The 17 January 2005 Complex Solar Radio Event Associated with Interacting Fast Coronal Mass Ejections

Hillaris, A.; Malandraki, O.; Klein, Karl‐Ludwig; Preka‐Papadema, P.; Moussas, X.; Bouratzis, C.; Mitsakou, E.; Tsitsipis, P.; Kontogeorgos, A.

doi:10.1007/s11207-011-9872-9

Cited by 11 publications

(15 citation statements)

References 38 publications

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“…as consequence of CME-CME interaction are in fact frequently reported (see, e.g., Reiner et al, 2003, Hillaris et al, 2011, Martínez Oliveros et al, 2012, Ding et al, 2014b. We note that the description of such a scenario is intimately connected to the 3D geometry and propagation direction of two CMEs.…”

Section: Radio Signatures Of Cme-cme Interactionsupporting

confidence: 52%

The Interaction of Successive Coronal Mass Ejections: A Review

et al. 2017

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We present a review of the different aspects associated with the interaction of successive coronal mass ejections (CMEs) in the corona and inner heliosphere, focusing on the initiation of series of CMEs, their interaction in the heliosphere, the particle acceleration associated with successive CMEs, and the effect of compound events on Earth's magnetosphere. The two main mechanisms resulting in the eruption of series of CMEs are sympathetic eruptions, when one eruption triggers another, and homologous eruptions, when a series of similar eruptions originates from one active region. CME-CME interaction may also be associated with two unrelated eruptions. The interaction of successive CMEs has been observed remotely in coronagraphs (with the Large Angle and Spectrometric Coronagraph Experiment -LASCO-since the early 2000s) and heliospheric imagers (since the late 2000s), and inferred from in situ measurements, starting with early measurements in the 1970s. The interaction of two or more CMEs is associated with complex phenomena, including magnetic reconnection, momentum exchange, the propagation of a fast magnetosonic shock through a magnetic ejecta, and changes in the CME expansion. The presence of a preceding CME a few hours before a fast eruption has been found to be connected with higher fluxes of solar energetic particles (SEPs), while CME-CME interaction occurring in the corona is often associated with unusual radio bursts, indicating electron acceleration. Higher suprathermal population, enhanced turbulence and wave activity, stronger shocks, and shock-shock or shock-CME interaction have been proposed as potential physical mechanisms to explain the observed associated SEP events. When measured in situ, CME-CME interaction may be associated with relatively well organized multiple-magnetic cloud events, instances of shocks propagating through a previous magnetic ejecta or more complex ejecta, when the characteristics of the individual eruptions cannot be easily distinguished. CME-CME interaction is associated with some of the most intense recorded geomagnetic storms. The compression of a CME by another and the propagation of a shock inside a magnetic ejecta can lead to extreme values of the southward magnetic field component, sometimes associated with large values of the dynamic pressure. This can result in intense geomagnetic storms, but also trigger substorms and large earthward motions of the magnetopause, potentially associated with changes in the outer radiation belts. Future in situ measurements in the inner heliosphere by Solar Probe+ and Solar Orbiter may shed light on the evolution of CMEs as they interact, by providing opportunities for conjunction and evolutionary studies.

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Section: Radio Signatures Of Cme-cme Interactionsupporting

confidence: 52%

The Interaction of Successive Coronal Mass Ejections: A Review

et al. 2017

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“…The type IV IP burst started at 10:55 UT on 17 January and ended by 18 January at 02:00 UT (event catalog number 14), for an overview of the dynamic spectrum see Figure 3 of Hillaris et al (2011). The coronal extension of the type IV IP burst was found to originate from AR10720 and persisted throughout the duration of its interplanetary counterpart.…”

Section: Overview Of the 17 January 2005 Extended Event Evolutionmentioning

confidence: 99%

“…A detailed study of the radio signatures of this event ( Table 1 in Hillaris et al, 2011, that presents a comprehensive outline of its time evolution) points towards possible multiple acceleration mechanisms. These include CME associated shocks in the high corona and the interplanetary space, and also, shock-independent accelerators at low altitudes associated with the type IV continuum behind the CME.…”

Section: Overview Of the 17 January 2005 Extended Event Evolutionmentioning

confidence: 99%

“…Often, in flare/CME events, the transition from the type-U and J bursts to the typical type III mark the restructuring, or opening, of the magnetic field lines as originally confined, energetic electrons gain access to open magnetic lines. An example of dynamic radio spectra showing this transition from U and J-type bursts to a standard type III burst at the beginning of the 17 January 2005 event can be found in Hillaris et al (2011). In the hectometric and kilometric regime, long duration storms of individual type III bursts Stone, 1970a,b, 1971;Bougeret, Fainberg, and Stone, 1983) covering several days (5.4 on average after Kayser et al, 1987) were recorded.…”

Section: Introductionmentioning

confidence: 96%

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Interplanetary Type IV Bursts

2016

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We study the characteristics of moving type IV radio bursts which extend to the hectometric wavelengths (interplanetary type IV or type IV IP bursts) and their relationship with energetic phenomena on the Sun. Our dataset comprises 48 interplanetary type IV bursts observed with the Radio and Plasma Wave Investigation (WAVES) instrument onboard Wind in the 13.825 MHz-20 kHz frequency range. The dynamic spectra of the Radio Solar Telescope Network (RSTN), the Nançay Decametric Array (DAM), the Appareil de Routine pour le Traitement et l' Enregistrement Magnetique de l' Information Spectral (ARTEMIS-IV), the Culgoora, Hiraiso and Izmiran Radio Spectrographs were used to track the evolution of the events in the low corona. These were supplemented with soft X-ray (SXR) flux-measurements from the Geostationary Operational Environmental Satellite (GOES) and coronal mass ejections (CME) data from the Large Angle and Spectroscopic Coronagraph (LASCO) onboard the Solar and Heliospheric Observatory (SOHO). Positional information of the coronal bursts was obtained by the Nançay radioheliograph (NRH). We examined the relationship of the type IV events with coronal radio bursts, CMEs and SXR flares. The majority of the events (45) were characterized as compact; their duration was on average 106 minutes. This type of events was, mostly, associated with M-and X-class flares (40 out of 45) and fast CMEs; 32 of these events had CMEs faster than 1000 km s −1 . Furthermore, in 43 compact events the CME was, possibly, subjected to reduced aerodynamic drag as it was propagating in the wake of a previous CME. A minority (three) of long lived type IV IP bursts was detected, with duration from 960 minutes to 115 hours. These events are referred to as extended or long duration and appear to replenish their energetic electron content, possibly from electrons escaping from the corresponding coronal type IV bursts. The latter were found to persist on the disk, for tens of hours to days. Prominent among them was the unusual interplanetary type IV burst of 18-23 May 2002, which is the longest event in the Wind /WAVES catalog. The three extended events were, usually, accompanied by a number of flares, of GOES class C in their majority, and of CMEs, many of which were slow and narrow.

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“…The CME-CME merging process is assumed to be revealed in radio observations as strong enhancement in type II bursts (see e.g., Gopalswamy et al 2001Gopalswamy et al , 2002Hillaris et al 2011;Kahler & Vourlidas 2014). The effects of such complex CME entities at Earth's magnetosphere cover extended periods of negative B z (e.g.…”

Section: Effects Of the Ambient Environment On Cme Propagationmentioning

confidence: 99%

Kinematical properties of coronal mass ejections

Temmer

2016

Astron Nachr

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Coronal mass ejections (CMEs) are the most dynamic phenomena in our solar system. They abruptly disrupt the continuous outflow of solar wind by expelling huge clouds of magnetized plasma into interplanetary space with velocities enabling to cross the Sun-Earth distance within a few days. Earth-directed CMEs may cause severe geomagnetic storms when their embedded magnetic fields and the shocks ahead compress and reconnect with the Earth's magnetic field. The transit times and impacts in detail depend on the initial CME velocity, size, and mass, as well as on the conditions and coupling processes with the ambient solar wind flow in interplanetary space. The observed CME parameters may be severly affected by projection effects and the constant changing environmental conditions are hard to derive. This makes it difficult to fully understand the physics behind CME evolution, preventing to do a reliable forecast of Earth-directed events. This short review focusing on observational data, shows recent methods which were developed to derive the CME kinematical profile for the entire Sun-Earth distance range as well as studies which were performed to shed light on the physical processes that CMEs encounter when propagating from Sun to Earth.Comment: accepted for publication in Astronomische Nachrichte

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The 17 January 2005 Complex Solar Radio Event Associated with Interacting Fast Coronal Mass Ejections

Cited by 11 publications

References 38 publications

The Interaction of Successive Coronal Mass Ejections: A Review

The Interaction of Successive Coronal Mass Ejections: A Review

Interplanetary Type IV Bursts

Kinematical properties of coronal mass ejections

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