The 6 September 2017 X9 Super Flare Observed From Submillimeter to Mid‐IR

Castro, C. G. Giménez de; Raulin, J. P.; Simões, Paulo J. A.; Kudaka, A. S.; Válio, Adriana

doi:10.1029/2018sw001969

Cited by 17 publications

(7 citation statements)

References 32 publications

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“…We could see that the non-thermal electrons are well correlated with MRO 11.2GHz light-curve, non-thermal electron beams accelerated and penetrated into deeper corona before the main HXMT hard X-ray phase. Later the non-thermal electrons lose their energy in the 'thick target' immediately, non-thermal electrons density decreases, heating the base corona or even the chromosphere, which might be an explanation to the mid-IR emission discussed in Giménez de Castro et al (2018). However during the whole flaring process, GS source beam size and the mean transverse magnetic field did not show drastic changes (see the results present in the figure 7), those findings also support our hypothesis of the GS source and its initial configuration.…”

Section: Magnetic Field and Non-thermal Electron Evolution Of Gs Sourcementioning

confidence: 97%

Non-thermal electron energization during the impulsive phase of an X9.3 flare revealed by Insight-HXMT

Zhang,

Wang,

et al. 2021

Preprint

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The X9.3 flare SOL20170906T11:55 was observed by the CsI detector aboard the first Chinese Xray observatory Hard X-ray Modulation telescope (Insight-HXMT). By using wavelets method, we report about 22s quasiperiodic pulsations(QPPs) during the impulsive phase. And the spectra from 100 keV to 800 keV showed the evolution with the gamma-ray flux, of a power-law photon index from ∼ 1.8 before the peak, ∼ 2.0 around the flare peak, to ∼ 1.8 again. The gyrosynchrotron microwave spectral analysis reveals a 36.6 ± 0.6 radius gyrosynchrotron source with mean transverse magnetic field around 608.2 Gauss, and the penetrated ≥ 10 keV non-thermal electron density is about 10 6.7 cm −3 at peak time. The magnetic field strength followed the evolution of high-frequency radio flux. Further gyrosynchrotron source modeling analysis implies that there exists a quite steady gyrosynchrotron source, the non-thermal electron density and transverse magnetic field evolution are similar to higherfrequency light curves. The temporally spectral analysis reveals that those non-thermal electrons are accelerated by repeated magnetic reconnection, likely from a lower corona source.

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Section: Magnetic Field and Non-thermal Electron Evolution Of Gs Sourcementioning

confidence: 97%

Non-thermal electron energization during the impulsive phase of an X9.3 flare revealed by Insight-HXMT

Zhang,

Wang,

et al. 2021

Preprint

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“…In September 2017 a quite interesting period of solar activity occurred with an X9.3‐class flare, the strongest solar flare in more than a decade, during its maximum phase (Chamberlin et al, ; Gimenez de Castro et al, ). The period from 3 to 13 September 2017 gave us an insight into solar‐terrestrial interaction and allowed us to study its influence on navigation in more detail.…”

Section: Introductionmentioning

confidence: 99%

Ionospheric Response to the X9.3 Flare on 6 September 2017 and Its Implication for Navigation Services Over Europe

et al. 2018

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On 6 September 2017, an X-class flare of the magnitude 9.3 occurred around noon UT, being the strongest flare event in a decade. The flare itself was the highlight of a quite interesting phase of solar-terrestrial interactions caused by the active region known as the Catania sunspot group 46 or active region number 2673 on the NOAA catalog. From 3 to 13 September 2017 strong flare activities occurred, accompanied by a number of radio bursts and earthward-directed coronal mass ejections. Solar wind influences at Earth were modest during the flare activity and limited to the polar regions (Linty et al., 2018, https://doi.org/10.1029/2018SW001940). But, the strong X9.3 flare itself had impacts on the dayside ionosphere causing some problems in navigation services as we present within this paper. The event data observed and analyzed give us the opportunity to improve our understanding of strong and extreme space weather events and allow us to distinguish between the influence of the different event classes on our technological infrastructure within periods of strong solar activity. Here we will discuss our observations with special focus on the X9.3 flare event and provide examples how the flare itself influenced services in the domains of aviation and maritime navigation in the European sector.

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“…These studies have reported a good temporal or spatial agreement (or both) between mid-IR data and emission from other wavelengths, such as: microwaves (MW; Kaufmann et al 2013), hard X-rays (HXR; Kaufmann et al 2013;Penn et al 2016), white-light (Kaufmann et al 2013;Penn et al 2016;Giménez de Castro et al 2018), and ultraviolet (UV) emission (Miteva et al 2016). Moreover, when compared to the flare emission in the submillimeter domain, the mid-IR presents higher flux density values.…”

Section: Introductionmentioning

confidence: 90%

“…The analysis of solar flares in mid-IR wavelengths, λ > 5 µm, is a new area of research with only a few events reported in the literature thus far. Kaufmann et al (2013Kaufmann et al ( , 2015, Miteva et al (2016) and Giménez de Castro et al (2018) used commercial IR cameras in the focus of small telescopes at room temperature with apertures ranging from 10 to 20 cm that produce images with diffraction limits around 15 and sensors centered at λ = 10 µm (ν = 30 THz). These observations revealed that the mid-IR emission originates from compact regions and displays impulsive behavior.…”

Section: Introductionmentioning

confidence: 99%

A solar flare driven by thermal conduction observed in mid-infrared

López

Castro

Mandrini

et al. 2022

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Context. The mid-infrared (mid-IR) range has been mostly unexplored for the investigation of solar flares. It is only recently that new mid-IR flare observations have begun opening a new window into the response and evolution of the solar chromosphere. These new observations have been mostly performed by the AR30T and BR30T telescopes that are operating in Argentina and Brazil, respectively. Aims. We present the analysis of SOL2019-05-15T19:24, a GOES class C2.0 solar flare observed at 30 THz (10 μm) by the ground-based telescope AR30T. Our aim is to characterize the evolution of the flaring atmosphere and the energy transport mechanism in the context of mid-IR emission. Methods. We performed a multi-wavelength analysis of the event by complementing the mid-IR data with diverse ground- and space-based data from the Solar Dynamics Observatory (SDO), the H-α Solar Telescope for Argentina, and the Expanded Owens Valley Solar Array (EOVSA). Our study includes the analysis of the magnetic field evolution of the flaring region and of the development of the flare. Results. The mid-IR images from AR30T show two bright and compact flare sources that are spatially associated with the flare kernels observed in ultraviolet (UV) by SDO. We confirm that the temporal association between mid-IR and UV fluxes previously reported for strong flares is also observed for this small flare. The EOVSA microwave data revealed flare spectra consistent with thermal free-free emission, which lead us to dismiss the existence of a significant number of non-thermal electrons. We thus consider thermal conduction as the primary mechanism responsible for energy transport. Our estimates for the thermal conduction energy and total radiated energy fall within the same order of magnitude, reinforcing our conclusions.

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The 6 September 2017 X9 Super Flare Observed From Submillimeter to Mid‐IR

Cited by 17 publications

References 32 publications

Non-thermal electron energization during the impulsive phase of an X9.3 flare revealed by Insight-HXMT

Non-thermal electron energization during the impulsive phase of an X9.3 flare revealed by Insight-HXMT

Ionospheric Response to the X9.3 Flare on 6 September 2017 and Its Implication for Navigation Services Over Europe

A solar flare driven by thermal conduction observed in mid-infrared

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