An Analysis of Interplanetary Solar Radio Emissions Associated With a Coronal Mass Ejection

Krupař, V.; Eastwood, J. P.; Krupařová, O.; Santolı́k, O.; Souček, J; Magdalenić, Jasmina; Vourlidas, A.; Maksimović, M.; Bonnin, X.; Bothmer, V.; Mrotzek, Niclas; Pluta, Adam; Barnes, David; Davies, J. A.; Oliveros, J. C. Martinez; Bale, S. D.

doi:10.3847/2041-8205/823/1/l5

Cited by 21 publications

(19 citation statements)

References 43 publications

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“…The conclusion in section 4 regarding the type II radio emission being emitted at the second harmonic rests on the assumption that the source position of the type II radio emission is close to the CME nose. This is not necessarily the case, as many type II radio bursts have been reported to originate from the CME flank (e.g., Feng et al, 2013;Krupar et al, 2016;Magdalenić et al, 2014;Shen et al, 2013;Xie et al, 2012). Mäkelä et al (2018) were able to locate the radio emission source of the 6 July 2012 CME to the CME nose using radio Figure 9.…”

Section: Discussionmentioning

confidence: 99%

Modeling the Multiple CME Interaction Event on 6–9 September 2017 with WSA‐ENLIL+Cone

et al. 2019

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A series of coronal mass ejections (CMEs) erupted from the same active region between 4–6 September 2017. Later, on 6–9 September, two interplanetary (IP) shocks reached L1, creating a complex and geoeffective plasma structure. To understand the processes leading up to the formation of the two shocks, we model the CMEs with the Wang‐Sheeley‐Arge (WSA)‐ENLIL+Cone model. The first two CMEs merged already in the solar corona driving the first IP shock. In IP space, another fast CME presumably interacted with the flank of the preceding CMEs and caused the second shock detected in situ. By introducing a customized density enhancement factor (dcld) in the WSA‐ENLIL+Cone model based on coronagraph image observations, the predicted arrival time of the first IP shock was drastically improved. When the dcld factor was tested on a well‐defined single CME event from 12 July 2012 the shock arrival time saw similar improvement. These results suggest that the proposed approach may be an alternative to improve the forecast for fast and simple CMEs. Further, the slowly decelerating kilometric type II radio burst confirms that the properties of the background solar wind have been preconditioned by the passage of the first IP shock. This likely caused the last CME to experience insignificant deceleration and led to the early arrival of the second IP shock. This result emphasizes the need to take preconditioning of the IP medium into account when making forecasts of CMEs erupting in quick succession.

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Section: Discussionmentioning

confidence: 99%

Modeling the Multiple CME Interaction Event on 6–9 September 2017 with WSA‐ENLIL+Cone

et al. 2019

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“…However, the active region has been observed by STEREO-A/Sun Earth Connection Coronal and Heliospheric Investigation/Extreme Ultraviolet Imager (SEC-CHI/EUVI; Howard et al 2008). We have used the wavelet technique by Stenborg et al (2008) to produce a composite image for the 171Å and 195Å channels ( The favorable configuration of Wind and STEREO-A allows us to accurately locate the sources of the type III bursts by radio triangulation (Krupar et al 2014a(Krupar et al , 2016. We identified data points that correspond to peak fluxes for four pairs of frequency channels observed by Wind /WAVES (428 kHz, 484 kHz, 548 kHz, and 624 kHz) and STEREO-A/WAVES (425 kHz, 475 kHz, 525 kHz, 625 kHz) with signals above background levels.…”

Section: Type III Bursts Measurementsmentioning

confidence: 99%

Density Fluctuations in the Solar Wind Based on Type III Radio Bursts Observed by Parker Solar Probe

Krupař

Szabó

Maksimović

et al. 2020

ApJS

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Radio waves are strongly scattered in the solar wind, so that their apparent sources seem to be considerably larger and shifted than the actual ones. Since the scattering depends on the spectrum of density turbulence, better understanding of the radio wave propagation provides indirect information on the relative density fluctuations = δn / n at the effective turbulence scale length. Here, we have analyzed 30 type III bursts detected by Parker Solar Probe (PSP). For the first time, we have retrieved type III burst decay times τ d between 1 MHz and 10 MHz thanks to an unparalleled temporal resolution of PSP. We observed a significant deviation in a power-law slope for frequencies above 1 MHz when compared to previous measurements below 1 MHz by the twin-spacecraft Solar TErrestrial RElations Observatory (STEREO) mission. We note that altitudes of radio bursts generated at 1 MHz roughly coincide with an expected location of the Alfvén point, where the solar wind becomes super-Alfvénic. By comparing PSP observations and Monte Carlo simulations we predict relative density fluctuations at the effective turbulence scale length at radial distances between 2.5 R and 14 R to range from 0.22 and 0.09. Finally, we calculated relative density fluctuations measured in situ by PSP at a radial distance from the Sun of 35.7 R during the perihelion #1, and the perihelion #2 to be 0.07 and 0.06, respectively. It is in a very good agreement with previous STEREO predictions ( = 0.06 − 0.07) obtained by remote measurements of radio sources generated at this radial distance.

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“…Morosan et al (2014) have shown the low-frequency type III bursts at the expanding flank of a CME. Krupar et al (2016) analyzed the type II and type III bursts and concluded that the radio emission arises from the flanks of the CME. Electrons generating type III bursts are produced at magnetic reconnection with open, nearly radial magnetic field lines, along which the electrons propagate.…”

Section: Comparison Of Corpuscular and Radio Emissionsmentioning

confidence: 99%

“…Note that the applied fitting procedure is aimed only at formal interpolating and extrapolating of the observed bursts. For such a goal, we use a simple approximation that fits the radio data, while many other formal approximations could alsodo the job (for a pattern of non-formal, in-depth consideration, see, e.g., Krupar et al 2016). …”

Section: Associated Electromagnetic Emissionsmentioning

confidence: 99%

Investigating the Origins of Two Extreme Solar Particle Events: Proton Source Profile and Associated Electromagnetic Emissions

Kocharov

Pohjolainen

Mishev

et al. 2017

ApJ

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We analyze the high-energy particle emission from the Sun in two extreme solar particle eventsin which protons are accelerated to relativistic energies and can cause a significant signal even in the ground-based particle detectors. Analysis of a relativistic proton event is based on modeling of the particle transport and interaction, from a nearSun source through the solar wind and the Earth's magnetosphere and atmosphere to a detector on the ground. This allows us to deduce the time profile of the proton source at the Sun and compare it with observed electromagnetic emissions. The 1998 May 2 event is associated with aflare and a coronal mass ejection (CME), which were well observed by the Nançay Radioheliograph, thusthe images of theradio sources are available. For the 2003 November 2 event, the low corona images of the CME liftoff obtained at the Mauna Loa Solar Observatoryare available. Those complementary data sets are analyzed jointly with the broadband dynamic radio spectra, EUV images, and other data available for both events. We find a common scenario for both eruptions, including the flare's dual impulsive phase, the CME-launch-associated decimetric-continuum burst, and the late, low-frequency type III radio bursts at the time of the relativistic proton injection into the interplanetary medium. The analysis supports the idea that the two considered events start with emission of relativistic protons previously accelerated during the flare and CME launch, then trapped in large-scale magnetic loops and later released by the expanding CME.

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An Analysis of Interplanetary Solar Radio Emissions Associated With a Coronal Mass Ejection

Cited by 21 publications

References 43 publications

Modeling the Multiple CME Interaction Event on 6–9 September 2017 with WSA‐ENLIL+Cone

Modeling the Multiple CME Interaction Event on 6–9 September 2017 with WSA‐ENLIL+Cone

Density Fluctuations in the Solar Wind Based on Type III Radio Bursts Observed by Parker Solar Probe

Investigating the Origins of Two Extreme Solar Particle Events: Proton Source Profile and Associated Electromagnetic Emissions

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