Kinematics and Energetics of the EUV Waves on 11 April 2013

Fulara, Aarti; Chandra, Ramesh; Chen, P. F.; Zhelyazkov, I.; Srivastava, A. K.; Uddin, Wahab

doi:10.1007/s11207-019-1445-3

Cited by 15 publications

(11 citation statements)

References 77 publications

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“…As a proof of concept we validate our model (INFROS) for an Earth-directed CME which erupted from the Sun on 2013 April 11 at around 06:50 UT. The CME was associated with an M6.6 class solar flare (Cohen et al 2014;Lario et al 2014;Vemareddy & Zhang 2014;Vemareddy & Mishra 2015;Joshi et al 2017;Fulara et al 2019) that occurred in the active region (AR) 11719. Its arrival at the L1 point was detected with the signature of shock arrival on 2013 April 13 at 22:54 UT, FR leading edge on 2013 April 14 at 17:00 UT and a trailing edge on 2013 April 15 at 19:30 UT.…”

Section: Infros Model Validation: a Test Case For The Cme Event On 20...mentioning

confidence: 99%

An Observationally Constrained Analytical Model for Predicting the Magnetic Field Vectors of Interplanetary Coronal Mass Ejections at 1 au

Sarkar

Gopalswamy

Srivastava

2020

ApJ

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We report on an observationally constrained analytical model, the INterplanetary Flux ROpe Simulator (INFROS), for predicting the magnetic-field vectors of coronal mass ejections (CMEs) in the interplanetary medium. The main architecture of INFROS involves using the near-Sun flux rope properties obtained from the observational parameters that are evolved through the model in order to estimate the magnetic field vectors of interplanetary CMEs (ICMEs) at any heliocentric distance. We have formulated a new approach in INFROS to incorporate the expanding nature and the time-varying axial magnetic field-strength of the flux rope during its passage over the spacecraft. As a proof of concept, we present the case study of an Earth-impacting CME which occurred on 2013 April 11. Using the near-Sun properties of the CME flux rope, we have estimated the magnetic vectors of the ICME as intersected by the spacecraft at 1 AU. The predicted magnetic field profiles of the ICME show good agreement with those observed by the in-situ spacecraft. Importantly, the maximum strength (10.5 ± 2.5 nT) of the southward component of the magnetic field (Bz) obtained from the model prediction, is in agreement with the observed value (11 nT). Although our model does not include the prediction of the ICME plasma parameters, as a first order approximation it shows promising results in forecasting of Bz in near real time which is critical for predicting the severity of the associated geomagnetic storms. This could prove to be a simple space-weather forecasting tool compared to the time-consuming and computationally expensive MHD models.

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Section: Infros Model Validation: a Test Case For The Cme Event On 20...mentioning

confidence: 99%

An Observationally Constrained Analytical Model for Predicting the Magnetic Field Vectors of Interplanetary Coronal Mass Ejections at 1 au

Sarkar

Gopalswamy

Srivastava

2020

ApJ

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“…In the past decade, the Atmospheric Imaging Assembly (AIA) on board Solar Dynamics Observatory (SDO) allowed to acquire observation data with unprecedented high spatial and temporal resolutions, revealing more detailed features of EUV waves. Events with both wave and non-wave components are found to be very common (Chen & Wu 2011;Asai et al 2012;Liu et al 2013;Cunha-Silva et al 2018;Fulara et al 2019). Such observations are also supported by three-dimensional (3D) models (Cohen et al 2009;Downs et al 2012).…”

Section: Introductionmentioning

confidence: 59%

Exploring the Nature of EUV Waves in a Radiative Magnetohydrodynamic Simulation

Wang,

Chen,

Ding

2021

Preprint

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Coronal extreme-ultraviolet (EUV) waves are large-scale disturbances propagating in the corona, whose physical nature and origin have been discussed for decades. We report the first three dimensional (3D) radiative magneto-hydrodynamic (RMHD) simulation of a coronal EUV wave and the accompanying quasi-periodic wave trains. The numerical experiment is conducted with the MURaM code and simulates the formation of solar active regions through magnetic flux emergence from the convection zone to the corona. The coronal EUV wave is driven by the eruption of a magnetic flux rope that also gives rise to a C-class flare. It propagates in a semi-circular shape with an initial speed ranging from about 550 to 700 km s −1 , which corresponds to an average Mach number (relative to fast magnetoacoustic waves) of about 1.2. Furthermore, the abrupt increase of the plasma density, pressure and tangential magnetic field at the wavefront confirms fast-mode shock nature of the coronal EUV wave. Quasi-periodic wave trains with a period of about 30 s are found as multiple secondary wavefronts propagating behind the leading wavefront and ahead of the erupting magnetic flux rope. We also note that the true wavefront in the 3D space can be very inhomogeneous, however, the lineof-sight integration of EUV emission significantly smoothes the sharp structures in 3D and leads to a more diffuse wavefront.

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“…However, in some recent observations, it was revealed that stationary fronts can also be created by fast-mode EUV waves (Chandra et al 2016;Fulara et al 2019). Using MHD simulations, Chen et al (2016) reproduced this type of stationary fronts and proposed that they are different in nature from those found before (Delannée & Aulanier 1999).…”

Section: Introductionmentioning

confidence: 91%

“…Due to their association with filament eruptions, coronal mass ejections (CMEs, Chen & Wu 2011;Chandra et al 2016Chandra et al , 2018b, type II radio bursts (Nitta et al 2013;Chandra et al 2018a;Fulara et al 2019), solar energetic particles (SEPs), and solar flares, the study of EUV waves becomes very interesting and crucial to understand the underlying physics behind these manifestations. One of the important consequences of EUV waves is to produce coronal loop oscillations (Ballai et al 2005;Kumar et al 2013;Guo et al 2015;Fulara et al 2019) and filament/prominence oscillations (Asai et al 2012;Shen et al 2014;Srivastava et al 2016). These oscillatory phenomena are useful for coronal seismology in order to derive the coronal magnetic field, which is still challenging to measure.…”

Section: Introductionmentioning

confidence: 99%

Fine Structures of an EUV Wave Event from Multi-Viewpoint Observations

Chandra,

Chen,

Devi

et al. 2021

Preprint

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In this study, we investigate an extreme ultraviolet (EUV) wave event on 2010 February 11, which occurred as a limb event from the Earth viewpoint and a disk event from the STEREO-B viewpoint. We use the data obtained by the Atmospheric Imaging Assembly (AIA) aboard the Solar Dynamics Observatory (SDO) in various EUV channels. The EUV wave event was launched by a partial prominence eruption. Similar to some EUV wave events in previous works, this EUV wave event contains a faster wave with a speed of ∼445±6 km s −1 , which we call coronal Moreton wave, and a slower wave with a speed of ∼298±5 km s −1 , which we call "EIT wave". The coronal Moreton wave is identified as a fast-mode wave and the "EIT wave" is identified as an apparent propagation due to successive field-line stretching. We also observe a stationary front associated with the fast mode EUV wave. This stationary front is explained as mode conversion from the coronal Moreton wave to a slow-mode wave near a streamer.

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Kinematics and Energetics of the EUV Waves on 11 April 2013

Cited by 15 publications

References 77 publications

An Observationally Constrained Analytical Model for Predicting the Magnetic Field Vectors of Interplanetary Coronal Mass Ejections at 1 au

An Observationally Constrained Analytical Model for Predicting the Magnetic Field Vectors of Interplanetary Coronal Mass Ejections at 1 au

Exploring the Nature of EUV Waves in a Radiative Magnetohydrodynamic Simulation

Fine Structures of an EUV Wave Event from Multi-Viewpoint Observations

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