Broadband microwave sub-second pulsations in an expanding coronal loop of the 2011 August 10 flare

Mészárosová, H.; Rybák, J.; Kashapova, L. K.; Gömöry, P.; Tokhchukova, S. Kh.; Myshyakov, I. I.

doi:10.1051/0004-6361/201528062

Cited by 11 publications

(10 citation statements)

References 43 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The tadpole signature has been found in the spectra of rapidly propagating disturbances observed using white light (Katsiyannis et al 2003;Nakariakov et al 2004), and in EUV (Nisticò et al 2014) which also allows spatial information about the wave trains to be measured (see also Yuan et al 2013). Similar signatures are also frequently detected in post-flare radio emission (e.g., Mészárosová et al 2009Mészárosová et al , 2016Karlický et al 2013), suggesting a common physical cause which is further supported by recent multi-wavelength studies such as the simultaneous detection of QPPs in hard X-ray, radio, and EUV bands . Goddard et al (2016) report the observation of a quasi-periodic wave train and shock-generated type II radio bursts having the same periodicity of approximately 1.8 minutes.…”

Section: Introductionmentioning

confidence: 82%

Dispersive Evolution of Nonlinear Fast Magnetoacoustic Wave Trains

Pascoe

Goddard

Nakariakov

2017

ApJL

View full text Add to dashboard Cite

Quasi-periodic rapidly propagating wave trains are frequently observed in extreme ultraviolet observations of the solar corona, or are inferred by the quasi-periodic modulation of radio emission. The dispersive nature of fast magnetohydrodynamic waves in coronal structures provides a robust mechanism to explain the detected quasiperiodic patterns. We perform 2D numerical simulations of impulsively generated wave trains in coronal plasma slabs and investigate how the behavior of the trapped and leaky components depend on the properties of the initial perturbation. For large amplitude compressive perturbations, the geometrical dispersion associated with the waveguide suppresses the nonlinear steepening for the trapped wave train. The wave train formed by the leaky components does not experience dispersion once it leaves the waveguide and so can steepen and form shocks. The mechanism we consider can lead to the formation of multiple shock fronts by a single, large amplitude, impulsive event and so can account for quasi-periodic features observed in radio spectra.

show abstract

Section: Introductionmentioning

confidence: 82%

Dispersive Evolution of Nonlinear Fast Magnetoacoustic Wave Trains

Pascoe

Goddard

Nakariakov

2017

ApJL

View full text Add to dashboard Cite

show abstract

“…Recently, Mészárosová et al (2016) reported a subsecond pulsation (0.07-1.49 s period) in broadband microwave (4-7 GHz) emission for 70 s during a C-class flare. The pulsation was associated with an expanding hot loop observed in the AIA 131, 94, and 193 Å channels.…”

Section: Discussionmentioning

confidence: 99%

Observation of a Short Period Quasi-periodic Pulsation in Solar X-Ray, Microwave, and EUV Emissions

Kumar

Nakariakov

Cho

2017

ApJ

View full text Add to dashboard Cite

This paper presents the multi-wavelength analysis of a 13 s quasi-periodic pulsation (QPP) observed in hard X-ray (12-300 keV) and microwave (4.9-34 GHz) emissions during a C-class flare occurred on 21 September 2015. AIA 304 and 171Å images show an emerging loop/flux tube (L1) moving radially outward, which interacts with preexisting structures within the active region. The QPP was observed during the expansion and rising motion of L1. The Nobeyama Radioheliograph (NoRH) microwave images in 17/34 GHz channels reveal a single radio source, which was co-spatial with a neighboring loop (L2). In addition, using AIA 304Å images, we detected intensity oscillations in the legs of loop L2 with a period of about 26 s. A similar oscillation period was observed in the GOES soft X-ray flux derivative. This oscillation period seems to increase with time. We suggest that the observed QPP is most likely generated by the interaction between loops L2 and L3 observed in the AIA hot channels (131 and 94Å). The merging speed of loops L2 and L3 was ∼35 km s −1 . Loop L1 destroyed possibly by its interaction with preexisting structures in the active region and produced a cool jet with the speed ∼106-118 km s −1 associated with a narrow CME (∼770 km s −1 ). Another mechanism of the QPP in terms of a sausage oscillation of the loop (L2) is also possible.

show abstract

“…(v) Fifthly, the slab tadpole waves (green crosses) mean a planar (two-dimensional) geometry where the tadpole tail precedes its head. Whereas the real cylindrical waveguides (three-dimensional) can have a rather circular cross-section profile with axes R1 ≈ R2, and the planar slab tadpole wave (Katsiyannis et al 2003;Mészárosová et al 2009aMészárosová et al ,b, 2014Mészárosová et al , 2016 can be realised in a heavily flattened cylinder (with, e.g. R1 << R2).…”

Section: Trapped and Leakage Tadpole Wave Modesmentioning

confidence: 99%

Magnetically coupled atmosphere, fast sausage MHD waves, and forced magnetic field reconnection during the SOL2014-09-10T17:45 flare

Meszarosova,

Gomory

2020

Preprint

View full text Add to dashboard Cite

Aims. We study the physical properties and behaviour of the solar atmosphere during the GOES X1.6 solar flare on 2014 September 10.Methods. The steady plasma flows and the fast sausage MHD waves were analysed with the wavelet separation method. The magnetically coupled atmosphere and the forced magnetic field reconnection were studied with the help of the Vertical-Current Approximation Non-linear Force-Free Field code.Results. We studied a mechanism of MHD wave transfer from the photosphere without dissipation or reflection before reaching the corona and a mechanism of the wave energy distribution over the solar corona. We report a common behaviour of (extreme)ultraviolet steady plasma flows (speed of 15.3→10.9 km s −1 ) and fast sausage MHD waves (Alfvén speed of 13.7→10.3 km s −1 and characteristic periods of 1 587→1 607 s), propagating in cylindrical plasma waveguides of the individual atmospheric layers (photosphere→corona) observed by SDO/AIA/HMI and IRIS space instruments. A magnetically coupled solar atmosphere by a magnetic field flux tube above a sunspot umbra and a magnetic field reconnection forced by the waves were analysed. The solar seismology with trapped, leakage, and tunnelled modes of the waves, dissipating especially in the solar corona, is discussed with respect to its possible contribution to the outer atmosphere heating.Conclusions. We demonstrate that a dispersive nature of fast sausage MHD waves, which can easily generate the leaky and other modes propagating outside of their waveguide, and magnetic field flux tubes connecting the individual atmospheric layers can distribute the magnetic field energy across the active region. This mechanism can contribute to the coronal energy balance and to our knowledge on how the coronal heating is maintained.

show abstract

Broadband microwave sub-second pulsations in an expanding coronal loop of the 2011 August 10 flare

Cited by 11 publications

References 43 publications

Dispersive Evolution of Nonlinear Fast Magnetoacoustic Wave Trains

Dispersive Evolution of Nonlinear Fast Magnetoacoustic Wave Trains

Observation of a Short Period Quasi-periodic Pulsation in Solar X-Ray, Microwave, and EUV Emissions

Magnetically coupled atmosphere, fast sausage MHD waves, and forced magnetic field reconnection during the SOL2014-09-10T17:45 flare

Contact Info

Product

Resources

About