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WSN 34 (2016) 121-134 EISSN 2392-2192

The Tendencies Group Type III Burst Form Type II Burst During Low activity

Z. S. Hamidi1,*, Fatin Nabila Mokthtar1, N. N. M. Shariff2, Marhana Omar Ali1,

Nurulhazwani Husien1, S. N. U. Sabri1, N. H. Zainol1, C. Monstein3 1School of Physics and Material Sciences, Faculty of Sciences, MARA University of Technology,

40450, Shah Alam, Selangor, Malaysia

2Academy of Contemporary Islamic Studies (ACIS), MARA University of Technology,

40450, Shah Alam, Selangor, Malaysia

3Institute of Astronomy, Wolfgang-Pauli-Strasse 27, Building HIT,

Floor J, CH-8093 Zurich, Switzerland

*E-mail address: [email protected]

ABSTRACT

Using the e-CALLISTO network radio observations on 1st June 2015, we present an analysis of

the complex type III and type II solar radio bursts during low activity. This event occurred on 1st July

2015 at 13:52 UT (complex solar burst type III) and 13:40 UT - 13:44 UT (solar burst type II). Solar

burst type detected at (i) BIR, (ii) BLENSW, (iii) Essen, (iv) Glascow (v) Osra, (vi) Rwanda. The

spectral shape consists of high flux densities at meter wavelengths. The energy going into plasma

heating during each flare was estimated by computing the time evolution of the energy content of the

thermal plasma and obtaining the peak value. This constitutes a lower limit to the thermal energy,

since it does not account for the cooling of the plasma prior to this time nor to any heating at later

times. It is also believed that the meter wavelength branch of the this type III spectrum may be

attributable to second-phase accelerated electrons to form type II burst. There are four sunspots of the

active regions (AR2355, AR2356, AR2357, and AR2358) during this event. The solar wind recorded

during the event is 342.4 km/s and the density of the proton recorded is 4.1 protons/cm3. Moreover, the

are some evidence that radio-quiet CMEs mostly came from the edges of the sun. The main goal of

this study was to determine whether is there any possibilities that the radio burst can be formed even

the Sun is at low activity and this event is one of the candidate events.

mailto:[email protected]

World Scientific News 34 (2016) 121-134

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Keywords: Sun; solar burst; type II; type III, radio region; X-ray region; Coronal Mass Ejections

(CMEs)

1. INTRODUCTION

The Sun, a typical star, dominates the solar system in size and mass. The Sun's core is

about 16 million K and has a distance of this star from our Earth is 1 AU [1] . A convection

zone, convective zone or convective region of a star is a layer which is unstable to convection.

Energy is primarily or partially transported by convection in such a region. In a radiation

zone, energy is transported by radiation and conduction [2]. The core is the innermost 10% of

the Sun's mass. It is where the energy from nuclear fusion is generated. The radiative zone is

where the energy is transported from the superhot interior to the colder outer layers by

photons while the energy in the outer 15% of the Sun's radius is transported by the bulk

motions of gas in a process called convection [3,4]. The corona is known to be very hot

because it has ions with many electrons removed from the atoms. At high enough

temperatures the atoms collide with each other with such energy to eject electrons. Usually

the magnetic field is somehow responsible for the sunspot cycle. In one 11-year cycle the

leading sunspot in a sunspot group will have a north magnetic pole while the trailing sunspot

in the group will have a south magnetic pole. The major drivers of space weather are closely

related to complicated explosion-like events on the Sun such as the solar flares and coronal

mass ejections (CME). This solar activity can be detected in terms of solar radio bursts occur

due to magnetic reconnection [5].

In this sub-section, we detail the properties of the type II and III burst. CME-driven

shocks are connected with the production of type II radio bursts (e.g., Nelson & Melrose

1985), whereas type III radio bursts are associated with solar flares (Wild 1950). Both type II

and III solar radio bursts are assumed to be generated by fast electrons, the emission being at

the plasma frequency and/or its second harmonic [6,7]. Type III bursts are commonly

observed whenever there is a bright active region on the visible side of the Sun and can be

considered as an indicator of increased solar activity.

Type III events are fast frequency drift bursts, which can occur singly, in groups, or in

storms. Naturally, solar type III radio bursts are produced by relatively low-energy electron

beams at a speed of about c/3, where c is the speed of light, with the kinetic energy being ∼30

keV [6,8,9]. Various previous studies have examined the energy budget of a limited number

of energy components in certain flares., which is distributed into kinetic energy, strong

radiation of the plasma, as well as energetic non-thermal particles. In tens of minutes they can

convert in excess of 1032

ergs of magnetic energy into accelerated particles, heated plasma,

and ejected solar material. [10,11]. The signal intensity for a type III burst can vary with

frequency.

Solar type II radio bursts are the electromagnetic signatures of magnetohydrodynamic

(MHD) shocks propagating outward in the solar atmosphere [12,13]. The frequency drift from

high to lowfrequencies (typically ∼0.5 MHz s−1

) results from the decrease of electron density

(Ne) and hence the plasma frequency, with increasing radial distance (r) in the solar

atmosphere [14].

The observed frequency drift rate can be converted into a velocity if the dependence of

electron density ne on height is known, and it is found that a typical speed is of order 1000


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kms-1

[15,16]. It is said to be bigger than the Alfven speed in the corona [17]. The widely

accepted steps in the type II radio burst emission models are (1) acceleration of electrons by

an MHD shock, (2) excitation of Langmuir (plasma) waves by the accelerated electron

streams, and (3) conversion of the Langmuir waves into escaping radiation at the local

electron plasma frequency (F) and its harmonic (H) [18].

2. METHODOLOGY AND INSTRUMENTATION

The focus of this research is to use the available observational data of solar radio bursts

from e-CALLISTO network. This event occurred on 1st July 2015 at 13:52 UT (complex

solar burst type III) and 13:40 UT - 13:44 UT (solar burst type II). This event is quit unique

because there are two different types of burst that occurred during low activity. The events are

very clear recorded by the six different sites of the e-CALLISTO network. The CALLISTO

stand for Compound Astronomical Low frequency, Low cost Instrument for Spectroscopy and

Transportable Observatory [26].

CALLISTO is the network that received the 24 hours solar observations [27]. The

antenna of e CALLISTO was installed almost around the world such as Humain in Belgium,

Irkutsk in Russia, Zurich and Bleien in Switzerland, Ooty in India, San Jose in Costa Rica,

Green Bank WV in USA, and in Mexico [28]. The different sites from e-Callisto network that

detected the bursts on 1st

June 2015 were illustrated in the Figure 1 below.


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Figure 1. Different sites from e-Callisto network that detected the bursts on 1st June 2015 at 1332

and 13:40 UT - 13:44 UT at (i) BIR, (ii) BLENSW, (iii) Essen, (iv) Glascow (v) Osra, (vi) Rwanda.

3. RESULTS AND DISCUSSION

We have carried out an analysis of the this 1st June event to that taken from e-

CALLISTO network. The energy going into plasma heating during each flare was estimated

by computing the time evolution of the energy content of the thermal plasma and obtaining

the peak value.

This constitutes a lower limit to the thermal energy, since it does not account for the

cooling of the plasma prior to this time nor to any heating at later times. Each of these

additional contributions are considered separately below; they are believed that there is a gap

before the evolution of the peak thermal energy.

Therefore, we can observe in a 12 minutes, the formation type II burst is formed after a

complex and a group of type III burst. No attempt was made to determine the kinetic energy

of turbulent and directed plasma motions, since no spectrally resolved lines were available to

give a measure of line broadening caused by such bulk motions.

In the present study, there is no direct correlation is seen between the type III burst

duration and either the type III intensity. Our immediate focus is an analysis is to observe the

probabilities for significant disturbances in Earth’s magnetic field are given for three activity

levels which are active, minor storm, and severe storm.


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Figure 2. Solar burst group type III and II detected at different sites from e-Callisto network on 1st

June 2015 at 1332 and13:40 UT - 13:44 UT UT. Type III burst followed by a type II with split band

observed. Figure: Solar burst type detected at (i) BIR, (ii) BLENSW, (iii) Essen, (iv) Glascow (v)

Osra, (vi) Rwanda.


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FLARE 0 – 24 Hour 24 – 48 Hour

CLASS M 01% 01%

CLASS X 01% 01%

FLARE 0 – 24 Hour 24 – 48 Hour

CLASS M 01% 01%

CLASS X 01% 01%

Figure 3. Data on Flare, Class M, and Class C (Credited to SolarMonitor)


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Figure 4. The sun's X-ray output had not completely flat lined, but the pulse was weak. Solar flare

activity was very low. Moreover, it was likely to remain so. NOAA forecasters said the odds of an X-

class flare was no more than 1%. However, there are no large coronal holes on the Earthside of the sun

Credit: SDO/HMI.

There are four sunspots of the active regions (AR2355, AR2356, AR2357, and

AR2358) during this event. However, the active region, AR2356 is more active compared to

others. This active region potentially produce 1% of M-class and X-class within 24hours. The

M-class flares are medium sized and they may cause brief radio blackouts that affect Earth’s

polar region. The radio flux during that time is 94 SFU and sunspot number is 47. It can be

considered that the Sun is at low activity. Table below show the data on Mid –and High

latitudes.


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0 – 24 Hour 24 – 48 Hour

ACTIVE 10% 10%

MINOR 01% 01%

SEVERE 01% 01%

Figure 5. Data on Mid-latitudes (Credited to SolarMonitor).

0 – 24 Hour 24 – 48 Hour

ACTIVE 10% 10%

MINOR 01% 01%

SEVERE 01% 01%

Figure 6. Data on High Latitudes (Credited to SolarMonitor).

To characterize the proton flux across the full integral energy range, we also determined

the shape of the energy spectra at both peak event. The solar wind recorded during the event

is 342.4 km/s and the density of the proton recorded is 4.1 protons/cm3. Another important

consideration is that, there are some evidence that radio-quiet CMEs mostly came from the

edges of the sun.

4. CONCLUSIONS

The main goal of this study was to determine whether is there any possibilities that the

radio burst can be formed even the Sun is at low activity and this event is one of the case.

Some CMEs produce radiation storms, and some don't, or at least the level of radiation is

significantly lower. The spectral shape consists of high flux densities at meter wavelengths. It

is shown that the density of protn might be a main reason why the structure of both burst

could be occurred during that time. It is also believed that the meter wavelength branch of the

this type III spectrum may be attributable to second-phase accelerated electrons to form type

II burst. It should be noted that normally, the type III burst usually produced the plasma to be

excited and therefore the type II burst can be potentially happen.

ACKNOWLEDGMENT

We are grateful to CALLISTO network, STEREO, LASCO, SDO/AIA, NOAA and SWPC make their data

available online. This work was partially supported by the 600-RMI/FRGS 5/3 (135/2014) and 600-RMI/RAGS

5/3 (121/2014) UiTM grants and Kementerian Pengajian Tinggi Malaysia. Special thanks to the National Space


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Agency and the National Space Centre for giving us a site to set up this project and support this project. Solar

burst monitoring is a project of cooperation between the Institute of Astronomy, ETH Zurich, and FHNW

Windisch, Switzerland, Universiti Teknologi MARA and University of Malaya. This paper also used NOAA

Space Weather Prediction Centre (SWPC) for the sunspot, radio flux and solar flare data for comparison

purpose. The research has made use of the National Space Centre Facility and a part of an initiative of the

International Space Weather Initiative (ISWI) program.

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( Received 22 December 2015; accepted 05 January 2016 )

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