Investigation of Relationship between High-energy X-Ray Sources and Photospheric and Helioseismic Impacts of X1.8 Solar Flare of 2012 October 23

Sharykin, I. N.; Kosovichev, A. G.; Sadykov, Viacheslav; Zimovets, I. V.; Myshyakov, I. I.

doi:10.3847/1538-4357/aa77f1

Cited by 23 publications

(30 citation statements)

References 36 publications

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“…Thus, one can conclude that helioseismic waves were generated during the whole impulsive phase and, probably, even in the pre-impulsive phase. Perhaps, the superposition of the helioseismic waves excited during the last two HXR peaks can explain the unusually long wavelength of the south-ward helioseismic wave (Kosovichev 2017).…”

Section: Helioseismic Flare Signalsmentioning

confidence: 99%

“…The value in each pixel is calculated as (I − I 0 )/I 0 , where I is the pixel value for a flare filtergram, and I 0 is the corresponding preflare value. We decided not to perform frequency filtering of the filtergram lightcurves to remove the variations caused by the line scanning as it was done in the paper of Sharykin et al (2017) because the photospheric signal was sufficiently strong in the flare emission sources. To demonstrate development of the photospheric emission we plot three filtergrams for 35 sec of the pre-impulsive phase (Fig.…”

Section: Helioseismic Flare Signalsmentioning

confidence: 99%

“…Recently, Sharykin et al (2017) used level-1 data from Helioseismic and Magnetic Imager (HMI) onboard Solar Dynamics Observatory (SDO) (Scherrer et al 2012), which represent filtergrams taken with different polarization filters across the Fe I 6173Å line the time cadence of ≈ 3.6 s by each of the two HMI cameras. The high temporal resolution allowed them to make a precise comparison between the hard X-ray emission (HXR) observed by Reuven Ramaty High Energy Spectroscopic Solar Imager (RHESSI), photospheric optical emission and sunquake sources of the X1.8 flare of October 23, 2012.…”

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confidence: 99%

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Onset of Photospheric Impacts and Helioseismic Waves in X9.3 Solar Flare of 2017 September 6

Sharykin

Kosovichev

2018

ApJ

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The X9.3 flare of September 6, 2017, was the most powerful flare of Solar Cycle 24. It generated strong white-light emission and multiple helioseismic waves (sunquakes). By using data from Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO) as well as hard X-ray data from KONUS instrument onboard WIND spacecraft, and Anti-Coincidence System (ACS) onboard the INTERGRAL space observatory, we investigate spatio-temporal dynamics of photospheric emission sources, identify sources of helioseismic waves and compare the flare photospheric dynamics with the hard X-ray (HXR) temporal profiles. The results show that the photospheric flare impacts started to develop in compact regions in close vicinity of the magnetic polarity inversion line (PIL) in the pre-impulsive phase before detection of the HXR emission. The initial photospheric disturbances were localized in the region of strong horizontal magnetic field of the PIL, and, thus, are likely associated with a compact sheared magnetic structure elongated along the PIL. The acoustic egression power maps revealed two primary sources of generation of sunquakes, which were associated with

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Section: Helioseismic Flare Signalsmentioning

confidence: 99%

Section: Helioseismic Flare Signalsmentioning

confidence: 99%

mentioning

confidence: 99%

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Onset of Photospheric Impacts and Helioseismic Waves in X9.3 Solar Flare of 2017 September 6

Sharykin

Kosovichev

2018

ApJ

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“…Notably, large energy flux densities between F12 and F13 have been inferred in bright solar flare kernels (Neidig et al 1993;Krucker et al 2011;Sharykin et al 2017), and we may expect values of the Balmer jump ratio as low as FcolorB 2 in spatially resolved, solar flare spectra as well as in spectra of dG superflares.…”

Section: Application To Superflares In Rapidly Rotating Dg Starsmentioning

confidence: 99%

“…Thus, these high energy particles are likely the source of powering most of the chromospheric heating and radiative response. Moreover, recent high spatial resolution imagery of NUV and optical footpoints in solar flares suggest a very high electron beam flux density (Fletcher et al 2007;Krucker et al 2011;Kleint et al 2016;Jing et al 2016;Kowalski et al 2017a;Sharykin et al 2017) which may be difficult to sustain due to plasma instabilities (Lee et al 2008;Li et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Parameterizations of Chromospheric Condensations in dG and dMe Model Flare Atmospheres

Kowalski

Allred

2018

ApJ

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The origin of the near-ultraviolet and optical continuum radiation in flares is critical for understanding particle acceleration and impulsive heating in stellar atmospheres. Radiative-hydrodynamic simulations in 1D have shown that high energy deposition rates from electron beams produce two flaring layers at T ∼ 10 4 K that develop in the chromosphere: a cooling condensation (downflowing compression) and heated non-moving (stationary) flare layers just below the condensation. These atmospheres reproduce several observed phenomena in flare spectra, such as the red wing asymmetry of the emission lines in solar flares and a small Balmer jump ratio in M dwarf flares. The high beam flux simulations are computationally expensive in 1D, and the (human) timescales for completing NLTE models with adaptive grids in 3D will likely be unwieldy for a time to come. We have developed a prescription for predicting the approximate evolved states, continuum optical depth, and the emergent continuum flux spectra of radiative-hydrodynamic model flare atmospheres. These approximate prescriptions are based on an important atmospheric parameter: the column mass (m ref ) at which hydrogen becomes nearly completely ionized at the depths that are approximately in steady state with the electron beam heating. Using this new modeling approach, we find that high energy flux density (>F11) electron beams are needed to reproduce the brightest observed continuum intensity in IRIS data of the 2014-Mar-29 X1 solar flare and that variation in m ref from 0.001 to 0.02 g cm −2 reproduces most of the observed range of the optical continuum flux ratios at the peaks of M dwarf flares.

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Physical properties of a fan-shaped jet backlit by an X9.3 flare

Pietrow

Druett

Rodríguez

et al. 2022

A&A

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Context. Fan-shaped jets sometimes form above light bridges and are believed to be driven by the reconnection of the vertical umbral field with the more horizontal field above the light bridges. Because these jets are not fully opaque in the wings of most chromospheric lines, it is not possible to study their spectra without highly complex considerations of radiative transfer in spectral lines from the atmosphere behind the fan. Aims. We take advantage of a unique set of observations of the Hα line along with the Ca II 8542 Å and Ca II K lines obtained with the CRISP and CHROMIS instrument of the Swedish 1-m Solar Telescope to study the physical properties of a fan-shaped jet that was backlit by an X9.3 flare. For what we believe to be the first time, we report an observationally derived estimate of the mass and density of material in a fan-shaped jet. Methods. The Hα flare ribbon emission profiles from behind the fan are highly broadened and flattened, allowing us to investigate the fan with a single slab via Beckers’ cloud model, as if it were backlit by a flat spectral profile of continuum emission. Using this model we derived the opacity and velocity of the material in the jet. Using inversions of Ca II 8542 Å emission via the STockholm inversion Code, we were also able to estimate the temperature and to cross-check the velocity of the material in the jet. Finally, we used the masses and the plane-of-sky and line-of-sight velocities as functions of time to investigate the downward supply of energy and momentum to the photosphere in the collapse of this jet, and evaluated it as a potential driver for a sunquake beneath. Results. We find that the physical properties of the fan material are reasonably chromospheric in nature, with a temperature of 7050 ± 250 K and a mean density of 2 ± 0.3 × 10−11 g cm−3. Conclusions. The total mass observed in Hα was found to be 3.9 ± 0.7 × 1013 g and the kinetic energy delivered to the base of the fan in its collapse was nearly two orders of magnitude below typical sunquake energies. We therefore rule out this jet as the sunquake driver, but cannot completely rule out larger fan jets as potential drivers.

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Investigation of Relationship between High-energy X-Ray Sources and Photospheric and Helioseismic Impacts of X1.8 Solar Flare of 2012 October 23

Cited by 23 publications

References 36 publications

Onset of Photospheric Impacts and Helioseismic Waves in X9.3 Solar Flare of 2017 September 6

Onset of Photospheric Impacts and Helioseismic Waves in X9.3 Solar Flare of 2017 September 6

Parameterizations of Chromospheric Condensations in dG and dMe Model Flare Atmospheres

Physical properties of a fan-shaped jet backlit by an X9.3 flare

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