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Tytuł:
Particle swarm optimization algorithm based low cost magnetometer calibration
Autorzy:
Ali, A.
Siddharth, S.
Syed, Z.
El-Sheimy, N.
Powiązania:
https://bibliotekanauki.pl/articles/129567.pdf
Data publikacji:
2011
Wydawca:
Stowarzyszenie Geodetów Polskich
Tematy:
artificial intelligence
systems
measurement
navigation
algorithm
sensor
sztuczna inteligencja
systemy
pomiar
nawigacja
algorytm
Opis:
Inertial Navigation Systems (INS) consist of accelerometers, gyroscopes and a microprocessor provide inertial digital data from which position and orientation is obtained by integrating the specific forces and rotation rates. In addition to the accelerometers and gyroscopes, magnetometers can be used to derive the absolute user heading based on Earth’s magnetic field. Unfortunately, the measurements of the magnetic field obtained with low cost sensors are corrupted by several errors including manufacturing defects and external electro-magnetic fields. Consequently, proper calibration of the magnetometer is required to achieve high accuracy heading measurements. In this paper, a Particle Swarm Optimization (PSO) based calibration algorithm is presented to estimate the values of the bias and scale factor of low cost magnetometer. The main advantage of this technique is the use of the artificial intelligence which does not need any error modeling or awareness of the nonlinearity. The estimated bias and scale factor errors from the proposed algorithm improve the heading accuracy and the results are also statistically significant. Also, it can help in the development of the Pedestrian Navigation Devices (PNDs) when combined with the INS and GPS/Wi-Fi especially in the indoor environments.
Źródło:
Archiwum Fotogrametrii, Kartografii i Teledetekcji; 2011, 22; 9-23
2083-2214
2391-9477
Pojawia się w:
Archiwum Fotogrametrii, Kartografii i Teledetekcji
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
First Report on Fusarium brachygibbosum Isolate FIR 16_ITS Isolated from Iraqi Wheat Plant
Autorzy:
Ali, Hamdia Z.
Hameed, Mahdi S.
Abdulrahman, Abdulrahman A.
Saood, Hutham M.
Powiązania:
https://bibliotekanauki.pl/articles/123408.pdf
Data publikacji:
2020
Wydawca:
Polskie Towarzystwo Inżynierii Ekologicznej
Tematy:
phylogenetic analysis
rDNA
Iraq
Opis:
In this study, the Fusarium Brachygibbosum fungus isolate FIR 16_ITS was isolated for the first time from the infected wheat plants in Iraq, during the winter of 2018, in the AL-Tewatha region – 20 km south east of Baghdad. In order to verify the identity of the species of the F. brachygibbosum isolate FIR 16_ITS with the growth symptoms on the wheat plants, the wheat seeds and tissue plants were obtained and used as a source for the re-isolation of the infection agent. F. brachygibbosum isolate FIR 16_ITS was hardly identified using visual approach. However, a molecular technique is important in verifying the species of F. brachygibbosum isolate FIR 16_ITS. The isolate obtained was used for the extraction of DNA and later used for the molecular identification and phylogenetic analyses based on rDNA-internal transcribed region (ITS) primer sets. The authors successfully obtained the amplified products of the ITS-rDNA region, and a sequence analysis indicated that the Fusarium sp. isolate FIR 16_ITS species screened in this study belonged to the F. brachygibbosum species. It was recorded in the NCBI under the following information NCBI; BioSample; Accession no.; SAMN11408139; ID: 11408139 and NCBI; BioProject; Accession no.; PRJNA532637; ID: 679434 (Locus Tag Prefix; E7750).
Źródło:
Journal of Ecological Engineering; 2020, 21, 3; 81-86
2299-8993
Pojawia się w:
Journal of Ecological Engineering
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
A Simulation for Detecting Nonlinear Echoes from Microbubbles Packets
Autorzy:
Ali, M. G. S.
Elsayed, N. Z.
Eid, E. A.
Powiązania:
https://bibliotekanauki.pl/articles/177697.pdf
Data publikacji:
2015
Wydawca:
Polska Akademia Nauk. Czytelnia Czasopism PAN
Tematy:
microbubbles packets
harmonic component
acoustic
radial dynamic
pressure spectrum
Opis:
This work presents a simulation of the response of packets of microbubbles in an ultrasonic pulse-echo scan line. Rayleigh-Plesset equation has been used to predict the echo from numerically obtained radial dynamics of microbubbles. Varying the number of scattering microbubbles on the pulse wave form has been discussed. To improve microbubble-specific imaging at high frequencies, the subharmonic and second harmonic signals from individual microbubbles as well as microbubbles packets were simulated as a function of size and pressure. Two different modes of harmonic generation have been distinguished. The strength and bandwidth of the subharmonic component in the scattering spectrum of microbubbles is greater than that of the second harmonic. The pressure spectra provide quantitative and detailed information on the dynamic behaviour of ultrasound contrast agent microbubbles packet.
Źródło:
Archives of Acoustics; 2015, 40, 2; 151-157
0137-5075
Pojawia się w:
Archives of Acoustics
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
An Approach to Design Broadband Air Backed Piezoelectric Sensor
Autorzy:
Ali, M. G. S.
Elsayed, N. Z.
Eid, E. A.
Powiązania:
https://bibliotekanauki.pl/articles/176360.pdf
Data publikacji:
2015
Wydawca:
Polska Akademia Nauk. Czytelnia Czasopism PAN
Tematy:
piezoelectric
equivalent circuits
impulse response
frequency response
matching layers
z-transform
Opis:
In this work, an approach to the design of broadband thickness-mode piezoelectric transducer is presented. In this approach, simulation of discrete time model of the impulse response of matched and backed piezoelectric transducer is used to design high sensitivity, broad bandwidth, and short-duration impulse response transducers. The effect of matching the performance of transmitting and receiving air backed PZT-5A transducer working into water load is studied. The optimum acoustical characteristics of the quarter wavelength matching layers are determined by a compromise between sensitivity and pulse duration. The thickness of bonding layers is smaller than that of the quarter wavelength matching layers so that they do not change the resonance peak significantly. Our calculations show that the −3 dB air backed transducer bandwidth can be improved considerably by using quarter wavelength matching layers. The computer model developed in this work to predict the behavior of multilayer structures driven by a transient waveform agrees well with measured results. Furthermore, the advantage of this this model over other approaches is that the time signal for optimum set of matching layers can be predicted rapidly.
Źródło:
Archives of Acoustics; 2015, 40, 1; 3-10
0137-5075
Pojawia się w:
Archives of Acoustics
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:
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:
Erbium-doped fiber ring laser dynamical analysis for chaos message masking scheme
Autorzy:
Ali, S. Z.
Islam, M. K.
Powiązania:
https://bibliotekanauki.pl/articles/173276.pdf
Data publikacji:
2017
Wydawca:
Politechnika Wrocławska. Oficyna Wydawnicza Politechniki Wrocławskiej
Tematy:
erbium-doped fiber ring laser chaos
optical chaos
chaos message masking
Lyapunov exponent
secure optical communication
Opis:
A detailed dynamical analysis of erbium-doped fiber ring laser cavity loss configuration for the chaos message masking scheme is carried out to optimize the generation of high quality chaos. A threefold increase in Lyapunov exponent implying higher security, and a significant increase in chaos bandwidth is achieved, both ideal for secure optical communication and nonlinear chaotic applications. The pulsed chaos is chaotic in a pulse time interval in addition to the amplitude resulting in better concealment of data pulses in a time domain. The chaos spectrum is a flat broadband and rich in spikes making spectral detection of a message more difficult. The range of five key parameters for which erbium-doped fiber ring laser retains its chaotic behaviour is also increased significantly reducing the effectiveness of a brute force attack to guess the erbium-doped fiber ring laser parameters. The chaos message masking scheme provides a higher security in comparison with additive chaos modulation scheme for implementation of chaotic optical communication using erbium- doped fiber ring laser. The security of a complete end-to-end chaotic optical communication system is tested by launching a spectral attack to estimate the message signal. The message signal clearly hides in a stronger chaotic signal and its spectral contents are not discernible.
Źródło:
Optica Applicata; 2017, 47, 3; 395-410
0078-5466
1899-7015
Pojawia się w:
Optica Applicata
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
Ethnobotanical knowledge and folk medicinal significance of the flora of district Gujrat, Punjab, Pakistan
Autorzy:
Ali, S.S.
Hussain, K.
Nawaz, K.
Bhatti, K.H.
Bashir, Z.
Nazeer, A.
Arif, U.
Jafar, S.
Siddiqi, E.H.
Powiązania:
https://bibliotekanauki.pl/articles/2049056.pdf
Data publikacji:
2020
Wydawca:
Instytut Włókien Naturalnych i Roślin Zielarskich
Tematy:
District Gujrat
medicine
ethnomedicinal flora
survey
native people
prowincja Gujrat
lek
rośliny lecznicze używane w medycynie ludowej
rdzenni mieszkańcy
badanie ankietowe
Opis:
Introduction: Medicinal plants are the natural source of medicines used in treatment of many diseases among local communities of various countries. It is also the raw material for the pharmaceutical industry. Pakistan is a country with a variety of medicinal plants, comprehensively studied in some areas, while others still need more studies of their flora. Objectives: The study was performed to catalogue the flora of district Gujrat, Punjab, Pakistan and to assess its ethnomedicinal importance. Methods: A field survey was conducted in the Gujrat district (including Sarai Alamgir, Gujrat and Kharian) in 2019–2020 to collect the flora. Nearly 200 people of various age groups were interviewed and the questionnaire was filled, the gender and professions of the participants were also noted. Results: The plant species collected belonged to 32 different Angiosperm families i.e. Poaceae, Brassicaceae, Fabaceae, Asteraceae, Moraceae, Amaranthaceae, Apiaceae, Myrtaceae, Rutaceae, Solanaceae, Malvaceae, Euphorbiaceae and Lamiaceae. The obtained material consisted of 30 herbs, 20 shrubs and 22 trees. The floral parts used most often were leaves (63%) followed by: flower (41%), fruit (28%), stem (16%), seed (16%), bark (14%), root (13%), whole plant (12%), underground part (3%) and latex (3%). According to the study, the highest RFC (Relative Frequency of Citation) values were 0.1 in Cassia fistula L. (0.25) and the smallest RFC values were observed in Stellaria media (L.) Vill. – 0.025. The highest UV (Use Values) were noted for Achyranthes aspera L. at 0.9. In disease category, the highest value (0.67) of ICF (Informant Consensus Factor) was observed for stomach and skin infections, while the lowest ICF value was noted for diabetes and gonorrhoea (0.27). Conclusions: It was concluded that the Gujrat district is rich in useful plants that can be used in the preparation of various medicines as well as be sold on the herbal market.
Źródło:
Herba Polonica; 2020, 66, 1; 37-51
0018-0599
Pojawia się w:
Herba Polonica
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
De la Vallée Poussin Summability, the Combinatorial Sum $\sum_{k=n}^{2n-1}$ (2k/k) and the de la Vallée Poussin Means Expansion
Autorzy:
Ali, Z. S.
Powiązania:
https://bibliotekanauki.pl/articles/357696.pdf
Data publikacji:
2017
Wydawca:
Politechnika Rzeszowska im. Ignacego Łukasiewicza. Oficyna Wydawnicza
Tematy:
complete metric space
hyperbolic space
infinite product
nonexpansive mapping
random weak ergodic property
przestrzeń metryczna całkowita
przestrzeń hiperboliczna
produkt nieskończony
mapowanie
własności ergodyczne
Opis:
In this paper we apply the de la Vallee Poussin sum to a combinatorial Chebyshev sum by Ziad S. Ali in [1]. One outcome of this consideration is the main lemma proving the following combinatorial identity: with $Re(z)$ standing for the real part of z we have \[ \sum_{k=n}^{2n-1}\left({2k \atop k}\right) = Re\left(\left({2k \atop k}\right) \text{}_{2}F_{1}(1, 1/2 + n; 1 + n; 4\right) - \left({4n \atop 2n}\right) \text{}_{2}F_{1}(1, 1/2 + 2n; 1 + 2n; 4) \] Our main lemma will indicate in its proof that the hypergeometric factors \[ _{2}F_{1}(1, 1/2 + n; 1 + n; 4); \text{ and } _{2}F_{1}(1, 1/2 + 2n; 1 + 2n; 4) \] are complex, each having a real and imaginary part. As we apply the de la Vallee Poussin sum to the combinatorial Chebyshev sum generated in the Key lemma by Ziad S. Ali in [1], we see in the proof of the main lemma the extreme importance of the use of the main properties of the gamma function. This represents a second important consideration. A third new outcome are two interesting identities of the hypergeometric type with their new Meijer G function analogues. A fourth outcome is that by the use of the Cauchy integral formula for the derivatives we are able to give a dierent meaning to the sum: \[ \sum_{k=n}^{2n-1}\left({2k \atop k}\right) \] A fifth outcome is that by the use of the Gauss-Kummer formula we are able to make better sense of the expressions \[ \left({2n \atop n}\right)\text{}_{2}F_{1}(1, 1/2 + n; 1 + n; 4), \text{ and } \left({4n \atop 2n}\right)\text{}_{2}F_{1}(1, 1/2 + 2n; 1 + 2n; 4) \] by making use of the series denition of the hypergeometric function. As we continue we notice a new close relation of the Key lemma, and the de la Vallee Poussin means. With this close relation we were able to talk about P the de la Vallee Poussin summability of the two innite series $\sum_{n=0}^{\infty}\cos n\theta$ and $\sum_{n=0}^{\infty}(-1)^{n}\cos n\theta$. Furthermore the application of the de la Vallee Poussin sum to the Key lemma has created two new expansions representing the following functions: \[ \frac{2^{(n-1)}(1+x)^{n}(-1+2^{n}(1+x)^{n})}{n(2x+1)}, \text{ where } x=\cos \theta \] and \[ \frac {-2^{(n-1)}(-1 + 2^{n}(1-x)^{n})(1-x)^{n}} {n(2x - 1)}, \text{ where } x=\cos \theta \] in terms of the de la Vall´ee Poussin means of the two infinite series \[ \sum_{n=0}^{\infty}\cos\theta, \] and \[ \sum_{n=0}^{\infty}(-1)^{n}\cos\theta, \]
Źródło:
Journal of Mathematics and Applications; 2017, 40; 5-20
1733-6775
2300-9926
Pojawia się w:
Journal of Mathematics and Applications
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
Current Situation of Radio Frequency Interference (RFI) Profile at Outdoor and Indoor Sites of Faculty of Applied Sciences, UITM, Malaysia
Autorzy:
Hamidi, Z. S.
Nizamudin, Nur Izzani
Shariff, N. N. M.
Syazwan, M.
Husien, Nurulhazwani
Ali, M. O.
Zainol, N. H.
Ramli, Nabilah
Sabri, S. N. U.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/1191429.pdf
Data publikacji:
2016
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Radio Frequency Interference (RFI)
radio astronomy
RFI sources
Opis:
This Radio Frequency Interference (RFI) study is currently one of a main sub-research in radio astronomy in Malaysia. The main objective of this monitoring is to test and qualify the potential of radio astronomical sources that can be observed in Malaysia generally. Analysis process focuses at indoor and outdoor of Faculty of Applied Sciences, UITM Shah ALAM, Malaysia (latitude: 03°06.534’N, longitude: 101°50.396’E). There are three mobile network communications that operate at the upper band frequency of 1800MHz, which are Maxis (1805-1830 MHz), Celcom (1830-1855 MHz) and Digi (1855-1880 MHz) for GSM/LTE network. We observed that both sites having the highest and second highest peak at the same frequency of 420 MHz and 1835 MHz with the same source, which were due to mobile application followed by the lowest peak due to radio navigation satellite. We verified that the source of RFI of 1835 MHz at the Faculty of Applied Sciences may come from Celcom mobile telecommunication network signal because there is transmitter on top of two Celcom towers. This observation must be continuously done to ensure that RFI level does not increase drastically and to ensure that allocation spectrum band that was reserved for radio astronomy activities was always protected.
Źródło:
World Scientific News; 2016, 40; 23-33
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
Heart-shape Active Region 2529 Producing Strong M6.7 class Solar Flare and Gradual Coronal Mass Ejections
Autorzy:
Hamidi, Z. S.
Omar Ali, M.
Nurul, Hazwani Husien
Sabri, S. N. U.
Zainol, N. H.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/1179601.pdf
Data publikacji:
2017
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Gradual Coronal Mass Ejections
Heart-shape active region
Sun
X-ray region
solar flare
Opis:
The Centre of the Sun is very important to be study because this layer is where the nuclear reaction will be occurred. During large event pre-flare usually continues a few minutes and followed by impulsive phase about 3 to 10 minutes. Solar storms such as solar flare and Coronal Mass Ejections are frequently occurred on the area of the Sun that have strong magnetic field or known as active region The release of the stored free magnetic energy that probably drives a CME can take many forms including (predominantly) mechanical in the form of an expanding CME and erupting filament, electromagnetic emission in the form of a flare, and also in the acceleration of energetic particles, magnetic field reconfiguration and bulk plasma motion. In this study, the data of active region of the Sun was taken from official website of the Langkawi National Observatory. The image of the active region was observed by using 11-inch Celestron telescope with solar filter. This data confirms that there was a strong M class of solar flare during the day due to eruption of AR 2529 was occurred on 18th of April. From the x-ray flux data also, it can be observed that few days before M6.7 class solar flare occurred, there were several C classes of flare. The evolution of small AR 2529 to a big heart-shape forms an eruption that producing strong M6.7 class of flare and three gradual CMEs. This strong flare caused significant impact around the high technologies of Pacific Ocean by fading the signal at frequencies below 15 MHz.
Źródło:
World Scientific News; 2017, 74; 181-193
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
Solar Radio Burst Type III due to M 2.9 Class Flare with a Geomagnetic Disturbance
Autorzy:
Hamidi, Z. S.
Ali, M. O.
Shariff, N. N. M.
Monstein, C.
Zainol, N. H.
Hussien, Nurul Hazwani
Ramli, Nabilah
Farid, M. S.
Powiązania:
https://bibliotekanauki.pl/articles/1190207.pdf
Data publikacji:
2016
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
solar radio burst
solar storm
flare
geomagnetic disturbance
Opis:
Varying forms of solar radio burst were classified by their frequent changes in time, which are known as drift rate. There are 5 types of radio emission were named type I, II, III, IV and V. This paper is highlighted on the type III event which occurred on 27th August 2015. In the IP medium, type III solar radio burst can be classified in three different groups which representing three different situations of electron beam production and propagation which are isolated, complex and storm type III burst. The most powerful manifestation of solar activity is solar flare together with coronal mass ejections, eruptive prominences and the solar wind are the solar events which affect the earth's atmosphere and can cause geomagnetic disturbance. In this study, the effect of M class flare with solar radio burst type III was investigated. During the day, the solar wind proton density seems to be high which is 8.4 protons/cm3 and accompanied by normal solar wind speed of 348.7 km/Sec. Spaceweather.com reported that there is one sunspot was detected (AR2403) and M class of the flare was detected during the day at 0544 UT. The data geomagnetic signal shows that during the day only geomagnetic disturbance that occur no such geomagnetic storm since the sunspot not facing the earth directly.
Źródło:
World Scientific News; 2016, 44; 155-167
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
The Correlation between Solar Flare Phenomena in an X-ray Region and Radio Flux Measurement from January to September 2010
Autorzy:
Hamidi, Z. S.
Shariff, N. N. M.
Ali, M. F.
Monstein, C.
Zulkifli, W. N. A. W.
Ibrahim, M. B.
Arifin, N. S.
Amran, N. A.
Powiązania:
https://bibliotekanauki.pl/articles/411743.pdf
Data publikacji:
2014
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
sun
chromospheres
flares
radio flux
solar activity
Opis:
A short term variation of solar flare in nine months (January 2010 to September 2010) is presented. This paper review and analyze the correlation between radio flux strength measurement and solar flare in the X-ray region. The radio flux measurement data were taken from the National Research Council; Ottawa while hard X-ray emission observed by Royal Observatory of Belgium. 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. As there was no class of an X of solar flare reported at all in this study, we can confirm that there are no major effects that happened on Earth and outer space such as Coronal Mass Ejections (CMEs) and solar storms. We concluded that the Sun shows a very minimum activity towards 24th solar cycle.
Źródło:
International Letters of Chemistry, Physics and Astronomy; 2014, 9; 84-92
2299-3843
Pojawia się w:
International Letters of Chemistry, Physics and Astronomy
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:
The Enlargement of Type II Burst After Type III at AR 12522 on 16th March 2016 In Conjunction With Flare-Related Coronal Mass Ejections Event
Autorzy:
Husien, Nurulhazwani
Hamidi, Z. S.
Shariff, N. N. M.
Ali, M. O.
Zainol, N. H.
Sabri, S. N. U.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/1178545.pdf
Data publikacji:
2017
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Coronal Mass Ejections
Sun
X-ray emission
Opis:
On 16th March 2016 the solar radio burst type II is recorded to appear on spectrograph after the type III formation. These two bursts related to the Coronal Mass Ejections (CMEs) event that recorded by the SOHO spacecraft several minutes before the formation of Type III on the spectrograph. It has been reported that the Type III burst a fast drift compared to the Type II burst. In this paper, the calculation has been proved that the type III burst has a higher drift rate compared to Type II. These two events of Type II and III burst also has been contributing to the formation of C class flare with magnitude of C2.2 It is also proven that the type III burst has a fast drift rate compared to type II burst. In this case, the type III has a fast drift rate of 81% compared to the type II burst. During this event, the active region AR 12522 erupted the C-class X-ray emission with magnitude of C2.2 contribute to these type III and II burst
Źródło:
World Scientific News; 2017, 70, 2; 230-240
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
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