Types of Microwave Quasi-Periodic Pulsations in Single Flaring Loops

Kupriyanova, E. G.; Melnikov, V. F.; Nakariakov, V. M.; Shibasaki, Κ.

doi:10.1007/s11207-010-9642-0

Cited by 122 publications

(109 citation statements)

References 25 publications

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“…Nevertheless, the detection and analysis of QPP signals, including the statistical surveys [7][8][9][10][11] and automated detection techniques [10], are traditionally carried out by methods based upon the Fourier transform, for example, the windowed Fourier, wavelet analysis, Hilbert transform, and Wigner-Ville (WV) transform. This approach assumes that the signal has a harmonic shape, possibly with slowly modulated amplitude and period.…”

Section: Qpp Detection and Analysismentioning

confidence: 99%

“…Moreover, the Morlet mother function that is commonly used in the QPP study (e.g. [7]), is not designed for accounting for the period modulation within the wavelet. Application of this technique is illustrated in the third column of figure 4.…”

Section: Qpp Detection and Analysismentioning

confidence: 99%

“…Detrending techniques that are less subjective, are the use of an autocorrelation function of the light curve (see, e.g. [7]), or the lowest intrinsic mode determined by EMD (see, e.g. [32]).…”

Section: The Trendmentioning

confidence: 99%

“…Recent commissioning of the new generation of space-borne and ground-based instruments that provide an almost uninterrupted monitoring of the Sun, allowed for statistical studies of QPP. It was established that QPP are a statistically significant feature of solar flares in both non-thermal [7] and thermal [8,9] emission. This conclusion excludes the possible occurrence of apparent QPP because of the red noise or the superposition of multiple unrelated flares.…”

Section: Introductionmentioning

confidence: 99%

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Non-stationary quasi-periodic pulsations in solar and stellar flares

Nakariakov

Kolotkov

Kupriyanova

et al. 2018

Plasma Phys. Control. Fusion

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Often the enhanced electromagnetic radiation generated in solar and stellar flares shows a pronounced (quasi)-oscillatory pattern-quasi-periodic pulsations (QPP), with characteristic periods ranging from a fraction of a second to several tens of minutes. We review recent advances in the empirical study of QPP in solar and stellar flares, addressing the intrinsic nonstationarity of the signal, i.e. the variation of its amplitude, period or phase with time. This nonstationarity could form a basis for a classification of QPP, necessary for revealing specific physical mechanisms responsible for their appearance. We could identify two possible classes of QPP, decaying harmonic oscillations, and trains of symmetric triangular pulsations. Apparent similarities between QPP and irregular geomagnetic pulsations Pi offer a promising avenue for the knowledge transfer in both analytical techniques and theory. Attention is also paid to the effect of the flare trend on the detection and analysis of QPP.

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Section: Qpp Detection and Analysismentioning

confidence: 99%

Section: Qpp Detection and Analysismentioning

confidence: 99%

Section: The Trendmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Non-stationary quasi-periodic pulsations in solar and stellar flares

Nakariakov

Kolotkov

Kupriyanova

et al. 2018

Plasma Phys. Control. Fusion

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show abstract

“…QPPs are classified mainly as short QPPs (sub-second), medium QPPs (seconds to several minutes), and long QPPs (from several minutes to tens of minutes) according to the possible physical mechanisms associated with them (Nakariakov & Melnikov, 2009;Kupriyanova et al, 2010). According to Aschwanden (1987), the short QPPs are probably connected with the interaction of electromagnetic, plasma, or whistler waves with accelerated particles detected in the radio emission.…”

Section: Introductionmentioning

confidence: 99%

Study of multi-periodic coronal pulsations during an X-class solar flare

Chowdhury

Srivastava

Dwivedi

et al. 2015

Advances in Space Research

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We investigate quasi-periodic coronal pulsations during the decay phase of an X 3.2 class flare on 14 May 2013, using soft X-ray data from the RHESSI satellite. Periodogram analyses of soft X-ray light curves show that ∼ 53 s and ∼ 72 s periods co-exist in the 3-6, 6-12 and 12-25 KeV energy bands. Considering the typical length of the flaring loop system and observed periodicities, we find that they are associated with multiple (first two harmonics) of fast magnetoacoustic sausage waves. The phase relationship of soft X-ray emissions in different energy bands using cross-correlation technique show that these modes are standing in nature as we do not find the phase lag. Considering the period ratio, we diagnose the local plasma conditions of the flaring region by invoking MHD seismology. The period ratio P 1 /2P 2 is found to be ∼ 0.65, which indicates that such oscillations are most likely excited in longitudinal density stratified loops.

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Soft X-Ray Pulsations in Solar Flares

Simões¹,

Hudson²,

Fletcher³

2016

Solar and Stellar Flares

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The soft X-ray emissions (hν > 1.5 keV) of solar flares come mainly from the bright coronal loops at the highest temperatures normally achieved in the flare process. Their ubiquity has led to their use as a standard measure of flare occurrence and energy, although the overwhelming bulk of the total flare energy goes elsewhere. Recently Dolla et al. (2012, Astrophys. J. Lett. 749 L16) noted quasi-periodic pulsations (QPP) in the soft X-ray signature of the X-class flare SOL2011-02-15, as observed by the standard photometric data from the GOES (Geostationary Operational Environmental Satellite) spacecraft. In this paper we analyze the suitability of the GOES data for this kind of analysis and find them to be generally valuable after September, 2010 (GOES-15). We then extend the Dolla et al. result to a complete list of X-class flares from Cycle 24, and show that most of them (80%) display QPPs in the impulsive phase. The pulsations show up cleanly in both channels of the GOES data, making use of time-series of irradiance differences (the digital time derivative on the 2-s sampling). We deploy different techniques to characterize the periodicity of GOES pulsations, considering the red-noise properties of the flare signals, finding a range of chracteristic time scales of the QPPs for each event, but usually with no strong signature of a single period dominating in the power spectrum. The QPP may also appear on somewhat longer time scales during the later gradual phase, possibly with a greater tendency towards coherence, but the sampling noise in GOES difference data for large irradiance values (Xclass flares) makes these more uncertain. We show that there is minimal phase difference between the differenced GOES energy channels, or between them and the hard X-ray variations on short time scales. During the impulsive phase the footpoints of the newly-forming flare loops may also contribute to the observed soft X-ray variations.

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Types of Microwave Quasi-Periodic Pulsations in Single Flaring Loops

Cited by 122 publications

References 25 publications

Non-stationary quasi-periodic pulsations in solar and stellar flares

Non-stationary quasi-periodic pulsations in solar and stellar flares

Study of multi-periodic coronal pulsations during an X-class solar flare

Soft X-Ray Pulsations in Solar Flares

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