single Type III Solar Burst
    Autorzy:
    Hamidi, Z. S.
    Ibrahim, M. B.
    Shariff, N. N. M.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/411732.pdf
    Data publikacji:
    2014
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    sun
    solar burst
    type II,III,IV
    radio region
    X-ray region
    solar flare
    active region
    Opis:
    The main feature of solar radio type II, III and IV burst is outlined. In this event there are three combinations of bursts that related to the solar flare phenomenon on 6th July 2012. This event is one of good example to observe how far the influence of type II burst could impact the formation of type IV burst and III solar bursts. At first stage, it was observed that a sub-type of H burst form within 2 minutes before type IV solar burst form. The type IV burst is due to the eruption of active region AR 1515 with a fine structure (FS). We used a Blein CALLISTO data in this case. Further analysis also showed that the total energy of the burst are in the range of 4.875 × 10-25 J to 8.48 × 10-25 J and plasma frequency is equal to 1.24 × 104 Hz. Therefore, we could say that in this case, before the solar burst type III occurred, the ejection of CMEs already ejected.
    Źródło:
    International Letters of Chemistry, Physics and Astronomy; 2014, 19, 2; 160-170
    2299-3843
    Pojawia się w:
    International Letters of Chemistry, Physics and Astronomy
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Verification of the Methods for Calculating the Probable Maximum Flow in the Widawa River in the Aspect of Water Management in the Michalice Reservoir
    Weryfikacja metod obliczania przepływów maksymalnych prawdopodobnych w rzece Widawie w aspekcie gospodarki wodnej zbiornika Michalice
    Autorzy:
    Gruss, Łukasz
    Wiatkowski, Mirosław
    Buta, Bogna
    Tomczyk, Paweł
    Powiązania:
    https://bibliotekanauki.pl/articles/1811751.pdf
    Data publikacji:
    2019
    Wydawca:
    Politechnika Koszalińska. Wydawnictwo Uczelniane
    Tematy:
    water reservoirs
    log-normal distribution
    Pearson type III distribution
    Weibull distribution
    maximum flow estimation
    Flood Frequency Analysis
    IMGW method
    zbiorniki wodne
    rozkład logarytmiczno-normalny
    rozkład Pearsona III typu
    rozkład Weibulla
    wyznaczanie przepływów maksymalnych
    metoda IMGW
    Opis:
    Flows with a given probability of exceedance are important from the point of view of water management, especially in water reservoirs. By determining these flows, it is possible to design a reservoir adapted to local conditions that will operate in line with the assumed function. Various methods exist in the world for determining the probable maximum flows; these methods are based on various assumptions. The aim of the article is to verify and assess the applicability of the Flood Frequency Analysis (FFA) and the IMGW method for use in catchments of controlled rivers where a retention reservoir was built during the hydrological observation period. This is important in updating the water management instructions and in designing new retention reservoirs. The authors undertook to investigate whether a series of maximum flows prepared for the IMGW method allows one to recognize the regime change, caused by the construction of the retention reservoir, in the water gauge Zbytowa profile on the Widawa River, using the Mann-Kendall test. The following distributions were used in the study: Pearson type III, log-normal and Weibull. The Mann-Kendall test showed homogeneity of three observational series: 1971-2000, 2001-2017 and 1971-2017 prepared for the FFA method despite the fact that in 2001 the Michalice retention reservoir was commissioned on the Widawa river and the water management in the basin changed this watercourse. However, the observational series prepared for the IMGW method were homogenous only prior to the construction of the reservoir (1971-2000). The observational series prepared in this way enabled the Mann-Kandall test to exclude the homogeneous series caused by the regime change as a result of the construction and operation of the Michalice retention reservoir. Only after the construction of the retention reservoir the observational series from the winter half-year were homogeneous. This is due to the fact that the flows in the winter half-year are definitely lower than those in the summer half-year. The best-fitting distribution for the empirical distribution for the Widawa (the Zbytowa profile) in the analyzed series is a log-normal distribution that can be used to calculate the probable maximum flows needed to update the reservoir's water management instructions. The Wilcoxon test showed no difference between the calculation methods analyzed and used to estimate the probable maximum flows in the Zbytowa profile on the Widawa river. Therefore, as a method for calculating the probable maximum flows for the Widawa river (the Zbytowa profile) in the aspect of managing the Michalice reservoir or some other river with controlled catchment and parameters similar to those of the Widawa (in the Zbytowa profile), one can recommend either of the two analyzed methods: both FFA and IMGW.
    Przepływy o zadanym prawdopodobieństwie przewyższenia są istotne z punktu widzenia gospodarowania wodami na zbiornikach wodnych. Dzięki wyznaczeniu tych przepływów możliwe jest zaprojektowanie zbiornika dostosowanego do lokalnych warunków, który będzie funkcjonował zgodnie z założoną funkcją. Na świecie obowiązują różne metody wyznaczania przepływów maksymalnych prawdopodobnych, które bazują na odmiennych założeniach. Celem artykułu jest weryfikacja i ocena możliwości zastosowania metody Flood Frequency Analysis (FFA) i metody IMGW do zastosowania w zlewniach rzek kontrolowanych, na których w okresie obserwacji hydrologicznej wybudowano zbiornik retencyjny. Ma to znaczenie w aktualizacji instrukcji gospodarowania wodą oraz w projektowaniu nowych zbiorników retencyjnych. Autorzy podjęli się zbadania czy serie przepływów maksymalnych przygotowane dla metody IMGW pozwalają na rozpoznanie zmiany reżimu, w rzece Widawie w przekroju Zbytowa, przy pomocy testu Manna-Kendalla, spowodowanej wybudowaniem zbiornika retencyjnego. W pracy wykorzystano następujące rozkłady: Pearsona typ III, logarytmiczno-normalnego oraz rozkład Weibulla. Test Manna-Kendalla wykazał jednorodności trzech serii obserwacyjnych: 1971-2000, 2001-2017 i 1971-2017 przygotowanych dla metody FFA pomimo, że na rzece Widawie w 2001 roku został oddany do eksploatacji zbiornik retencyjny Michalice i zmieniło się gospodarowanie wodą w zlewni tego cieku. Natomiast serie obserwacyjne sporządzone dla metody IMGW były jednorodne jedynie przed budową zbiornika (okres 1971-2000). Tak przygotowana seria obserwacyjna umożliwiła testowi Manna-Kandalla wykluczyć serie jednorodne spowodowane zmianą reżimu na skutek wybudowania i pracy zbiornika retencyjnego Michalice. Jedynie po budowie zbiornika retencyjnego serie obserwacyjne z półrocza zimowego były jednorodne. Jest to spowodowane tym, że przepływy w półroczu zimowym są zdecydowanie niższe niż przepływy w półroczu letnim. Najbardziej dopasowanym rozkładem zmiennej Qmax dla rzeki Widawy (profil Zbytowa) w analizowanych seriach jest rozkład logarytmiczno-normalny, który może zostać wykorzystany do obliczeń przepływów maksymalnych prawdopodobnych potrzebnych do aktualizacji instrukcji gospodarki wodnej zbiornika. Test Wilcoxona wykazał, brak różnic pomiędzy analizowanymi metodami obliczeniowymi użytymi do obliczeń maksymalnych przepływów o określonym prawdopodobieństwie przewyższenia rzeki Widawy (profil Zbytowa), dlatego też jako metodę do obliczania przepływów maksymalnych prawdopodobnych w zlewni rzeki Widawy w profilu Zbytowa w aspekcie gospodarowania wodami zbiornika retencyjnego Michalice lub innej rzeki o zlewni kontrolowanej o podobnych parametrach zlewni co zlewnia rzeki Widawa (profil Zbytowa), można wskazać obie analizowane metody: FFA i IMGW.
    Źródło:
    Rocznik Ochrona Środowiska; 2019, Tom 21, cz. 1; 566-585
    1506-218X
    Pojawia się w:
    Rocznik Ochrona Środowiska
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
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