Coronal mass ejections and type II radio bursts

Auraß, H.

doi:10.1007/bfb0106455

Cited by 43 publications

(29 citation statements)

References 55 publications

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“…Signatures of such shock waves appear as type II radio bursts in solar dynamic radio spectra (Mann 1995;Aurass 1997). These shock waves are able to accelerate electrons up to supra-thermal velocities, resulting in type II radio bursts.…”

Section: Solar Physics and Space Weathermentioning

confidence: 99%

LOFAR: The LOw-Frequency ARray

Haarlem

Wise

Gunst

et al. 2013

A&A

2,099

783

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LOFAR, the LOw-Frequency ARray, is a new-generation radio interferometer constructed in the north of the Netherlands and across europe. Utilizing a novel phased-array design, LOFAR covers the largely unexplored low-frequency range from 10-240 MHz and provides a number of unique observing capabilities. Spreading out from a core located near the village of Exloo in the northeast of the Netherlands, a total of 40 LOFAR stations are nearing completion. A further five stations have been deployed throughout Germany, and one station has been built in each of France, Sweden, and the UK. Digital beam-forming techniques make the LOFAR system agile and allow for rapid repointing of the telescope as well as the potential for multiple simultaneous observations. With its dense core array and long interferometric baselines, LOFAR achieves unparalleled sensitivity and angular resolution in the low-frequency radio regime. The LOFAR facilities are jointly operated by the International LOFAR Telescope (ILT) foundation, as an observatory open to the global astronomical community. LOFAR is one of the first radio observatories to feature automated processing pipelines to deliver fully calibrated science products to its user community. LOFAR's new capabilities, techniques and modus operandi make it an important pathfinder for the Square Kilometre Array (SKA). We give an overview of the LOFAR instrument, its major hardware and software components, and the core science objectives that have driven its design. In addition, we present a selection of new results from the commissioning phase of this new radio observatory.

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Section: Solar Physics and Space Weathermentioning

confidence: 99%

LOFAR: The LOw-Frequency ARray

Haarlem

Wise

Gunst

et al. 2013

A&A

2,099

783

View full text Add to dashboard Cite

show abstract

“…During large solar flare type iii burst can starts at frequency in GHz. Typically type III bursts will start at 10s or 100s of MHz and can start at even lower frequencies [5]. Some type III burst will only exist at high frequencies above 100MHz [6].…”

Section: Introductionmentioning

confidence: 99%

Preliminary Analysis on the Solar Burst Type III and the Effect of the Magnetic Reconnection

Husien

Hamidi

Shariff

et al. 2015

ILCPA

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ABSTRACT. 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.

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“…It should be noted that the direction of the source motion at a given frequency is on average found to be perpendicular between broadband radio pulsations (BBP) and zebra patterns (ZP) sources [6]. In the case of BBP, the frequency drift can be as high as (≈-250 MHz s −1 ) [7].…”

Section: Introductionmentioning

confidence: 99%

The Evolution of Unstable 'Beta-Gamma' Magnetic Fields of Active Region AR 2222

Hamidi

Sabri

Shariff

et al. 2015

ILCPA

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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/cm 3 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 Mclass 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.

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Coronal mass ejections and type II radio bursts

Cited by 43 publications

References 55 publications

LOFAR: The LOw-Frequency ARray

LOFAR: The LOw-Frequency ARray

Preliminary Analysis on the Solar Burst Type III and the Effect of the Magnetic Reconnection

The Evolution of Unstable 'Beta-Gamma' Magnetic Fields of Active Region AR 2222

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