Search

STEM education integrates science, Technology, Engineering, and Mathematics knowledge that is emphasized in Malaysia Education Blueprint 2013-2025. A few STEM elements are drawn in Islamic Education syllabus in the lower forms. This study aims to examine the extent to which STEM elements are absorbed in form one to three Islamic Education syllabus. Qualitative study framework that analyses the extent of STEM elements existence in Islamic Education syllabus based on syllabus perception. Excellent and efficient teaching can inculcate students' interest in science, and the awareness of its integration with Islamic religion is needed for the ummah and Islamic civilization advancement. Keywords: STEM Education, Syllabus, Islamic Education eISSN: 2398-4287 © 2022. The Authors. Published for AMER ABRA cE-Bs by e-International Publishing House, Ltd., UK. This is an open access article under the CC BYNC-ND license (http://creativecommons.org/licenses/by-nc-nd/4.0/). Peer–review under responsibility of AMER (Association of Malaysian Environment-Behaviour Researchers), ABRA (Association of Behavioural Researchers on Asians) and cE-Bs (Centre for Environment-Behaviour Studies), Faculty of Architecture, Planning & Surveying, Universiti Teknologi MARA, Malaysia. DOI: https://doi.org/10.21834/ebpj.v7iSI7%20(Special%20Issue).3805

The purpose of the philanthropic practices in Islamic tradition is not only about Islamic ethics and fiqh, but to enhance the efficiency of welfare distribution and development of the ummah, including the community intelligence. This paper reports the current status of the philanthropic practices that have been utilised in the astronomy field and their effects in buttressing the advancement of Islamic astronomy (falak syar’ie), astronomy, and space science. This paper acts as a preliminary study as part of a bigger research therefore, it is limited to a review of philanthropic practices that have been and are being implemented in astronomy and the extent of their impact in this field. The inductive and deductive approaches were used in analyzing the research data obtained from the literature review. This paper found that philanthropy is a practical mechanism that could be applied in sustaining the development of astronomy and space science knowledge. In Malaysia, the practice of philanthropy from individuals funds in supporting the field of astronomy is seen as quite positive. Nonetheless, this practice is seen as less encouraging within the government, non-profits and corporations. Therefore, it would be great if philanthropic institutions along with strategic fund planning could be established. More structured fund management will lead to intelligible planning for the growth of the astronomy field in this country.

The instability of the Sun’s magnetic field can ignite many eruptive events on the solar surface, including flares, coronal mass ejections, and prominence eruptions. The inner heliosphere environment is affected, and consequently, these events are said to contribute to the celestial weather change. As one of the many eruptive events, a solar flare is of the most frequent due to the magnetic reconnection process in which the accelerated electrons from the reconnection sites escape into the interplanetary space and cause solar radio bursts type III (SRBT III). When it is observed near the Earth, this SRBT III is in the form of radio dynamics spectrum; thus, monitoring this spectrum is vital to the further analysis of the said SRBT III. In this paper, we investigate the background levels: short and long periods of the CALLISTO instruments from two different stations where for each site, a 10-day background-level observation is randomly selected. For the purpose of this study, the mean differences and coefficient of variation (CV) distributions for every frequency channel are determined where most of the frequency channels have displayed small mean differences between these two background levels: short and long periods and the CV distributions as well. These short-period observations, within 15 min of the background levels, are found significant enough to warrant further analysis of the solar radio bursts detected by the CALLISTO instruments.

For around 50 years, a solar flare is among the activities of the Sun that has been evaluated and observed by scientists. The origin of the solar flare is from the sunspot associated with a solar burst. The solar burst can be break into 5 types. Long duration solar bursts have been investigated in this study. There are 15 selected dates that have been chosen from 2019 until 2020. Radio flux and sunspot numbers affiliated with long-duration solar bursts have been analyzed in this paper. As a result, the longest and the shortest solar burst that has been recorded is 535 minutes on 14/04/19 and 36 minutes on 21/03/19 respectively. The Sun is very important to be consistently observed because in rare cases, the flare is very strong and can affect the Earth’s magnetosphere.

An Islamic prayer time has been extensively investigated by astronomers. However, since there are some issues regarding the different views in the fixation of the altitude of Sun, the twilight angle and the latest issues of an extra eight minutes that need to be added for Subh prayer time, therefore it was being re-calculate again. The purpose of this study is to re-identify Subh and Isha solar angle at Besut, Kuala Terengganu by using SQM-LU-DL and to compare official prayer times with the observations by providing time and angle differences to evaluate the correct time frame of Subh and Isha. This study is focused on the sky brightness that was being measured by using Sky Quality Meter-Lens-USB-Data Logger (SQM-LU-DL) to measure the twilight. The data for 2018 is from April until October. For 2019, there are only two months which are February and March with one minute interval in the range of SQM-LU-DL. The observation of the data is based on the pattern of the graph which is the growth curve by plotting the magnitude of the Sun against time. This data can be related to the altitude of the Sun which is the condition to determine the beginning of Subh and Isha prayers time. As the result, the average of theoretical and quantitative measurements of Isha is 17.59° and 17.80°, while for Subh is around 20.26° and 18.69°.

Sunspot is known as the area with the highest solar magnetic activity and has the coolest region compared to its surrounding. It is also influenced by sunspot complexity and magnetic field strength. The huge explosion of solar energetic particles in the interplanetary space due to Coronal Mass Ejections (CMEs) and solar flares is believed due to instability of magnetic field and complexity magnetic field in the sunspot. Due to these events, the intense solar radio emission also known as solar radio bursts were released to the Earth. Delta (δ) sunspot is one of the largest magnetic classification of sunspot and seen mostly released solar flares and CMEs, however, Beta Gamma (βγ) sunspot has the highest formation from 2012 to 2016 compared to other type of bursts and has tendency to produce solar flares and CMEs. The data were collected using Space Weather Website (SWPC) and NOAA, e-CALLISTO network and LPDA. The data were collected within 5 years (2012-2016) and reveals βγ sunspot has (349 counts) (62.77%), followed by βγσ sunspot (160 counts) (28.78%), δ sunspot (39 counts) (7.01%) and βγ sunspot (8 counts) (1.44%), thus, highlights the highest type of magnetic classification occurred on Active Region (AR) was βγ sunspot. Highest formation of βγ sunspot illustrated the complexity of the βγ sunspot due instability of magnetic field inside AR and has tendency to produce flares and CMEs compared to other types of magnetic classifications. Furthermore, βγ sunspot demonstrated a tendency to generate Type II burst, Type III burst, Type IV burst and combination of bursts which we classified as selected events. This finding proved that Type IV burst has the highest formation of burst followed by Type III burst, Type II burst and selected events. Type IV burst has counted for 161 counts (56.29%), Type III burst (100 counts) (34.96%), Type II burst (14 counts) (4.9%) and selected events (11 days) (3.85%). The type of bursts was determined by the range frequency of burst and the duration of burst. The different types of bursts have different ranges of frequency and duration of bursts. Type IV burst displayed the highest formation due its associated phenomena mostly was sunspot where the location of events occurred, followed by Type III burst (solar flares), Type II burst (CMEs) and selected events. These findings were important in solar activity study as prediction and forecast for Solar Cycle 25. These significant findings manage the process of shutting down the system from breakdown due to high energetic particles being released from solar flares and CMES. This prediction can shut down the system in satellites and prevent the power grid and telecommunication system from breakdown.

We present the study of sequence of geomagnetic storm (GMS) and its relation with the two solar flare events on 20th April 2020 and 29th May 2020. The parameter such as solar wind, interplanetary magnetic field (IMF) and Kp index play an important roles and affect the GIC level and climate change. The space weather prediction about solar radio burst and geomagnetic storm can be only possible if we know the activity of the Sun. Solar activity and geomagnetic activity were observed during the time period of both events in order to know whether solar burst associated with the GMS or not. In study we found that solar burst did not depends on GMS however it depends on solar activity meanwhile geomagnetic storm occurred when the Kp index above 5. We also found that the strength of GMS are excellently correlated with solar wind, and IMF thus it support earlier result of investigators. Furthermore, there is no confirmation about how GMS does influence the GIC level. The data of these activities, can be taken from the space weather websites. We have also discussed the various results obtained in present investigation in view recent scenario of geomagnetic storm.

Floods have caused inevitable major disasters around the world as well as in Malaysia. This paper demonstrates that lessons can be taken from the previous flood disasters when developing an effective flood preparedness plan. As a common practice, disaster management is based on a top–down approach or is government-centred. This article attempts to highlight the significance of developing a flood preparedness plan by involving the communities affected. Qualitative analysis was adopted in order to gain in-depth insight of the communities. Two flood-prone communities were chosen: (1) Machang, Kelantan; and (2) Kuala Lipis, Pahang. There were two important things executed by the community for the preparation: (1) community-based disaster risk management; and (2) intensive mutual assistance. https://doi.org/10.4102/jamba.v11i1.598

The solar wind is one of the main properties of the Sun which has a stream of charged particles released from the corona of the Sun. The study of this parameter has started in 1957 and there are a few models that related to prove how the solar wind could escape from the Sun’s gravity. In this paper, we choose the latest solar event that occurred on 16th October 2020 in this new 25th solar cycle. During these months, the Sun considered as active mode and the active region AR2776 potentially contributes high solar activities. Uniquely, a micro solar flare class B formed together with solar burst type II. A very intense flashing which also known as Ellerman bombs can be detected in the optical region. The sunspot number is only 14 and solar wind exceeds up to 306 kms -1 with a density of 4.0 protons/cm 3. We confirmed that AR2776 is a member of Solar Cycle 25.

The main objective of this paper is focused on the overview of log periodic dipole antenna that was constructed and placed at UiTM and the data obtained from the antenna. The LPDA antenna was combined with the CALLISTO spectrometer where this is a program under the International Space Weather Initiative to support new country to be a part of solar astrophysics group. Until now, there are many locations around the world that grab this opportunity to contribute the data from their country so that all people can be benefited from it. The function of the antenna and CALLISTO system is more to monitor the Sun for 24 hours per day. The monitoring of the Sun is important as the activities from it such as solar flares and Coronal Mass Ejections (CMEs) could harm and disturb the technologies such as GPS and satellites. UiTM take this chance to build the log periodic dipole antenna and the data recorded was presented in this paper. The future improvement of the antenna was discussed to obtain the best performance in gaining the data.

The first continuous assessment of night sky brightness (NSB) at Selangor Observatory are presented. The brightness at night sky was monitored over 6 months in 2018, using portable light sensor called the Sky Quality Meter-type USB-Data Logging with a fixed position - pointing towards zenith. From the 179 records of night, the study shows that the average NSB readings at Selangor Observatory is 20.04 ± 0.18 magnitude per square arc second (MPSAS), after excluding the moonlight factor. Meanwhile, during the stable night sky conditions, the most recorded NSB value is 21.1 MPSAS with 0.78 MPSAS range and 21.03 MPSAS in average. Therefore, Selangor Observatory is still a relevant location for the implementation of astronomical work since it has a night sky within Bortle scale Class 4 to 5.

Solar activity is very important to be observed in order to study its effects to Earth’s climate and space weather generally. In order to understand the behavior of the Sun and its activity, developing ground-based instruments is one of the ways to record the occurrence of the activity other than satellites data. We present in this paper our work on the implementation of Log Periodic Dipole Antenna (LPDA). The LPDA has been successfully set up at UiTM Shah Alam, Malaysia in 2016 with high performance with 8.4-meter height and it has achieved gain as high as 7.28 dB. It mainly records solar radio bursts during the occurrence of solar activity and has been operating at frequency range of 45-870 Hz. This project is done under International Space Weather Initiative (ISWI) by using CALLISTO spectrometer at the same frequency range to monitor solar observations in supporting developing countries with latest technologies of instrument. Beneficially in Malaysia, our station contributes half of the data on e-CALLISTO website due to 12 hours Sun exposure compared to other stations in different countries. All types of solar bursts obtained by e-CALISTO are presented in this paper.

This event allows us to investigate the electron density and drift rate of solar burst type II During 1st June 2015. 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 25-80 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 II solar burst type event due to active region AR2358. The drift rate of solar burst type II exceeds 0.03 MHz/s with a density of electron in the solar corona. There are 18 CMEs occurring that day and the distributions of CME speed are between 200 ms-1 to 1100 ms-1 so that the average velocity of the CMEs that occur that day is 1025 m/s. This is one of the largest number of sunspots that have recorded in this year. However, all of these sunspots are quiet and stable and the solar activity remains low. Therefore, it can be observed that only B class of flare from the X-Ray Flux Data.

CALLISTO (Compound Astronomical Low Frequency Low Cost Instrument for Spectroscopy and Transportable Observatory) is one of the projects from ISWI and initiative of United Nation and NASA as a support to help developing countries to monitor activities of the Sun for the whole day. Today, more than 164 instruments at more than 100 locations use this system to do research on the Sun. The objective of this paper is to show that even the activity from the Sun is not too intense and large, the CALLISTO system can detect the signal, hence the importance of this system is acknowledged. This is as a hint for us to use the antenna as the part of the CALLISTO system to get the full coverage all day long with the contributed data from around the world. A weak Coronal Mass Ejection (CME) with the median velocity of 231 km/s was observed on 9th March 2019 by SOHO coronagraph and detected by CALLISTO system from multiple sites of UK, Switzerland and Italy. This faint CME was not giving the high impact to the Earth’s magnetosphere and thus no minor occurrence of the geomagnetic storm.

Night sky brightness is one of the important parameters to be considered in determining the quality of a site for astronomy observation. However, light pollution acts as a major contributor to sky brightness at night. We measure the night sky brightness at Kundasang, Sabah to obtain the first preliminary sky brightness reading. In order to measure light pollution in Kundasang Sabah, Unihedron Sky Quality Meter (SQM-LU-DL) was used for the measurement with a fixed position and oriented towards the zenith. The measurements have been done during the period of July 2018 to February 2019. The measurement is taken between approximately 7 p.m. to 5.30 a.m. everyday. The best night sky brightness reading is on January 5th, 2019 with a value of 21.34 ± 0.7 mag/arcsec2. The preliminary average reading of sky brightness is 20.71 ± 0.2 mag/arcsec2. Comparison with previous similar studies for the same condition of astronomy sites in Malaysia and other locations indicate that Kundasang, Sabah is a suitable location for astronomical observation.

Solar Radio Bursts Type III (SRBT III) and their correlation with solar flares always had been interesting issues. The objective of this research is to study the correlation of SRBT III related to solar flares to magnetic reconnection theory. The importance of this correlation is to enhance the understanding of the particles behaviour during the events over this burst. The data for both SRBT III can be obtained from the e - CALLISTO website. Meanwhile, the data for solar flares were obtained from the Solar Monitor website and Computer Aided CMEs Tracking website respectively. There are 44 data have been collected starting from 2012 until 2017. The Pearson Correlation Coefficient is a method used in obtaining the correlation of the variables of SRBT III and solar flares events. The value of R obtained for the peak flux and the starting frequency of SRBT III is +0.3364. The mean of the peak flux is 6.0 × 10−5W/m2 which is in the M group with a magnitude of 6.0. From this study, they found that the single SRBT III is due to the single magnetic reconnection whereas for the storm and group SRBT III is due to the multiple magnetic reconnections.

Light pollution is regarded as one of environmental issues, although it is often neglected by vast majority of us. It has severe impacts on human health & nocturnal creatures. Due to that, measurement of light pollution is crucial as it serves as an indicator on how polluted our sky. The objective of this paper is to compare light pollution measurement at designated sites. For this paper, we choose four (4) stationary sites that are located according to cardinal directions i.e. Selangor Observatory (BCS), Kuala Lipis (LPS), Besut (BST) and Langkawi National Observatory (ONL). All sites were installed Sky Quality Meter (LU-DL type). The measurement is in magnitude per arc second (mpsas) or abbreviated as mag/arcsec2 unit. The higher the measurement value indicates the less polluted sky. We found that 9th of June 2018 was identified as best day for the four (4) sites based on the average of sky magnitude along night. The less polluted site is LPS site with 21.15 mag/arcsec2 and the worst site is BST with 19.58 mag/arcsec2. Measurement of light pollution in the long run is vital in order to have a reliable dataset and for protection of the night sky brightness.

This study highlights the importance of solar activity observation in radio region which covers 45-870 MHz, which also provides clues on the appearance of magnetic reconnection. It was carried out by utilizing e-CALLISTO data from Glasgow station. On 9th March 2019, intense solar radio bursts type III sparked off and were detected by Glasgow station in the UK at 12.29 UT, that lasted for 15 minutes. There were two bursts that were observed to appear separately by 1-minute interval. Accompanying the bursts formation was a B6.5 flare, the highest flare throughout the day and it was recorded by NOAA at 12.26 UT which was in the time frame of the bursts event. It is believed that the type III bursts were associated to the flare formation as radio emissions were emitted at the beginning of the flare during reconnection. From the analysis, results have shown that multiple magnetic reconnection process took place during the solar activity as indicated by a large group of bursts. However, no extended bursts formed for the rest of the day as well as lack of activity produced by the same region for the following days and that could be a hint of the decay phase of AR 2734. Detailed discussions on the bursts corresponding to the flare activity are discussed in this paper.

Most type I bursts appear in chains of five or more individual bursts. We studied the event of solar type I solar bursts recorded by the Compact Astronomical Low-cost Low-frequency Instrument for Spectroscopy and Transportable Observatory (CALLISTO-ROSEWELL) spectrometer on 11th March 2013 in the frequency range 320–450 MHz. It was observed 5 s after the flare which happens at 16:24:05UT. The drift rate of this burst is 8 MHz/s with a range of energy between 1.4081 × 106 eV to 1.739 × 106 eV. There are six sunspots were producing flares which are AR1691, AR1690, AR19692, AR1693, AR1694, and AR1689. The sunspot number is 89 and the level of energy is proportional to 680 SFU. Solar Burst Type I is normally in a storm structure and become one of the pre-burst stage. In this case, the burst is associated with a large solar flares. Type I solar burst can be as an indicator of pre-solar flare and CMEs if the intensity of the burst is high. The physical conditions inside and outside the source and the emission mechanisms are discussed.

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 37 stations (using 68 instruments) forming this network from more than 96 countries. We investigate the radio frequency interference (RFI) affecting CALLISTO at these stations. We found that the RFI severely affecting CALLISTO within radio astronomical windows below 870 MHz are in the ranges of 80–110 MHz and 460–500 MHz. We also found that all stations are relatively free from RFI at 270–290 MHz. We investigate the general effect of RFI on detection of solar bursts. We considered type III solar bursts on 10th May, 28th June, 6th July and 8th July, type II on 24th April and type IV on 9th March (all in 2012) in order to measure the percentage of RFI level during solar burst in general. The SNR of the strong solar bursts in for these detections have maxima reaching up to 46.20 (for 6th July).

Solar radio burst type III and II is the subject matter that we are focusing on because type II and III burst are seem to have relation to each other. The most common of type III burst is called isolated type III burst which is produced by energetic electron from small scale energy release site on the sun and it is ranging from small bright point to large active region. This stage can be considered as a pre-flare stage that could be a signature of electron acceleration. Nevertheless, the most important is that the nonlinear wave-wave interaction which involving interaction of electrostatic electron plasma that called as Langmuir waves active region radio emissions is believed to be a main subject that relevant with a type III burst. In this study, solar radio bursts are observed by using the CALLISTO spectrometer. The log Periodic Dipole Antenna (LPDA) involved in this search over a broad region centered on the Sun and it covered the range of frequency from 45 MHz-870 MHz and it is connected to the CALLISTO spectrometer. At certain period of time, when the Sun launches billons tones of electrically conducting gas plasma into the space at millions of miles per hours it is assigned that CMEs begin to launches. At this time, the appearance of SRBT III was observed and followed by SRBT II within the time interval of 15 minutes. During flares, large scale of magnetic field structures can be destabilized and be repelled into the interplanetary medium; along with the large mass it contains to form so-called CMEs. Based on the result obtained, the SRBT III is followed by SRBT II which only in short period. During the SRBT II, the solar flare was also appearing and same goes to the CMEs

This paper is highlighted on the duration of time for the Coronal Mass Ejections (CMEs) to occur related to solar flare event and the class of solar burst type III that present within the two phenomenon. It is important to understand the evaluations of solar flare until CMEs mean to be appearing and know the basic characterization of solar radio burst type III. It can be observed that CME is even larger than the sun itself. At certain period of time, when the Sun launches billons tones of electrically conducting gas plasma into the space at millions of miles per hours it is assigned that CMEs begin to launch. The data on 23rd of April was selected whereby; solar radio burst type 3 was detected (about 17:36 UT – 17:44 UT). At 17:40 solar flare with a radio burst and CMEs were produced by the sun. Associated with this event, current condition of solar wind speed is 359.5 km/sec with density of 6.0 protons/ and sunspot number are 118. Those at the high latitude have a chance of aurora due to the small geomagnetic storm.

From the data from a BLEIN Callisto site, we aim to provide a comprehensive description of the synopsis formation and dynamics of a a single solar burst type III and magnetic reconnection effect. The data above is the solar radio burst type iii occurred on 10th September 2005 between 05:44 UT till 06:00 UT.This eruption has started since 5:55 UT with a formation of type III solar burst. The wave emission process of solar radio burst type III from magnetic reconnection region in a solar flare were investigated by using a two-dimensional, that are electromagnetic and relativistic particle-in-cell code. The solar radio burst type III initially impose into two plasma populations : background dense plasma and hot electrons that can be generated by the magnetic reconnection process in a solar flare. The conversion of the energy stored in the magnetic field by a process called the magnetic reconnection released the energy in the solar flares and related phenomena. By the launching the e-CALLISTO network, its prove the existence of the magnetic reconnection on the surface of the sun in radio region.

The formation of detected solar radio burst type II occurred was captured using Compound Astronomical Low Cost Frequency Spectrometer Transportable Observatory (CALLISTO) system which gives a better resolution of a wonderful image than other countries. The phenomenon was found on 2nd November 2014 at 09:39 [UT] in Switzerland. CALLISTO spectrometer device detects and traces a Coronal Mass Ejections (CMEs) phenomenon that causes the occurrence of the solar burst type II. As it happened, the drift rate of the solar radio burst Type II is calculated and discussed in details. Plasma frequency (fp), Langmuir waves and type II radiation relates each other in the establishment of this phenomenon. This paper presents a study of drift rate selected event of solar radio burst type II based on CMEs. The drift rate at this moment was about 3.2 MHz/s which has low drift rate thus the velocity OF THE CMEs was just about 695 km/s shown from NOAA.

The basis of the nonlinear least square fitting is to fit the nonlinear rotation curve model with the observed rotation curve of the Orion dwarf galaxy. It has been the most powerful tool to study the distribution of dark matter in galaxies where it is used to obtain the proper mass model of a galaxy. In this paper, we present the rotation curve fit of Orion dwarf galaxy, corrected for asymmetric drift by using the gradient method of nonlinear least square. Our results showed an excellent agreement between the mass models of cored halo profile with the observed rotation curve. Thus, we can estimate the value of disk mass, MD; the core radius, r0 and core density, ro of the galaxy with 1-s of uncertainty. We finally indicated the dark matter halo distribution as cored dark matter halo with density, 3.9 × 106MŸ kpc-3.

This event allows us to investigate how 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 IV was recorded by CALLISTO spectrometer from 240-360 MHz. Using data from a the KRIM observatory, we aim to provide a comprehensive description of the synopsis formation and dynamics of a a single solar burst type IV event due to active region AR2222. For five minutes, the event exhibited strong pulsations on various time scales and “broad patterns” with a formation of a group type III solar burst. AR 2222 remained the most active region, producing a number of minor C-Class solar flares. The speed of the solar wind also exceeds 370.8 km/second with 10.2 g/cm3 density of proton in the solar corona. The radio flux also shows 171 SFU. Besides, there are 3 active regions, AR2217, AR2219 and AR2222 potentially pose a threat for M-class solar flares. Active region AR2222 have unstable 'beta-gamma' magnetic fields that harbor energy for M-class flares. As a conclusion, we believed that Sun’s activities more active in order to achieve solar maximum cycle at the end of 2014.

Type I solar burst were identified based on data recorded by CALLISTO BLEIN, Switzerland in the period of 17th of January, 2011. Solar Radio Burst Type I is one of the main type of solar burst which is believed to provide a diagnostic of electron acceleration in the corona. This noise storm burst is associated with emerging and growing active regions and last from hours to days. It can be observed that solar radio burst type I is formed within four minutes, although the number of sunspots is just 15. The results of the recent time indicate that Sunspot group 1147 has been mostly quiet since it rounded the eastern limb, but previous week's far side activity shows it is capable of significant eruptions. In 2011, only one day has been detected with spotless day, which means that it is about 7% of overall cases. Probabilities for significant disturbances in Earth's magnetic field are given for three activity levels: active, minor storm, severe storm. From the current conditions in the space weather website on 16th January 2011 that is the first event was shown that the solar wind occurred with a speed of 433.2 km/second while its density about 3.2 protons/cm3. Besides the solar wind, X-ray solar flare with 6 hours maximum: B1 at 1846 UT and 24 hours: B2 at 1544 UT were detected. While type I seem to be an indicator of pre-solar flare and CMEs, 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. We could conclude one active region will not produce a huge explosion of solar phenomena.

Recent data of a complex solar radio burst type II is analyzed and reviewed. The monitoring of solar radio burst was done by using the Compact Astronomical Low cost, Low frequency Instrument for Spectroscopy and Transportable Observatory (CALLISTO) from BLEIN 7 meter dish telescope at ETH, Zurich in frequency range of 25 until 1000 MHz. During the inspection of the X-ray spectrum, we observed that the C3-category flare was caused by a filament of magnetism, which rose up and erupted between 0400 and 0600 UT. This occurred three hours before the signature of solar radio burst type II. There are some of the material in the filament fell back to the sun, causing a flash of X-rays where it hit the Sun surface. This is a Hydra Flare which occurred without sunspots. On the basis of these results, we suggest that a single shock in the leading edge of the CME could be the source of the multiple type II bursts and support the notion that the CME nose and the CME-streamer interaction are the two main mechanisms able to generate the bursts.

Halo event of coronal mass ejections (CMEs) had been once in a while reported in coronagraph observations of the Sun before the Solar and Heliospheric Observatory (SOHO) mission has been carried out. However, since mid-1996 the SOHO Large Angle Spectrometric Coronagraph (LASCO) instruments have observed numerous halo or partial-halo CMEs. Partial halo is when CMEs aimed at Earth which is called as "halo events" because of the way they look in coronagraph images. As the expanding cloud of an Earth-directed CME becomes larger and it appears to envelop the Sun, forming a halo around our star. Statistical interpretation states that most of the halos CMEs occur at average speed of ~957 km/s. In 2015, eight (8) halo CMEs events were detected accompanied by slow partial halo CMEs. Sunspot number, solar radio flux and solar wind involves in interpreting the slow movements of halo CMEs. In this paper, we study partial halo CME events with slow velocity and we discussed the slow partial halo CMEs which is due to the weak magnetic fields affect from low solar radio flux and solar wind fluctuation. The slow halo CME events were observed through CALLISTO System and compare it with database from CACTUS. As a result, we found that there are slow halo CMEs occur with velocity as low as 100- 200km/s.

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

Monitoring the Sun reveals a variety of fascinating and complex physical phenomena which are being studied mainly by analyzing its emission. Solar activity has an impact with space weather. The characteristic features of the climate of Malaysia are uniform temperature, very high humidity and copious rainfall. It has an average of temperature of 26.7 °C. Therefore, it is suitable to monitor the Sun. In following work, we will emphasize the development of solar astronomy in Malaysia. The ground based observation (i) optical and (ii) radio are the main region that we focused on. Optical observation has started earlier comparing with radio observation. In optical region it covers from 400 – 700 nm while in radio region, we focus from 45 MHz to 870 MHz. The number of observatories is increasing. A dedicated work to understand the Sun activity in radio region is a part of an initiative of the United Nations together with NASA in order to support developing countries participating in „Western Science‟ research. Realize how important for us to keep doing a research about the solar bursts, by using the new radio spectrometer, CALLISTO (Compound Low Cost Low Frequency Transportable Observatories) spectrometer. Malaysia is one of the earliest country from South-East Asia (ASEAN) that involve this research. One of the advantages to start the solar monitoring in Malaysia is because our strategic location as equator country that makes possible to observing a Sun for 12 hours daily throughout a year. We strongly believe that Malaysia as one of contributor of solar activity data through E-CALLISTO network. This is a very good start for developing a radio astronomy in Malaysia. With the implementation of 45 MHz - 870 MHz CALLISTO systems and development of solar burst monitoring network, a new wavelength regime is becoming available for solar radio astronomy. Overall, this article presents an overview of optical and radio astronomy in Malaysia. With the present level of the international collaboration, it is believed that the potential involvement of local and international scientist in solar astrophysics will increase.

Observations of type II and III solar bursts indicated that white type III bursts mane appear at any altitude, from the vary lov 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-CALLISTRO network. It was found solar burst type II exploded uite minimum with 1-2 events from 2006 − 2010. However, the data 2011 for solar burst type II increased drastically with 16 events has been recordered. The occurencess of Coronal Mass Ejections (CMEs) events are also increasing up to four times in 2011. Most of both events can be observed in the range of 150 MHz till 500 MHz. Overcall, we can say that the range of photon energy for solar burst type III is between 7.737 x 10-7 eV to 1.596 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 investigatoin of solar burst will be cocern the 2011 data seem to a significant tend 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 fare and Coronal Mass Ejections (CMEs) events. It is expected that both types will increase gradually in the beginning of 2014.

The observational of active region emission of the Sun contain an critical answer of the time-dependence of the underlying heating mechanism. In this case, we investigate an X2.2 solar flare from a new Active Region AR2087 on the southeast limb of the Sun. The solar flare peaked in the X-rays is around 11:42 UT. It was found that the snapshot of this event from the Solar Dynamics Observatory (SDO) channel with the GOES X-ray plot overlayed. The flare is very bright causes by a diffraction pattern. We explore a parameter space of heating and coronal loop properties. Based on the wavelength, it shows plasma around 6 million Kelvin. At the same time, data from the NOAA issued an R3 level radio blackout, which is centered on Earth where the Sun is currently overhead at the North Africa region. This temporary blackout is caused by the heating of the upper atmosphere from the flare. The blackout level is now at an R1 and this will soon pass. Other than the temporary radio blackout for high frequencies centered over Africa this event will not have a direct impact on us. Until now, we await more data concerning a possible Coronal Mass Ejections (CMEs) but anything would more than likely not head directly towards Earth. An active region AR2087 just let out an X1.5 flare peaking at 12:52 UT. This shows plasmas with temperatures up to about 10 Million Kelvin. This event is considered one of the massive eruption of the Sun this year.

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.

Solar space weather events like Coronal Mass Ejections and solar flares are usually accompanied by solar radio bursts, which can be used for a low-cost real-time space weather monitoring. In order to make a standard system, a CALLISTO (Compound Astronomical Low-costLow-frequency Instrument for Spectroscopy in Transportable Observatory) spectrometers, designed and built by electronics engineer Christian Monstein of the Institute for Astronomy of the Swiss Federal Institute of Technology Zurich (ETH Zurich) have been already developed all over the worldsince 2005 to monitor the solar activities such as solar flare and Coronal Mass Ejections (CMEs). Upto date, there are 25 sites that used the same system in order to monitor the Sun within 24 hours. Thisoutstanding project also is a part of the United Nations together with NASA initiated the InternationalHeliophysical Year IHY2007 to support developing countries participating in ‘Western Science’. Beginning February 2012, Malaysia has also participated in this project. The goals of this work is to highlight how does the signal processing of solar radio burst data transfer from a site of National Space Centre Banting Selangor directly to the Institute of Astrophysics Switzerland. Solar activities inthe low region, focusing from 150 MHz to 400 MHz is observed daily beginning from 00.30UT 12.30UT. Here, we highlighted how does the signal processing work in order to make sure that the operation is in the best condition. Although the solar activities have experienced rapid growth recently,high-level management of CALLISTO system has remained successfully manage the storage of data.It is also not easy to maintain the future data seems the number of sites are also growing from time totime. In this work, we highlighted the potential role of Malaysia as one of the candidate site that possible gives a good data and focusing on a few aspects such as optimization, and performance evaluation data and visualization.

In this article, we describe and compare several sources of the nonlinear of Radio Frequency Interference (RFI) based on classification methods. It is very important to characterize and understand the nature of interference in as much of the candidate spectrum as possible. Preliminary analysis has been done in 2011. As data sizes of observations grow with new and improved solar monitoring system, the need for completely automated, robust methods for RFI mitigation is highlighted. The current status of RFI noise level is being compared at two different sites (i) indoor and (ii) outdoor. The main objective is to evaluate and find the best range of low frequency in MHz for the solar monitoring purpose. Our findings are consistent with those of previous studies. There is not much different in terms of the sources of RFI. However, the level of RFI is become increase. Based on the results, it was found that the distribution of RFI sources in indoor site is in the range from -(80-105) dBm. A strong and moderate RFI can be identified in the range of -100 dBm. The dominant sources in this region are due to the fixed mobile signal with 10 points of this signal from 1-2000 MHz. If we compare with outdoor site, the distribution of RFI sources in indoor site is in the range from -(75-105) dBm. It means that the signal of noise is larger compared with indoor site. While new sources strive to remain the increasing of RFI signal levels, numerous factors interact to influence the pattern of this noise. Reporting to the authoritative body should be made to make sure the allocation of the solar monitoring frequency region was not used by other applications. This work is a current scenario of the nonlinear RFI level at our site.

An extreme 2012 October 23 solar flare event marked on the onset of the CALLISTO data, being one of the highest solar flare event that successfully detected. The formation of harmonic solar burst type II in meter region and their associated with X1.8-class solar flares has been reported. This burst has been observed at the National Space Centre, Banting, detected by the Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy and Transportable Observatory (CALLISTO) system in the range of 150-400 MHz in the low frequency band. It occurred between 3.17:45 UT to 3.19:00 UT within 1 minute 15 seconds. The Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy and Transportable Observatory CALLISTO spectrometer is a solar dedicated spectrometer system that has been installed all over the world to monitor the Sun activity in 24 hours. The growth of this burst is often accompanied by abundance enhancement of particles which may take the form of multiple independent drifting bands or other forms of fine structure. Due to the results, the drift rate of this burst is 2.116 MHz s–1, which is considered as a slow drift rate. These drifting bands are approximately having a frequency ratio 2:1. This burst is a particular interest, though of sporadic and infrequent occurrence. The splitting is due to the effect of magnetic splitting, analogous to the Zeeman Effect. This is one of the examples which the type II burst is not always associated with CMEs event. The combination of radio and x-ray region give a complete view of the solar flare eruption from e active region AR1598. Both different electromagnetic spectrum shows the exact time. Other interesting results is that this type II burst is not associated with CMEs as usual, but due to the very high solar flare event with a fundamental form at more than 100 MHz. An extension of the present work will be a detailed study of the possible triggering and the driving mechanism of solar flare explosion.

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

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.

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.

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.

A preliminary correlation study of the herring − bone type II with a type III 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. The type II solar radio burst with a split and herring bone is occurring at the same time from 36 MHz till 50 MHz. We have noted that an individual type III burst also can be observed at 13:23 UT from 45-50 MHz. During that day, a stream of solar wind from a coronal hole on the Sun has disturbing Earth's magnetosphere creating a minor geomagnetic storm, G1 on the NOAA scale of G1-G5. In this case, the solar flare is not very high, but CME is responsible to form a solar radio burst type II. Overall, based on seven days observation beginning from 25th March 2013, the solar activity is considered as very low. The highest solar flare can be observed within 7 days is only a class of B8 flare. There was no CMEs event that directed to the Earth is detected. The geomagnetic field activities are also at minimum level. Although the solar flare event is at a lower stage, it is still possible to form the solar radio burst type II which is associated with CME event. From the selected event, although theoretically solar radio burst type II is associated with CMEs, there is no compelling solar radio burst type II without a flare. The only difference is the dynamic structure and the intensity and speed of both phenomena (solar flares and CMEs) which depend on the active region. Nevertheless, understanding how energy is released in solar flares is one of the central questions in astrophysics. This solar radio burst type II formation is the first event that successfully detected by e-CALLISTO network in 2013.