Flare on 2011 September 22 and coronal mass ejection from observations in the He i 10830-Å line

Akimov, L. A.; Belkina, I. L.; Marchenko, G. P.

doi:10.1093/mnras/stt2344

Cited by 4 publications

(3 citation statements)

References 14 publications

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“…Using a scanning spectrograph, several maps of an active region were obtained before, during and after the development of an M3.2 flare, making it possible to derive the magnetic and dynamical disturbances at photospheric layers. Interestingly, some studies on flares have recently been published using data obtained in the same spectral region (e.g., Akimov et al 2014;Judge et al 2014;Sasso et al 2014;Zeng et al 2014). With a data set with similar characteristics, Judge et al (2014) concentrated their study on the seismic implications of the flare.…”

Section: Introductionmentioning

confidence: 99%

“…Sasso et al (2014) performed one scan of an active region after the onset of a flare and measured the Stokes profiles of the Si i 10827 Å line and of the He i 10830 Å triplet, deriving the magnetic structure of a filament present in the active region. Other works (e.g., Akimov et al 2014;Zeng et al 2014) only used either He i 10830 Å chromospheric filtergrams or intensity spectra. In this paper, we complement previous studies by analyzing the photospheric magnetic and dynamic changes in the emission region before, during and after the flare.…”

Section: Introductionmentioning

confidence: 99%

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Magnetic and Dynamical Photospheric Disturbances Observed During an M3.2 Solar Flare

Kuckein

Collados

Sainz

2015

ApJ

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This letter reports on a set of full-Stokes spectropolarimetric observations in the near infrared He i 10830Å spectral region covering the pre-, flare, and post-flare phases of an M3.2 class solar flare. The flare originated on 2013 May 17 and belonged to active region NOAA 11748. We detected strong He i 10830Å emission in the flare. The red component of the He i triplet peaks at an intensity ratio to the continuum of about 1.86. During the flare, He i Stokes V is substantially larger and appears reversed compared to the usually larger Si i Stokes V profile. The photospheric Si i inversions of the four Stokes profiles reveal the following:(1) the magnetic field strength in the photosphere decreases or is even absent during the flare phase, as compared to the pre-flare phase. However, this decrease is not permanent. After the flare the magnetic field recovers its pre-flare configuration in a short time (i.e., in 30 minutes after the flare).(2) In the photosphere, the line-of-sight velocities show a regular granular up-and down-flow pattern before the flare erupts. During the flare, upflows (blueshifts) dominate the area where the flare is produced. Evaporation rates of ∼ 10 −3 and ∼ 10 −4 g cm −2 s −1 have been derived in the deep and high photosphere, respectively, capable of increasing the chromospheric density by a factor of two in about 400 seconds.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Magnetic and Dynamical Photospheric Disturbances Observed During an M3.2 Solar Flare

Kuckein

Collados

Sainz

2015

ApJ

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“…Zeng et al (2014) have presented high resolution filtergrams of a C-class flare to study the mechanism which leads to He i 1083.0 nm emission. Akimov et al (2014) have described an X1.4 flare as observed with a spectroheliograph in the vicinity of He i 1083.0 nm. Using spectropolarimetry Sasso et al (2011Sasso et al ( , 2014 have covered a C2.0 flare with one spectral scan and focused their analysis on the magnetic structure of an activated filament.…”

Section: Introductionmentioning

confidence: 99%

Full Stokes observations in the He i 1083 nm spectral region covering an M3.2 flare

Kuckein¹,

Collados

Sainz

et al. 2014

Proc. IAU

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Abstract. We present an exceptional data set acquired with the Vacuum Tower Telescope (Tenerife, Spain) covering the pre-flare, flare, and post-flare stages of an M3.2 flare. The full Stokes spectropolarimetric observations were recorded with the Tenerife Infrared Polarimeter in the He i 1083.0 nm spectral region. The object under study was active region NOAA 11748 on 2013 May 17. During the flare the chomospheric He i 1083.0 nm intensity goes strongly into emission. However, the nearby photospheric Si i 1082.7 nm spectral line profile only gets shallower and stays in absorption. Linear polarization (Stokes Q and U ) is detected in all lines of the He i triplet during the flare. Moreover, the circular polarization (Stokes V ) is dominant during the flare, being the blue component of the He i triplet much stronger than the red component, and both are stronger than the Si i Stokes V profile. The Si i inversions reveal enormous changes of the photospheric magnetic field during the flare. Before the flare magnetic field concentrations of up to ∼ 1500 G are inferred. During the flare the magnetic field strength globally decreases and in some cases it is even absent. After the flare the magnetic field recovers its strength and initial configuration.

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Burst-Finder: burst recognition for E-CALLISTO spectra

et al. 2019

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Flare on 2011 September 22 and coronal mass ejection from observations in the He i 10830-Å line

Cited by 4 publications

References 14 publications

Magnetic and Dynamical Photospheric Disturbances Observed During an M3.2 Solar Flare

Magnetic and Dynamical Photospheric Disturbances Observed During an M3.2 Solar Flare

Full Stokes observations in the He i 1083 nm spectral region covering an M3.2 flare

Burst-Finder: burst recognition for E-CALLISTO spectra

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