scholarly journals Determining a Complex Solar Radio Burst Type II on 2nd November 2014 Driven by a Hydra Solar Flare as a Blast Waves

2015 ◽  
Vol 47 ◽  
pp. 87-93
Author(s):  
Zety Sharizat Hamidi ◽  
M.B. Ibrahim ◽  
N.N.M. Shariff ◽  
C. Monstein
Keyword(s):  
Radio Burst ◽  
Solar Radio ◽  
Low Cost ◽  
Low Frequency ◽  
Leading Edge ◽  
Blast Waves ◽  
Solar Radio Burst ◽  
The Sun ◽  
X Rays ◽  
Type Ii

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.

scholarly journals Investigation of Drift Rate of Solar Radio Burst Type II due to Coronal Mass Ejections Phenomenon

2015 ◽  
Vol 48 ◽  
pp. 146-154 ◽  
Author(s):  
N.H. Zainol ◽  
Zety Sharizat Hamidi ◽  
N.N.M. Shariff ◽  
S. Arifin ◽  
C. Monstein
Keyword(s):  
Radio Burst ◽  
Coronal Mass Ejections ◽  
Solar Radio ◽  
Drift Rate ◽  
Plasma Frequency ◽  
Low Cost ◽  
Solar Radio Burst ◽  
Type Ii ◽  
Langmuir Waves ◽  
Low Drift

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.

scholarly journals Determination of Flux Density of the Solar Radio Burst Event by Using Log Periodic Dipole Antenna (LPDA)

2014 ◽  
Vol 26 ◽  
pp. 21-29 ◽  
Author(s):  
Zety Sharizat Hamidi ◽  
N.N.M. Shariff
Keyword(s):  
Flux Density ◽  
Radio Burst ◽  
Solar Radio ◽  
Spectral Power ◽  
Low Cost ◽  
Low Frequency ◽  
Dipole Antenna ◽  
Solar Radio Burst ◽  
Isotropic Source ◽  
Space Agency

In this article, an evaluation of the flux density of the solar radio burst is presented. A rod aluminium’s type as a conductor with nineteenth (19) elements of different sizes is being prepared to construct a log periodic dipole antenna (LPDA) from 45-870 MHz. The performance was carried out at the National Space Agency (PAN), Sg. Lang, Banting Selangor by connecting to the Compound Low Cost Low Frequency Spectroscopy Transportable Observatory (CALLISTO) spectrometer. The input impedance, R0 = 50 ohm is chosen for this LPDA antenna. From the analysis, the gain of the antenna is 9.3 dB. This antenna potentially captures a signal that covers about 0.08 m2 area of the Sun.The temperature of the burst that detected at the feedpoint of the antenna is 32 K. However, the signal becomes decrease to 28.75 K while by CALLISTO spectrometer as a receiver. It was also found that the isotropic source spectral power is 1576 W/Hz. Since the burst level above the background sky is 0.41 dB , the flux density of the burst is 5.5 x 10-21 W/m2/Hz. Based on the results, we conclude that this antenna is suitable for to observe the Sun activities at low frequency region.

scholarly journals The Tendencies and Timeline of the Solar Burst Type II Fragmented

2014 ◽  
Vol 31 ◽  
pp. 84-102 ◽  
Author(s):  
Zety Sharizat Hamidi ◽  
N.N.M. Shariff ◽  
C. Monstein
Keyword(s):  
Active Region ◽  
Solar Flare ◽  
Radio Burst ◽  
Solar Radio ◽  
Active Regions ◽  
Solar Radio Burst ◽  
Beta Radiation ◽  
X Rays ◽  
Type Ii ◽  
Harmonic Structure

We report the timeline of the solar radio burst Type II that formed but fragmented at certain point based on the eruption of the solar flare on 13th November 2012 at 2:04:20 UT. The active region AR 1613 is one of the most active region in 2012. It is well known that the magnetic energy in the solar corona is explosively released before converted into the thermal and kinetic energy in solar flares. In this work, the Compound Astronomical Low-frequency, Low-cost Instrument for Spectroscopy Transportable Observatories (CALLIISTO) system is used in obtaining a dynamic spectrum of solar radio burst data. There are eight active regions and this is the indicator that the Sun is currently active. Most the active regions radiate a Beta radiation. The active regions 1610, 1611 and 1614 are currently the largest sunspots on the visible solar disk. There is an increasing chance for an isolated M-Class solar flare event. It is also expected that there will be a chance of an M flare, especially from AR 1614 and 1610. Although these two observations (radio and X-rays) seem to be dominant on the observational analysis, we could not directly confirmed that this is the only possibility, and we need to consider other processes to explain in detailed the injection, energy loss and the mechanism of the acceleration of the particles. In conclusion, the percentage of energy of solar flare becomes more dominant rather than the acceleration of particles through the Coronal Mass Ejections (CMEs) and that will be the main reason why does the harmonic structure of type II burst is not formed. This event is one fine example of tendencies solar radio burst type III, which makes the harmonic structure of solar radio burst type II fragmented.

scholarly journals An Analysis of a Single Solar Radio Burst Type III and Type II Coronal Mass Ejections Associated to Solar Flare Event

2015 ◽  
Vol 51 ◽  
pp. 17-25
Author(s):  
M. Omar Ali ◽  
Zety Sharizat Hamidi ◽  
N.N.M. Shariff ◽  
C. Monstein
Keyword(s):  
Active Region ◽  
Solar Flare ◽  
Radio Burst ◽  
Solar Radio ◽  
Solar Radio Burst ◽  
Small Scale ◽  
The Sun ◽  
Type Ii ◽  
Type Iii ◽  
Short Period

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

scholarly journals Scenario of Solar Radio Burst Type III during Solar Eclipse on 14th November 2012

2014 ◽  
Vol 32 ◽  
pp. 135-143
Author(s):  
Zety Sharizat Hamidi ◽  
N.N.M. Shariff ◽  
C. Monstein
Keyword(s):  
Local Time ◽  
Solar Eclipse ◽  
Radio Burst ◽  
Solar Radio ◽  
Low Cost ◽  
Solar Wind Speed ◽  
Low Frequency ◽  
Solar Radio Burst ◽  
Type Iii ◽  
National Space

A compact solar flare was observed during a total solar eclipse event on 13-14 November 2012. This phenomenon is beginning in local time on November 14 west of the date line over northern Australia, and ended in local time on November 13 east of the date line near the west coast of South America. During the eclipse, the highest magnitude was 1.0500, occurring only 12 hours before perigee, with the maximum eclipse totality lasting just over four minutes. Considering the observational facts, the solar radio burst type III can be detected from the National Space Centre Malaysia by the Compound Low Cost Low Frequency Transportable Observatory (CALLISTO) system from 00:00 UT – 1:30 UT. The group and individual solar burst type III can be detected in the region of 150-400 MHz. However, the eclipse cannot be observed from our site. From the observation, it was found that the eruption in the active region is becoming more active with a tens of groups solar radio burst type III can be observed. It continuing bursting within the first one hour. The sunspot number exceeds to 108 and solar wind speed 454.9 km/sec. Still the Sun remains active and we need to consider other processes to explain in detailed the injection, energy loss and the mechanism of the acceleration of the particles

scholarly journals Evidence for the Transfer of Corpuscles to Distant Parts of the Sun Following a Solar Radio Burst

1961 ◽  
Vol 14 (4) ◽  
pp. 540 ◽  
Author(s):  
RF Mullaly
Keyword(s):  
Radio Burst ◽  
Solar Radio ◽  
Brightness Distribution ◽  
Solar Radio Burst ◽  
The Sun ◽  
Time Intervals ◽  
The Past ◽  
Grating Interferometer ◽  
Half Power ◽  
East West

The brightness distribution of 21-cm radiation over the Sun's surface has been studied for the past four years with the Christiansen crossed-grating interferometer (Christiansen et al. 1961) at Fleurs near Sydney. The observations described here were made using one arm of this cross as a simple grating interferometer, providing a transit instrument with a fan beam of about 2' of arc resolution to half-power points in the east-west direction and very low resolution north-south. The Sun was scanned repeatedly from east to west at time intervals of approximately 4 min.

The 158 MHz Solar Interferometer at Culgoora

1967 ◽  
Vol 1 (2) ◽  
pp. 59-61 ◽  
Author(s):  
R. T. Stewart
Keyword(s):  
Active Region ◽  
Radio Burst ◽  
Solar Radio ◽  
Second Harmonic ◽  
Solar Observatory ◽  
Solar Radio Burst ◽  
The Sun ◽  
Harmonic Frequency ◽  
The North ◽  
East West

The function of the 158 MHz interferometer operating at the CSIRO Solar Observatory, Culgoora, N.S.W., is the measurement of solar radio burst positions at a frequency close to the second harmonic frequency of the radioheliograph. The interferometer is designed to measure the north-south and east-west position co-ordinates of an isolated active region on the Sun with an accuracy of ~1′ arc, at rates up to 16 s−1.

scholarly journals Type II Solar Radio Burst with a Split and Herring − Bones during a Minimum Solar Activity

2014 ◽  
Vol 32 ◽  
pp. 104-111
Author(s):  
Zety Sharizat Hamidi ◽  
N.N.M. Shariff ◽  
C. Monstein
Keyword(s):  
Solar Activity ◽  
Solar Flare ◽  
Radio Burst ◽  
Solar Flares ◽  
Solar Radio ◽  
Correlation Study ◽  
Solar Radio Burst ◽  
Type Ii ◽  
Type Iii ◽  
Lower Stage

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.

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