DH Type II Radio Bursts During Solar Cycles 23 and 24: Frequency-Dependent Classification and Their Flare-CME Associations

Patel, Binal D.; Joshi, Bhuwan; Cho, Kyung-Suk; Kim, Rok‐Soon

doi:10.1007/s11207-021-01890-6

Cited by 12 publications

(3 citation statements)

References 33 publications

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“…The latter percentages could increase with a maximum of 9% if all cases with data gaps turned out to have radio bursts. The reverse association from IP IIs to SFs is investigated in [48] and it was shown that 82% of IP type IIs are associated with SFs in SC23, whereas the association is only slightly reduced to 71% for SC24. As type III bursts are much more frequent compared to type IIs, any investigation over the last two SCs on the link between IP IIIs and solar activity phenomena would require substantial efforts.…”

Section: Discussionmentioning

confidence: 99%

M-Class Solar Flares in Solar Cycles 23 and 24: Properties and Space Weather Relevance

Miteva

Samwel

2022

Universe

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A comprehensive statistical analysis on the properties and accompanied phenomena of all M-class solar flares (as measured in soft X-rays) in the last two solar cycles (1996–2019) is presented here with a focus on their space weather potential. The information about the parent active region and the underlying sunspot (Hale) type is collected for each case, where possible, in order to identify photospheric precondition as precursors for the solar flare eruption or confinement. Associations with coronal mass ejections, solar energetic particles, and interplanetary radio emissions are also evaluated and discussed as possible proxies for flare eruption and subsequent space weather relevance. The results show that the majority (∼80%) of the analyzed M-class flares are of β, β-γ, and β-γ-δ magnetic field configuration. The M-class population of flares is accompanied by CMEs in 41% of the cases and about half of the flare sample has been associated with radio emission from electron beams. A much lower association (≲10%) is obtained with shock wave radio signatures and energetic particles. Furthermore, a parametric scheme is proposed in terms of occurrence rates between M-class flares and a variety of accompanied solar phenomena as a function of flare sub-classes or magnetic type. This study confirms the well-known reduced but inevitable space weather importance of M-class flares.

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Section: Discussionmentioning

confidence: 99%

M-Class Solar Flares in Solar Cycles 23 and 24: Properties and Space Weather Relevance

Miteva

Samwel

2022

Universe

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“…The studies concerning the onset and triggering of a solar flare, filament/prominence eruption, and CME have established that these are different manifestations of the same explosive magnetic eruption in the solar atmosphere (Forbes 2000;Moore et al 2001;Chen 2017;Green et al 2018;Georgoulis et al 2019). In addition to these phenomena, a shock can also be considered as a fourth aspect of the eruption, present at the front and flanks of the CME if the CME's speed exceeds the local Alfvén speed (Cho et al 2008;Gopalswamy et al 2012;Patel et al 2021). Contemporary observations also reveal a few special categories of CMEs, for example, narrow (Gilbert et al 2001;Chen 2011), streamer-puff (Bemporad et al 2005;Panesar et al 2016a), and stealth CMEs (Howard & Harrison 2013;O'Kane et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Source Region and Launch Characteristics of Magnetic-arch-blowout Solar Coronal Mass Ejections Driven by Homologous Compact-flare Blowout Jets

Patel,

Joshi,

Sterling

et al. 2024

ApJ

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We study the formation of four coronal mass ejections (CMEs) originating from homologous blowout jets. All of the blowout jets originated from NOAA Active Region (AR) 11515 on 2012 July 2, within a time interval of ≈14 hr. All of the CMEs were wide (angular widths ≈ 95°–150°), and propagated with speeds ranging between ≈300 and 500 km s−1 in LASCO coronagraph images. Observations at various EUV wavelengths in Solar Dynamics Observatory/Atmospheric Imaging Assembly images reveal that in all the cases, the source region of the jets lies at the boundary of the leading part of AR 11515 that hosts a small filament before each event. Coronal magnetic field modeling based on nonlinear force-free extrapolations indicates that in each case, the filament is contained inside of a magnetic flux rope that remains constrained by overlying compact loops. The southern footpoint of each filament is rooted in the negative polarity region where the eruption onsets occur. This negative polarity region undergoes continuous flux changes, including emergence and cancellation with opposite polarity in the vicinity of the flux rope, and the EUV images reveal brightening episodes near the filament’s southeastern footpoint before each eruption. Therefore, these flux changes are likely the cause of the subsequent eruptions. These four homologous eruptions originate near adjacent feet of two large-scale loop systems connecting from that positive polarity part of the AR to two remote negative polarity regions, and result in large-scale consequences in the solar corona.

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“…We will also address the issue of directivity in the events detected simultaneously by at least two widely separated spacecraft. Recently, Patel et al (2021) studied DH type II radio bursts during the past two solar cycles. Since type IVs and type IIs are generally considered as a radio diagnostic of strong CMEs, this work will complement the aforementioned study, forming a unique combined database of particle acceleration signatures of interplanetary CMEs.…”

Section: Introductionmentioning

confidence: 99%

Interplanetary Type IV Solar Radio Bursts: A Comprehensive Catalog and Statistical Results

Mohan,

Gopalswamy,

Kumari

et al. 2024

ApJ

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Decameter hectometric (DH; 1–14 MHz) type IV radio bursts are produced by flare-accelerated electrons trapped in postflare loops or the moving magnetic structures associated with the coronal mass ejections (CMEs). From a space weather perspective, it is important to systematically compile these bursts, explore their spectrotemporal characteristics, and study the associated CMEs. We present a comprehensive catalog of DH type IV bursts observed by the Radio and Plasma Wave Investigation instruments on board the Wind and Solar TErrestrial RElations Observatory spacecraft covering the period of white-light CME observations by the Large Angle and Spectrometric Coronagraph on board the Solar and Heliospheric Observatory mission between 1996 November and 2023 May. The catalog has 139 bursts, of which 73% are associated with a fast (>900 km s−1) and wide (>60°) CME, with a mean CME speed of 1301 km s−1. All DH type IV bursts are white-light CME-associated, with 78% of the events associated with halo CMEs. The CME source latitudes are within ±45°. Seventy-seven events had multiple-vantage-point observations from different spacecraft, letting us explore the impact of the line of sight on the dynamic spectra. For 48 of the 77 events, there were good data from at least two spacecraft. We find that, unless occulted by nearby plasma structures, a type IV burst is best viewed when observed within a ±60° line of sight. Also, bursts with a duration above 120 minutes have source longitudes within ±60°. Our inferences confirm the inherent directivity in the type IV emission. Additionally, the catalog forms a Sun-as-a-star DH type IV burst database.

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DH Type II Radio Bursts During Solar Cycles 23 and 24: Frequency-Dependent Classification and Their Flare-CME Associations

Cited by 12 publications

References 33 publications

M-Class Solar Flares in Solar Cycles 23 and 24: Properties and Space Weather Relevance

M-Class Solar Flares in Solar Cycles 23 and 24: Properties and Space Weather Relevance

Source Region and Launch Characteristics of Magnetic-arch-blowout Solar Coronal Mass Ejections Driven by Homologous Compact-flare Blowout Jets

Interplanetary Type IV Solar Radio Bursts: A Comprehensive Catalog and Statistical Results

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