The Experts below are selected from a list of 360 Experts worldwide ranked by ideXlab platform
C Monstein - One of the best experts on this subject based on the ideXlab platform.
-
two stage evolution of an extended c class eruptive flaring activity from sigmoid active region noaa 12734 sdo and udaipur Callisto observations
Solar Physics, 2021Co-Authors: Bhuwan Joshi, Kushagra Upadhyay, Prabir K Mitra, R Bhattacharyya, D Oberoi, Sasikumar K Raja, C MonsteinAbstract:In this article, we present a multi-wavelength investigation of a C-class flaring activity that occurred in the active region NOAA 12734 on 8 March 2019. The investigation utilizes data from the Atmospheric Imaging Assembly (AIA) and the Helioseismic Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO) and the Udaipur-Callisto solar radio spectrograph of the Physical Research Laboratory. This low intensity C1.3 event is characterized by typical features of a long-duration event (LDE), viz. extended flare arcade, large-scale two-ribbon structures and twin coronal dimmings. The eruptive event occurred in a coronal sigmoid and displayed two distinct stages of energy release, manifested in terms of temporal and spatial evolution. The formation of twin-dimming regions are consistent with the eruption of a large flux rope with footpoints lying in the western and eastern edges of the coronal sigmoid. The metric radio observations obtained from Udaipur-Callisto reveals a broad-band ( $\approx50\,\text{--}\,180~\text{MHz}$ ), stationary plasma emission for $\approx7~\text{min}$ during the second stage of the flaring activity that resemble a type IV radio burst. A type III decametre-hectometre radio bursts with starting frequency of $\approx2.5~\text{MHz}$ precedes the stationary type IV burst observed by Udaipur-Callisto by $\approx5~\text{min}$ . The synthesis of multi-wavelength observations and non-linear force-free field (NLFFF) coronal modeling together with magnetic decay index analysis suggest that the sigmoid flux rope underwent a zipping-like uprooting from its western to eastern footpoints in response to the overlying asymmetric magnetic field confinement. The asymmetrical eruption of the flux rope also accounts for the observed large-scale structures viz. apparent eastward shift of flare ribbons and post-flare loops along the polarity inversion line (PIL), and provides evidence for lateral progression of magnetic reconnection site as the eruption proceeds.
-
two stage evolution of an extended c class eruptive flaring activity from sigmoid active region noaa 12734 sdo and udaipur Callisto observations
arXiv: Solar and Stellar Astrophysics, 2021Co-Authors: Bhuwan Joshi, Kushagra Upadhyay, Prabir K Mitra, R Bhattacharyya, D Oberoi, Sasikumar K Raja, C MonsteinAbstract:We present a multi-wavelength investigation of a C-class flaring activity that occurred in the active region NOAA 12734 on 8 March 2019. The investigation utilises data from AIA and HMI on board the SDO and the Udaipur-Callisto solar radio spectrograph of the Physical Research Laboratory. This low intensity C1.3 event is characterised by typical features of a long duration event (LDE), viz. extended flare arcade, large-scale two-ribbon structures and twin coronal dimmings. The eruptive event occurred in a coronal sigmoid and displayed two distinct stages of energy release, manifested in terms of temporal and spatial evolution. The formation of twin dimming regions are consistent with the eruption of a large flux rope with footpoints lying in the western and eastern edges of the coronal sigmoid. The metric radio observations obtained from Udaipur-Callisto reveals a broad-band ($\approx$50-180 MHz), stationary plasma emission for $\approx$7 min during the second stage of the flaring activity that resemble a type IV radio burst. A type III decametre-hectometre radio bursts with starting frequency of $\approx$2.5 MHz precedes the stationary type IV burst observed by Udaipur-Callisto by $\approx$5 min. The synthesis of multi-wavelength observations and Non-Linear Force Free Field (NLFFF) coronal modelling together with magnetic decay index analysis suggests that the sigmoid flux rope underwent a zipping-like uprooting from its western to eastern footpoints in response to the overlying asymmetric magnetic field confinement. The asymmetrical eruption of the flux rope also accounts for the observed large-scale structures viz. apparent eastward shift of flare ribbons and post flare loops along the polarity inversion line (PIL), and provides an evidence for lateral progression of magnetic reconnection site as the eruption proceeds.
-
solar radio observation using Callisto at the uso prl udaipur
IEEE MTT-S International Microwave and RF Conference, 2019Co-Authors: Kushagra Upadhyay, Bhuwan Joshi, Prabir K Mitra, R Bhattacharyya, D Oberoi, C MonsteinAbstract:This paper presents a detailed description of various subsystems of Callisto solar radio spectrograph installed at the USO/PRL. In the front-end system, a log periodic dipole antenna (LPDA) is designed for the frequency range of 40-900 MHz. In this paper LPDA design, its modifications, and simulation results are presented. We also present some initial observations taken by Callisto at Udaipur.
-
Callisto spectrometer at iiser pune
arXiv: Instrumentation and Methods for Astrophysics, 2018Co-Authors: Sasikumar K Raja, Prasad Subramanian, S Ananthakrishnan, C MonsteinAbstract:A Callisto spectrometer to monitor solar radio transient emissions from $\approx 0.8-1.6~R_{\odot}$ (above photosphere) is installed at IISER, Pune, India (longitude $73^{\circ} 55'$ E and latitude $18^{\circ}31'$ N). In this paper, we illustrate the instrumental details (log-periodic dipole antenna and the receiver system) along with the recorded solar radio bursts and radio frequency interferences produced by the thunderstorms in the frequency range 45-870 MHz. We also developed the image processing pipelines using `sunpy' and in-house developed python library called `pyCallisto'.
-
a year of operation of melibea e Callisto solar radio telescope
Journal of Physics: Conference Series, 2015Co-Authors: A Russu, R Gomezherrero, M Prieto, C Monstein, H Ivanov, J Rodriguezpacheco, J J BlancoAbstract:The e-Callisto (Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy and Transportable Observatory) is a worldwide radio-spectrograph network with 24 hours a day solar radio burst monitoring. The e-Callisto network is led by the Swiss Federal Institute of Technology Zurich (ETHZ Zurich), which work up collaborations with local host institutions. In 2013 the University of Alcala joined the e-Callisto network with the installation of two Solar Radio Telescopes (SRT): the EA4RKU-SRT that was located at the University of Alcala from January 2013 till June 2013 and the Melibea-SRT that is located at Peralejos de las Truchas (Guadalajara) in operation from June 2013. The Spanish e-Callisto SRTs provide routine data to the network. We present examples of type III and type II radio-bursts observed by Melibea during its first year of operation and study their relation with soft X-ray flares observed by GOES and Coronal Mass Ejections (CMEs) and Solar Energetic Particle (SEP) events observed by space-borne instrumentation.
Paul M Schenk - One of the best experts on this subject based on the ideXlab platform.
-
differential cratering of synchronously rotating satellites by ecliptic comets
Icarus, 2001Co-Authors: Kevin Zahnle, Paul M Schenk, Steven Sobieszczyk, Luke Dones, Harold F LevisonAbstract:Abstract We use Monte Carlo methods to simulate impacts of ecliptic comets on the synchronously rotating satellites of giant planets. We reconfirm the long-standing prediction that the cratering rate should be much higher on the leading hemispheres than on the trailing hemisphere; indeed we find that previously published analytical formulations modestly underestimate the degree of apex–antapex asymmetry to be expected. We then compare our results to new mapping of impact craters on Ganymede, Callisto, and Triton. Ganymede reveals a pronounced apex–antapex asymmetry that is nonetheless much less than predicted. All of Triton's confirmed impact craters are clustered toward the apex of motion, far exceeding the predicted asymmetry. No asymmetry is observed on Callisto. In each case at least one of our basic assumptions must be wrong. Likely candidates include the following: (i) the surfaces of all but the most sparsely cratered satellites are saturated or nearly saturated with impact craters; (ii) these satellites have rotated nonsynchronously over geological time; (iii) most of the craters are made not by heliocentric (Sun-orbiting) comets and asteroids but rather by planetocentric (planet-orbiting) debris of indeterminate origin; or (iv) pathological endogenic resurfacing has created illusions of structure. Callisto's surface is readily classified as nearly saturated. Ganymede's bright terrains, although less heavily cratered than those of Callisto, can also be explained by crater densities approaching saturation on a world where endogenic processes were active. The leading alternative is nonsynchronous rotation, an explanation supported by the distribution of catenae (crater chains produced by impact of tidally disrupted comets). Triton's craters can be explained by planetocentric debris or by capricious resurfacing, but both hypotheses are inherently improbable.
-
estimates of comet fragment masses from impact crater chains on Callisto and ganymede
Geophysical Research Letters, 1995Co-Authors: William B Mckinnon, Paul M SchenkAbstract:Chains of impact craters, or catenae, have been identified in Voyager images of Callisto and Ganymede. Although these resemble in some respects secondary crater chains, the source craters and basins for the catenae cannot be identified. The best explanation, proposed by Melosh and Schenk, is a phenomenon similar to that displayed by former comet P/Shoemaker-Levy 9: tidal (or other) breakup close to Jupiter followed by gradual orbital separation of the fragments and collision with a Galilean satellite on the outbound leg of the trajectory. Because the trajectories must pass close to Jupiter, this constrains the impact geometry (velocity and impact angle) of the individual fragments. For the dominant classes of impactors, short-period Jupiter-family comets and asteroids, velocities at Callisto and Ganymede are dominated by jovian gravity and a satellite's orbital motion, and are insensitive to the pre-fragmentation heliocentric velocity; velocities are insensitive to satellite gravity for all impactor classes. Complex crater shapes on Callisto and Ganymede are determined from Voyager images and Schmidt-Holsapple scaling is used to back out individual fragment masses. We find that comet fragment radii are generally less than ∼500 m (for ice densities), but can be larger. These estimates can be compared with those for the Shoemaker-Levy 9 impactors.
-
split comets and the origin of crater chains on ganymede and Callisto
Nature, 1993Co-Authors: H J Melosh, Paul M SchenkAbstract:WHEN the Voyager 1 spacecraft flew through the jovian system in January 1979, it returned images of several prominent chains of impact craters on the surface of the moon Callisto (Fig. 1). These impressively straight chains, or catenae, are composed of between 4 and 25 craters, and are up to 620 km long. They were initially thought to be secondary craters produced by debris from a larger primary impact1, but detailed searches for source craters have been largely unsuccessful: a satisfactory explanation for the crater chains has yet to be found. Inspired by the recent observations of comet Shoemaker–Levy 9, which split into a line of about 20 fragments as it swept past Jupiter2, we suggest that the impact of previous split comets might be responsible for at least some of the catenae on Callisto. In support of this hypothesis, we find that nearly all of Callisto's crater chains are on the Jupiter-facing hemisphere, as are an additional three catenae that we have found on Ganymede. We present a simple model of tidal breakup which both reproduces the range of observed chain lengths and indicates that the parent comets responsible for the Callisto catenae were typically no more than about 10 km in diameter.
-
central pit and dome craters exposing the interiors of ganymede and Callisto
Journal of Geophysical Research, 1993Co-Authors: Paul M SchenkAbstract:Central pit craters on the large icy satellites Ganymede and Callisto are an unusual crater class perhaps related to the unusual properties of water ice. The detailed morphology and dimensions of pit crater features differ from those of smaller, normal, complex craters on these two satellites. Pit crater depths appear to be constant regardless of diameter. Rim collapse is also restricted relative to that in lunar craters or smaller Ganymede craters. The floors of pits in craters larger than ∼60 km are occupied by smooth bright domes. Pit-to-crater and dome-to-crater diameter ratios increase linearly with crater diameter, and are indistinguishable on Ganymede and Callisto and with terrain type or surface longitude. The floors and central structures of young, bright-rayed pit craters such as Osiris are covered by a thin uniformly bright impact melt or frost deposit. Thus, domes and pits form rapidly, on the time scale of the impact itself, rather than by long-term, postimpact intrusion or extrusion. The bright domes in pit craters are most simply explained as the uplift and exposure of relatively ice-rich material from depths of ∼3.5 to 5 km during impact. This process is almost directly analogous to the uplift and exposure of anamolous deep-seated material observed in terrestrial and lunar craters. The unusual pit morphology on icy satellites may be the result of impact into crust that is mechanically much weaker at shallow depth than on rocky bodies such as the Moon. Because crater morphology is strongly dependent on ice-rock composition, the similarity of pit and dome dimensions on Ganymede and Callisto indicates that the structure and rheology of the crusts of these bodies (down to depths of ∼10 km) are very similar and have been for several b.y. Pit crater morphology indicates that the crusts of both satellites are probably ice-rich and differentiated.
-
ganymede and Callisto complex crater formation and planetary crusts
Journal of Geophysical Research, 1991Co-Authors: Paul M SchenkAbstract:Results are presented on measurements of crater depths and other morphological parameters (such as central peak and terrace frequency) of fresh craters on Ganymede and Callisto, two geophysically very similar but geologically divergent large icy satellites of Jupiter. These data were used to investigate the crater mechanics on icy satellites and the intersatellite crater scaling and crustal properties. The morphological transition diameters of and complex crater depths on Ganymede and Callisto were found to be similar, indicating that the crusts of both satellites are dominated by water ice with only a minor rocky component.
Christian Monstein - One of the best experts on this subject based on the ideXlab platform.
-
Effective Data Collection and Analysis of Solar Radio Burst Type II Event Using Automated Callisto Network System
2016 International Conference on Industrial Engineering Management Science and Application (ICIMSA), 2016Co-Authors: N. H. Zainol, N. N. M. Shariff, Christian Monstein, S. N. U. Sabri, Z. S. Hamidi, Nurul Hazwani Husien, M. S. FaidAbstract:The Callisto network systems are widely used for continuous data collection of solar activities every day through the internet connection and stored in the central database in the computer. The system installation began in 2002 in Zurich, and its network has spread all around the globe ever since, benefiting researchers and individuals worldwide. This research paper presents one of selected event using a radio spectrometer the Callisto system from Ireland, which demonstrates a solar radio burst event detected during the 13:23 (UT) to 13:26 (UT) on 30th March 2013 in Ireland. Besides, data from Glasgow and Humain were compared to be analyzed. Those installed Callisto in each country is called as extendable the Callisto system (e-Callisto). The analysis being carried out based on spectrogram data of the Callisto system obtained from these three countries. Results showed that all three sites observed the same Solar Radio Burst Type II at the same time but different in locations. The e- Callisto system has proven to be a new tool for monitoring solar activity and for space weather research.
-
the dependence of log periodic dipole antenna lpda and e Callisto software to determine the type of solar radio burst i v
International Conference on Industrial Engineering Management Science and Application, 2016Co-Authors: S. N. U. Sabri, N. H. Zainol, N. N. M. Shariff, M. O. Ali, Z. S. Hamidi, M. S. Faid, Nurulhazwani Hussien, Christian MonsteinAbstract:Solar radio burst originated at the layer of the atmosphere where the Geo-effective disturbance occurred which energy will be released in solar flares and Coronal Mass Ejections (CMEs) will be launched. Solar Radio Burst can be divided into 5 types and determined by using the Log Periodic Dipole Antenna (LPDA) and e-Callisto system. The LPDA was set up in a 45-870 MHz range in frequency and has maximum boom length 5.45m. Besides that, it has minimum scale factor, τ=0.76 and maximum at τ=0.98. We put some effort to construct suitable with designs, high specification and practical enough with the size of boom length as the conclusion the scale factor that suitable with this design is 0.8118 as a directivity of an antenna. LPDA has 19 elements which using two (2) aluminium rod with 7.01dB gain. The antenna has a function to receive the signals then connected to the low noise amplifier and e-Callisto spectrometer completes it as a system. A Callisto (Compound Astronomical Low-Cost- Low-Frequency Instrument for Spectroscopy Transportable Observatory) spectrometer was used to figure out the dynamic of solar corona which in metric and decimetric wavelength radio observation and the main objective of this study was to study how the solar radio burst can be detected by using LPDA (Malaysia) and e-Callisto (ETH Zurich, Switzerland) which were set up in a different location.In this paper, the potential of Malaysia be one of the candidates to contribute a good data will be highlighted and we will focus more on performance evaluation and visualization data.
-
signal detection of the solar radio burst type iii based on the Callisto system project management
International Conference on Industrial Engineering Management Science and Application, 2016Co-Authors: Z. S. Hamidi, N. H. Zainol, N. N. M. Shariff, M. O. Ali, S. N. U. Sabri, Nurul Hazwani Husien, M. S. Faid, Christian MonsteinAbstract:The E-Callisto (Compact Astronomical Low Cost Frequency Instrument for Spectroscopy and Transportable Observatory) network is a worldwide system in order to observe the Sun's activity in the radio region. At present, more than 80 instruments have been installed at more than 43 locations, with users from more than 113 countries in the e- Callisto network. At present, more than 80 instruments have been installed at more than 43 locations, with users from more than 113 countries in the e-Callisto network. In this paper, we make use of the e-Callisto data that shows a sign of solar activity. On 9th May, the Solar Radio Burst Type III (SRBT III) happens for two times. The first detection of SRBT III occurred less than 1 minute within 05:31UT and 05:32 UT as illustrated in Figure 3. The second SRBT III seems to be occurred within 05:41 UT to 05:42 UT for approximately 1 minute. The Coronal mass ejection which was ejected from the active region AR2339, was detected at 05:42UT has the 'beta-gamma' magnetic field that harbors energy for strong solar flares. From the results, the point we wish to make here is that at least some of these type III bursts with low starting frequencies are consistent with front-side flares, which indicates to us that the low starting frequencies observed for many of these bursts are intrinsic to the type III emissions and do not result from occulting of the high-frequency emissions from any plasma structures.
-
Analysis of radio astronomy bands using Callisto spectrometer at Malaysia-UKM station
Experimental Astronomy, 2016Co-Authors: Azam Zavvari, Mohammad Tariqul Islam, Radial Anwar, Zamri Zainal Abidin, Mhd Fairos Asillam, Christian MonsteinAbstract:The e-Callisto system is a worldwide network that aims to observe solar radio emission for astronomical science. Callisto instruments have been deployed worldwide in various locations that together can provide continuous observation of the solar radio spectrum for 24 h per day year-round. Malaysia-UKM is a strategic equatorial location and can observe the Sun 12 h per day. This paper gives an overview of the spectrum allocation for radio astronomy, which falls in the specified operating frequency band of the Callisto spectrometer. The radio astronomy bands are analyzed at the Malaysia-UKM station according to the International Telecommunication Union recommendations. Some observational results are also presented in this paper.
-
an automated system for signal detection of solar radio burst type ii due to coronal mass ejections phenomena
International Conference on Information Science and Applications, 2016Co-Authors: N. H. Zainol, N. N. M. Shariff, Z. S. Hamidi, Christian MonsteinAbstract:This paper presents the signal detection by automated system for an event related to solar phenomena. Here, a system of Compound Astronomical Low-Cost Low-Frequency Instrument for Spectroscopy and Transportable Observatory (Callisto) for detecting, interpreting and observing automatically radio signal obtained from solar activity is been used. The system observes and collects radio signal for every day via internet and stored in a central data and it is a worldwide network of radio spectrometer where has been installed in various locations all over the world. An event detects by the Callisto on 2nd November 2014 in Blein, Switzerland shows the present of solar radio burst type II due to Coronal Mass Ejections (CMEs). The Log Periodic Dipole Antenna (LPDA) was connected to the Callisto system software to collect the signal of solar activity. LPDA monitors solar radio flux in due to solar radio burst type II phenomena. It standardized the frequency range for Callisto networking to operate well. Callisto system has already proven to be a precious new tool for monitoring solar activity and for space weather research.
Z. S. Hamidi - One of the best experts on this subject based on the ideXlab platform.
-
Effective Data Collection and Analysis of Solar Radio Burst Type II Event Using Automated Callisto Network System
2016 International Conference on Industrial Engineering Management Science and Application (ICIMSA), 2016Co-Authors: N. H. Zainol, N. N. M. Shariff, Christian Monstein, S. N. U. Sabri, Z. S. Hamidi, Nurul Hazwani Husien, M. S. FaidAbstract:The Callisto network systems are widely used for continuous data collection of solar activities every day through the internet connection and stored in the central database in the computer. The system installation began in 2002 in Zurich, and its network has spread all around the globe ever since, benefiting researchers and individuals worldwide. This research paper presents one of selected event using a radio spectrometer the Callisto system from Ireland, which demonstrates a solar radio burst event detected during the 13:23 (UT) to 13:26 (UT) on 30th March 2013 in Ireland. Besides, data from Glasgow and Humain were compared to be analyzed. Those installed Callisto in each country is called as extendable the Callisto system (e-Callisto). The analysis being carried out based on spectrogram data of the Callisto system obtained from these three countries. Results showed that all three sites observed the same Solar Radio Burst Type II at the same time but different in locations. The e- Callisto system has proven to be a new tool for monitoring solar activity and for space weather research.
-
the dependence of log periodic dipole antenna lpda and e Callisto software to determine the type of solar radio burst i v
International Conference on Industrial Engineering Management Science and Application, 2016Co-Authors: S. N. U. Sabri, N. H. Zainol, N. N. M. Shariff, M. O. Ali, Z. S. Hamidi, M. S. Faid, Nurulhazwani Hussien, Christian MonsteinAbstract:Solar radio burst originated at the layer of the atmosphere where the Geo-effective disturbance occurred which energy will be released in solar flares and Coronal Mass Ejections (CMEs) will be launched. Solar Radio Burst can be divided into 5 types and determined by using the Log Periodic Dipole Antenna (LPDA) and e-Callisto system. The LPDA was set up in a 45-870 MHz range in frequency and has maximum boom length 5.45m. Besides that, it has minimum scale factor, τ=0.76 and maximum at τ=0.98. We put some effort to construct suitable with designs, high specification and practical enough with the size of boom length as the conclusion the scale factor that suitable with this design is 0.8118 as a directivity of an antenna. LPDA has 19 elements which using two (2) aluminium rod with 7.01dB gain. The antenna has a function to receive the signals then connected to the low noise amplifier and e-Callisto spectrometer completes it as a system. A Callisto (Compound Astronomical Low-Cost- Low-Frequency Instrument for Spectroscopy Transportable Observatory) spectrometer was used to figure out the dynamic of solar corona which in metric and decimetric wavelength radio observation and the main objective of this study was to study how the solar radio burst can be detected by using LPDA (Malaysia) and e-Callisto (ETH Zurich, Switzerland) which were set up in a different location.In this paper, the potential of Malaysia be one of the candidates to contribute a good data will be highlighted and we will focus more on performance evaluation and visualization data.
-
signal detection of the solar radio burst type iii based on the Callisto system project management
International Conference on Industrial Engineering Management Science and Application, 2016Co-Authors: Z. S. Hamidi, N. H. Zainol, N. N. M. Shariff, M. O. Ali, S. N. U. Sabri, Nurul Hazwani Husien, M. S. Faid, Christian MonsteinAbstract:The E-Callisto (Compact Astronomical Low Cost Frequency Instrument for Spectroscopy and Transportable Observatory) network is a worldwide system in order to observe the Sun's activity in the radio region. At present, more than 80 instruments have been installed at more than 43 locations, with users from more than 113 countries in the e- Callisto network. At present, more than 80 instruments have been installed at more than 43 locations, with users from more than 113 countries in the e-Callisto network. In this paper, we make use of the e-Callisto data that shows a sign of solar activity. On 9th May, the Solar Radio Burst Type III (SRBT III) happens for two times. The first detection of SRBT III occurred less than 1 minute within 05:31UT and 05:32 UT as illustrated in Figure 3. The second SRBT III seems to be occurred within 05:41 UT to 05:42 UT for approximately 1 minute. The Coronal mass ejection which was ejected from the active region AR2339, was detected at 05:42UT has the 'beta-gamma' magnetic field that harbors energy for strong solar flares. From the results, the point we wish to make here is that at least some of these type III bursts with low starting frequencies are consistent with front-side flares, which indicates to us that the low starting frequencies observed for many of these bursts are intrinsic to the type III emissions and do not result from occulting of the high-frequency emissions from any plasma structures.
-
an automated system for signal detection of solar radio burst type ii due to coronal mass ejections phenomena
International Conference on Information Science and Applications, 2016Co-Authors: N. H. Zainol, N. N. M. Shariff, Z. S. Hamidi, Christian MonsteinAbstract:This paper presents the signal detection by automated system for an event related to solar phenomena. Here, a system of Compound Astronomical Low-Cost Low-Frequency Instrument for Spectroscopy and Transportable Observatory (Callisto) for detecting, interpreting and observing automatically radio signal obtained from solar activity is been used. The system observes and collects radio signal for every day via internet and stored in a central data and it is a worldwide network of radio spectrometer where has been installed in various locations all over the world. An event detects by the Callisto on 2nd November 2014 in Blein, Switzerland shows the present of solar radio burst type II due to Coronal Mass Ejections (CMEs). The Log Periodic Dipole Antenna (LPDA) was connected to the Callisto system software to collect the signal of solar activity. LPDA monitors solar radio flux in due to solar radio burst type II phenomena. It standardized the frequency range for Callisto networking to operate well. Callisto system has already proven to be a precious new tool for monitoring solar activity and for space weather research.
-
the international cooperation of solar radio burst project using e Callisto system network
International Conference on Information Science and Applications, 2016Co-Authors: Z. S. Hamidi, N. N. M. Shariff, Christian Monstein, Abdel Baset Mohamed El Nabwi Abdel Hamid Ibrahim, M I M YusofAbstract:The Callisto (Compound Low Cost-Low Frequency for Transportable Observatories) system is one of the most outstanding project under ISWI with there are more than 80 instruments in more than 43 locations with users from more than 116 countries. In this paper, we will highlight the concept of Callisto, distributing the observational sites all over the world and how this system is become as one of the efficient solutions to achieve the 24 hours radio observation. This innovative project is to monitor the Sun at the radio frequency range, which is very important to understand the solar flare and Coronal Mass Ejections correspond to different aspects of the same magnetic energy release. Malaysia also occupies an important role in the Callisto due to the 12 hours monitoring of solar activities throughout the year. Since 2007, the e-Callisto system has already proven to be a valuable new tool for monitoring solar activity and for space weather research.
N. N. M. Shariff - One of the best experts on this subject based on the ideXlab platform.
-
Effective Data Collection and Analysis of Solar Radio Burst Type II Event Using Automated Callisto Network System
2016 International Conference on Industrial Engineering Management Science and Application (ICIMSA), 2016Co-Authors: N. H. Zainol, N. N. M. Shariff, Christian Monstein, S. N. U. Sabri, Z. S. Hamidi, Nurul Hazwani Husien, M. S. FaidAbstract:The Callisto network systems are widely used for continuous data collection of solar activities every day through the internet connection and stored in the central database in the computer. The system installation began in 2002 in Zurich, and its network has spread all around the globe ever since, benefiting researchers and individuals worldwide. This research paper presents one of selected event using a radio spectrometer the Callisto system from Ireland, which demonstrates a solar radio burst event detected during the 13:23 (UT) to 13:26 (UT) on 30th March 2013 in Ireland. Besides, data from Glasgow and Humain were compared to be analyzed. Those installed Callisto in each country is called as extendable the Callisto system (e-Callisto). The analysis being carried out based on spectrogram data of the Callisto system obtained from these three countries. Results showed that all three sites observed the same Solar Radio Burst Type II at the same time but different in locations. The e- Callisto system has proven to be a new tool for monitoring solar activity and for space weather research.
-
the dependence of log periodic dipole antenna lpda and e Callisto software to determine the type of solar radio burst i v
International Conference on Industrial Engineering Management Science and Application, 2016Co-Authors: S. N. U. Sabri, N. H. Zainol, N. N. M. Shariff, M. O. Ali, Z. S. Hamidi, M. S. Faid, Nurulhazwani Hussien, Christian MonsteinAbstract:Solar radio burst originated at the layer of the atmosphere where the Geo-effective disturbance occurred which energy will be released in solar flares and Coronal Mass Ejections (CMEs) will be launched. Solar Radio Burst can be divided into 5 types and determined by using the Log Periodic Dipole Antenna (LPDA) and e-Callisto system. The LPDA was set up in a 45-870 MHz range in frequency and has maximum boom length 5.45m. Besides that, it has minimum scale factor, τ=0.76 and maximum at τ=0.98. We put some effort to construct suitable with designs, high specification and practical enough with the size of boom length as the conclusion the scale factor that suitable with this design is 0.8118 as a directivity of an antenna. LPDA has 19 elements which using two (2) aluminium rod with 7.01dB gain. The antenna has a function to receive the signals then connected to the low noise amplifier and e-Callisto spectrometer completes it as a system. A Callisto (Compound Astronomical Low-Cost- Low-Frequency Instrument for Spectroscopy Transportable Observatory) spectrometer was used to figure out the dynamic of solar corona which in metric and decimetric wavelength radio observation and the main objective of this study was to study how the solar radio burst can be detected by using LPDA (Malaysia) and e-Callisto (ETH Zurich, Switzerland) which were set up in a different location.In this paper, the potential of Malaysia be one of the candidates to contribute a good data will be highlighted and we will focus more on performance evaluation and visualization data.
-
signal detection of the solar radio burst type iii based on the Callisto system project management
International Conference on Industrial Engineering Management Science and Application, 2016Co-Authors: Z. S. Hamidi, N. H. Zainol, N. N. M. Shariff, M. O. Ali, S. N. U. Sabri, Nurul Hazwani Husien, M. S. Faid, Christian MonsteinAbstract:The E-Callisto (Compact Astronomical Low Cost Frequency Instrument for Spectroscopy and Transportable Observatory) network is a worldwide system in order to observe the Sun's activity in the radio region. At present, more than 80 instruments have been installed at more than 43 locations, with users from more than 113 countries in the e- Callisto network. At present, more than 80 instruments have been installed at more than 43 locations, with users from more than 113 countries in the e-Callisto network. In this paper, we make use of the e-Callisto data that shows a sign of solar activity. On 9th May, the Solar Radio Burst Type III (SRBT III) happens for two times. The first detection of SRBT III occurred less than 1 minute within 05:31UT and 05:32 UT as illustrated in Figure 3. The second SRBT III seems to be occurred within 05:41 UT to 05:42 UT for approximately 1 minute. The Coronal mass ejection which was ejected from the active region AR2339, was detected at 05:42UT has the 'beta-gamma' magnetic field that harbors energy for strong solar flares. From the results, the point we wish to make here is that at least some of these type III bursts with low starting frequencies are consistent with front-side flares, which indicates to us that the low starting frequencies observed for many of these bursts are intrinsic to the type III emissions and do not result from occulting of the high-frequency emissions from any plasma structures.
-
an automated system for signal detection of solar radio burst type ii due to coronal mass ejections phenomena
International Conference on Information Science and Applications, 2016Co-Authors: N. H. Zainol, N. N. M. Shariff, Z. S. Hamidi, Christian MonsteinAbstract:This paper presents the signal detection by automated system for an event related to solar phenomena. Here, a system of Compound Astronomical Low-Cost Low-Frequency Instrument for Spectroscopy and Transportable Observatory (Callisto) for detecting, interpreting and observing automatically radio signal obtained from solar activity is been used. The system observes and collects radio signal for every day via internet and stored in a central data and it is a worldwide network of radio spectrometer where has been installed in various locations all over the world. An event detects by the Callisto on 2nd November 2014 in Blein, Switzerland shows the present of solar radio burst type II due to Coronal Mass Ejections (CMEs). The Log Periodic Dipole Antenna (LPDA) was connected to the Callisto system software to collect the signal of solar activity. LPDA monitors solar radio flux in due to solar radio burst type II phenomena. It standardized the frequency range for Callisto networking to operate well. Callisto system has already proven to be a precious new tool for monitoring solar activity and for space weather research.
-
the international cooperation of solar radio burst project using e Callisto system network
International Conference on Information Science and Applications, 2016Co-Authors: Z. S. Hamidi, N. N. M. Shariff, Christian Monstein, Abdel Baset Mohamed El Nabwi Abdel Hamid Ibrahim, M I M YusofAbstract:The Callisto (Compound Low Cost-Low Frequency for Transportable Observatories) system is one of the most outstanding project under ISWI with there are more than 80 instruments in more than 43 locations with users from more than 116 countries. In this paper, we will highlight the concept of Callisto, distributing the observational sites all over the world and how this system is become as one of the efficient solutions to achieve the 24 hours radio observation. This innovative project is to monitor the Sun at the radio frequency range, which is very important to understand the solar flare and Coronal Mass Ejections correspond to different aspects of the same magnetic energy release. Malaysia also occupies an important role in the Callisto due to the 12 hours monitoring of solar activities throughout the year. Since 2007, the e-Callisto system has already proven to be a valuable new tool for monitoring solar activity and for space weather research.
