Quaternary Geology Inventory, Lower Nelson River Basin (63I,J,G, 64G,H)

Klassen, R W; Netterville, J. A.

doi:10.4095/121241

Cited by 19 publications

(25 citation statements)

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“…Inconsistencies in speeds between Moreton and EUV waves (Klassen et al 2000), as well as the observation of stationary fronts (Delannée & Aulanier 1999) led to alternate interpretations and models for the observed wavelike signatures. There are two main opposing theories, waves and non-waves, to explain the visible features of EUV waves.…”

Section: Introductionmentioning

confidence: 99%

Coronal Response to an Euv Wave From Dem Analysis

Vanninathan

Veronig

Dissauer

et al. 2015

ApJ

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EUV (Extreme-Ultraviolet) waves are globally propagating disturbances that have been observed since the era of the SoHO/EIT instrument. Although the kinematics of the wave front and secondary wave components have been widely studied, there is not much known about the generation and plasma properties of the wave. In this paper we discuss the effect of an EUV wave on the local plasma as it passes through the corona. We studied the EUV wave, generated during the 2011 February 15 X-class flare/CME event, using Differential Emission Measure diagnostics. We analyzed regions on the path of the EUV wave and investigated the local density and temperature changes. From our study we have quantitatively confirmed previous results that during wave passage the plasma visible in the Atmospheric Imaging Assembly (AIA) 171Å channel is getting heated to higher temperatures corresponding to AIA 193Å and 211Å channels. We have calculated an increase of 6 -9% in density and 5 -6% in temperature during the passage of the EUV wave. We have compared the variation in temperature with the adiabatic relationship and have quantitatively demonstrated the phenomenon of heating due to adiabatic compression at the wave front. However, the cooling phase does not follow adiabatic relaxation but shows slow decay indicating slow energy release being triggered by the wave passage. We have also identified that heating is taking place at the front of the wave pulse rather than at the rear. Our results provide support for the case that the event under study here is a compressive fast-mode wave or a shock.

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Section: Introductionmentioning

confidence: 99%

Coronal Response to an Euv Wave From Dem Analysis

Vanninathan

Veronig

Dissauer

et al. 2015

ApJ

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“…In wave models, they are interpreted as a fastmode wave, most likely triggered by a CME, and represent the coronal counterpart of the Moreton waves (see, e.g., Vršnak & Cliver 2008;Patsourakos & Vourlidas 2012). In the non-wave models, they are explained by other processes related to the large-scale magnetic field reconfiguration and can be interpreted as a disk projection of the expanding envelope of the CME (see, e.g., Delannée & Aulanier 1999;Chen et al 2005;Attrill et al 2007), being usually much slower and more diffuse (see, e.g., Klassen et al 2000;Warmuth et al 2004a,b). According to Klassen et al (2000), 90% of the metric type II bursts are associated with EUV waves, but there is no correlation between their speeds.…”

Section: Introductionmentioning

confidence: 99%

Solar type II radio bursts associated with CME expansions as shown by EUV waves

Cunha-Silva

Fernandes

Selhorst

2015

A&A

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Aims. We investigate the physical conditions of the sources of two metric type II bursts associated with coronal mass ejection (CME) expansions with the aim of verifying the relationship between the shocks and the CMEs by comparing the heights of the radio sources and of the extreme-ultraviolet (EUV) waves associated with the CMEs. Methods. The heights of the EUV waves associated with the events were determined in relation to the wave fronts. The heights of the shocks were estimated by applying two different density models to the frequencies of the type II emissions and compared with the heights of the EUV waves. For the event on 13 June 2010 that included band-splitting, the shock speed was estimated from the frequency drifts of the upper and lower frequency branches of the harmonic lane, taking into account the H/F frequency ratio f H / f F = 2. Exponential fits on the intensity maxima of the frequency branches were more consistent with the morphology of the spectrum of this event. For the event on 6 June 2012 that did not include band-splitting and showed a clear fundamental lane on the spectrum, the shock speed was directly estimated from the frequency drift of the fundamental emission, determined by linear fit on the intensity maxima of the lane. For each event, the most appropriate density model was adopted to estimate the physical parameters of the radio source. Results. The event on 13 June 2010 had a shock speed of 590-810 km s −1 , consistent with the average speed of the EUV wave fronts of 610 km s −1 . The event on 6 June 2012 had a shock speed of 250-550 km s −1 , also consistent with the average speed of the EUV wave fronts of 420 km s −1 . For both events, the heights of the EUV wave revealed to be compatible with the heights of the radio source, assuming a radial propagation of the type-II-emitting shock segment.

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“…(2) On the one hand, the wave front expansion speed ranges from 458 km s −1 to 762 km s −1 in different directions, roughly of the order of the average surface projected expansion speeds for fast-mode waves (Wang 2000). These speeds appear greater than typical EUV waves speeds of 200-400 km s −1 (Klassen et al 2000;Thompson & Myers 2009). The EUV wave was faster than the blowout jet speed (190-350 km s −1 ), and the EUV wave front was easily distinguishable from the bubble-like CME structure.…”

Section: Discussionmentioning

confidence: 99%

A Blowout Jet Associated with One Obvious Extreme-ultraviolet Wave and One Complicated Coronal Mass Ejection Event

Miao

Liu

et al. 2018

ApJ

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In this paper, we present a detailed analysis of a coronal blowout jet eruption which was associated with an obvious extreme-ultraviolet (EUV) wave and one complicated coronal mass ejection (CME) event based on the multi-wavelength and multi-view-angle observations from Solar Dynamics Observatory and Solar Terrestrial Relations Observatory. It is found that the triggering of the blowout jet was due to the emergence and cancellation of magnetic fluxes on the photosphere. During the rising stage of the jet, the EUV wave appeared just ahead of the jet top, lasting about 4 minutes and at a speed of 458 -762 km s −1 . In addition, obvious dark material is observed along the EUV jet body, which confirms the observation of a mini-filament eruption at the jet base in the chromosphere. Interestingly, two distinct but overlapped CME structures can be observed in corona together with the eruption of the blowout jet. One is in narrow jet-shape, while the other one is in bubble-shape. The jet-shaped component was unambiguously related with the outwardly running jet itself, while the bubble-like one might either be produced due to the reconstruction of the high coronal fields or by the internal reconnection during the mini-filament ejection according to the double-CME blowout jet model firstly proposed by , suggesting more observational evidence should be supplied to clear the current ambiguity based on large samples of blowout jets in future studies.

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Quaternary Geology Inventory, Lower Nelson River Basin (63I,J,G, 64G,H)

Cited by 19 publications

References 0 publications

Coronal Response to an Euv Wave From Dem Analysis

Coronal Response to an Euv Wave From Dem Analysis

Solar type II radio bursts associated with CME expansions as shown by EUV waves

A Blowout Jet Associated with One Obvious Extreme-ultraviolet Wave and One Complicated Coronal Mass Ejection Event

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