Origin of Coronal Shock Waves Associated With Slow Coronal Mass Ejections

Magdalenić, Jasmina; Marqué, C.; Zhukov, A. N.; Vršnak, Bojan; Žic, Tomislav

doi:10.1088/0004-637x/718/1/266

Cited by 60 publications

(47 citation statements)

References 42 publications

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“…The rise of the CMEs was not synchronized with the rise phase of the flare, while the onset time of the type II burst fell between the onset and the peak energy release of the flare. Similar cases were reported by Magdalenić et al (2008Magdalenić et al ( , 2010.…”

Section: Discussionsupporting

confidence: 89%

“…The most compelling support of a flare interpretation of type II bursts was provided by both White et al (2007) and Magdalenić et al (2008Magdalenić et al ( , 2010. White et al (2007) presented a type II burst that was associated with a long-duration CME-less X3.6-class flare.…”

Section: Introductionmentioning

confidence: 95%

“…The heights of the NRH sources at 236 and 164 MHz were used to select the most appropriate density model. The method we used is similar to the one presented by Magdalenić et al (2008Magdalenić et al ( , 2010. We obtained the electron densities N e corresponding to the frequencies f = 236/2 = 118 MHz and f = 164/2 = 82 MHz, by employing the equation for the plasma frequency f ≈ 9 √ N e , where N e is expressed in cm −3 and f in kHz (since we assumed harmonic emission for the type II burst, the NRH frequencies were converted to the fundamental ones by halving their values).…”

Section: The 2000 March 2 Eventmentioning

confidence: 99%

“…White et al (2007) presented a type II burst that was associated with a long-duration CME-less X3.6-class flare. Magdalenić et al (2008Magdalenić et al ( , 2010) considered a limb event and using radio and EUV images showed that the impulsive CME acceleration in their event lagged the type II burst that was synchronized with the associated flare.…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

On the relationship of shock waves to flares and coronal mass ejections

Nindos

Alissandrakis

Hillaris

et al. 2011

A&A

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Context. Metric type II bursts are the most direct diagnostic of shock waves in the solar corona. Aims. There are two main competing views about the origin of coronal shocks: that they originate in either blast waves ignited by the pressure pulse of a flare or piston-driven shocks due to coronal mass ejections (CMEs). We studied three well-observed type II bursts in an attempt to place tighter constraints on their origins. Methods. The type II bursts were observed by the ARTEMIS radio spectrograph and imaged by the Nançay Radioheliograph (NRH) at least at two frequencies. To take advantage of projection effects, we selected events that occurred away from disk center. Results. In all events, both flares and CMEs were observed. In the first event, the speed of the shock was about 4200 km s −1 , while the speed of the CME was about 850 km s −1 . This discrepancy ruled out the CME as the primary shock driver. The CME may have played a role in the ignition of another shock that occurred just after the high speed one. A CME driver was excluded from the second event as well because the CMEs that appeared in the coronagraph data were not synchronized with the type II burst. In the third event, the kinematics of the CME which was determined by combining EUV and white light data was broadly consistent with the kinematics of the type II burst, and, therefore, the shock was probably CME-driven. Conclusions. Our study demonstrates the diversity of conditions that may lead to the generation of coronal shocks.

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Section: Discussionsupporting

confidence: 89%

Section: Introductionmentioning

confidence: 95%

Section: The 2000 March 2 Eventmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

On the relationship of shock waves to flares and coronal mass ejections

Nindos

Alissandrakis

Hillaris

et al. 2011

A&A

View full text Add to dashboard Cite

show abstract

“…It may be driven by two possible physical mechanisms, i.e. (i) a blast wave ignited by the pressure pulse of a flare (Vrsnak et al, 1995;Vršnak and Lulić, 2000a;Vršnak and Lulić, 2000b;Khan and Aurass, 2002;Narukage et al, 2002;Hudson et al, 2003;Magdalenić et al, 2010), (ii) a piston-driven shock due to a CME (Klassen et al, 1999;Klassen, Pohjolainen, and Klein, 2003;Cho et al, 2011). Thus, coronal shock waves may be associated with solar flares, CMEs, or some combination of these phenomena (Magara et al, 2000;Magdalenić et al, 2008;Vršnak and Cliver, 2008).…”

Section: Introductionmentioning

confidence: 99%

Multiwavelength Study of a Solar Eruption from AR NOAA 11112: II. Large-Scale Coronal Wave and Loop Oscillation

et al. 2012

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We analyse multiwavelength observations of an M2.9/1N flare that occurred in AR NOAA 11112 on 16 October 2010. AIA 211Å EUV images reveal the presence of a faster coronal wave (decelerating from ≈1390 to ≈830 km s −1 ) propagating ahead of a slower wave (decelerating from ≈416 to ≈166 km s −1 ) towards the western limb. The dynamic radio spectrum from Sagamore Hill radio telescope shows the presence of metric type II radio burst, which reveals the presence of a coronal shock wave (speed≈800 km s −1 ). The speed of the faster coronal wave derived from AIA 211Å images is found to be comparable to the coronal shock speed. AIA 171Å high-cadence observations showed that a coronal loop, which was located at the distance of ≈0.32R to the west of the flaring region, started to oscillate by the end of the impulsive phase of the flare. The results indicate that the faster coronal wave may be the first driver of the transversal oscillations of coronal loop. As the slower wave passed through the coronal loop, the oscillations became even stronger. There was a plasmoid eruption observed in EUV and a white-light CME was recorded, having velocity of ≈340-350 km s −1 . STEREO 195Å images show an EIT wave, propagating in the same direction of the lower-speed coronal wave observed in AIA, but decelerating from ≈320 to ≈254 km s −1 . These observations reveal the co-existence of both waves (i.e. coronal Moreton and EIT waves), and type II radio burst seems to be associated with the coronal Moreton wave.

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Coronal Shock Waves, EUV Waves, and Their Relation to CMEs. I. Reconciliation of “EIT Waves”, Type II Radio Bursts, and Leading Edges of CMEs

Grechnev

Uralov

Chertok

et al. 2011

Energy Storage and Release Through the Solar Activity Cycle

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We show examples of excitation of coronal waves by flare-related abrupt eruptions of magnetic rope structures. The waves presumably rapidly steepened into shocks and freely propagated afterwards like decelerating blast waves that showed up as Moreton waves and EUV waves. We propose a simple quantitative description for such shock waves to reconcile their observed propagation with drift rates of metric type II bursts and kinematics of leading edges of coronal mass ejections (CMEs). Taking account of different plasma density falloffs for propagation of a wave up and along the solar surface, we demonstrate a close correspondence between drift rates of type II bursts and speeds of EUV waves, Moreton waves, and CMEs observed in a few known events.

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Origin of Coronal Shock Waves Associated With Slow Coronal Mass Ejections

Cited by 60 publications

References 42 publications

On the relationship of shock waves to flares and coronal mass ejections

On the relationship of shock waves to flares and coronal mass ejections

Multiwavelength Study of a Solar Eruption from AR NOAA 11112: II. Large-Scale Coronal Wave and Loop Oscillation

Coronal Shock Waves, EUV Waves, and Their Relation to CMEs. I. Reconciliation of “EIT Waves”, Type II Radio Bursts, and Leading Edges of CMEs

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