Solar Ellerman Bombs in 1D Radiative Hydrodynamics

Reid, Aaron; Mathioudakis, M.; Kowalski, Adam F.; Doyle, J. G.; Allred, Joel C.

doi:10.3847/2041-8213/835/2/l37

Cited by 29 publications

(36 citation statements)

References 38 publications

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“…Reid et al (2017) first calculated the line profiles of EBs using a thermal model, with results similar to observations. However, as EBs are believed to be caused by magnetic reconnection, the non-thermal effects by electrons, which they did not take into consideration, might be important.…”

Section: Introductionmentioning

confidence: 88%

“…The Mg II k line profiles are computed using the RH code (Uitenbroek 2001;Pereira & Uitenbroek 2015), and the integrated intensity of the Si IV 1403 Å line over wavelength is calculated using the CHIANTI atomic database (Del Zanna et al 2015). One can see that, similar to Reid et al (2017), the outer wings of the Mg II k line are enhanced, while there is very little influence on the k 2 peaks. The light curve of the Si IV integrated intensity shows very little fluctuation, which is atypical in UV bursts.…”

Section: Comparison Between Simulations and Observationsmentioning

confidence: 99%

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RADYN Simulations of Non-thermal and Thermal Models of Ellerman Bombs

Hong

Carlsson

Ding

2017

ApJ

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Ellerman bombs (EBs) are brightenings in the Hα line wings that are believed to be caused by magnetic reconnection in the lower atmosphere. To study the response and evolution of the chromospheric line profiles, we perform radiative hydrodynamic simulations of EBs using both non-thermal and thermal models. Overall, these models can generate line profiles that are similar to observations. However, in non-thermal models we find dimming in the Hα line wings and continuum when the heating begins, while for the thermal models dimming occurs only in the Hα line core, and with a longer lifetime. This difference in line profiles can be used to determine whether an EB is dominated by non-thermal heating or thermal heating. In our simulations, if a higher heating rate is applied, then the Hα line will be unrealistically strong and there are still no clear UV burst signatures.

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Section: Introductionmentioning

confidence: 88%

Section: Comparison Between Simulations and Observationsmentioning

confidence: 99%

RADYN Simulations of Non-thermal and Thermal Models of Ellerman Bombs

Hong

Carlsson

Ding

2017

ApJ

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“…Due to the contribution function of Ca II 8542Å encompassing a broad range of heights along the photosphere and chromosphere (Cauzzi et al 2008;Reid et al 2017), some stratification with height would also be necessary in order to fully utilize the observations. The input observations were optimized in order to accumulate a sufficient signal in Stokes-Q, -U, and -V. The area within the red box of Figure 1 was used for the inversions and was spatially binned 2 × 2.…”

Section: Nicole Inversionsmentioning

confidence: 99%

“…Bi-directional flows have also been reported in EBs, with the upflows showing a higher velocity than the downflows at EB locations, with values much lower than that of micro-flares (±5 km s −1 ; Isobe et al 2007;Matsumoto et al 2008;Archontis & Hood 2009;Reid et al 2017).…”

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confidence: 99%

Chromospheric Inversions of a Micro-flaring Region

Reid

Henriques

Mathioudakis

et al. 2017

ApJ

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We use spectropolarimetric observations of the Ca II 8542Å line, taken from the Swedish 1 m Solar Telescope, in an attempt to recover dynamic activity in a micro-flaring region near a sunspot via inversions. These inversions show localized mean temperature enhancements of ∼1000K in the chromosphere and upper photosphere, along with co-spatial bi-directional Doppler shifting of 5-10 km s −1 . This heating also extends along a nearby chromospheric fibril, which is co-spatial to 10-15 km s −1 downflows. Strong magnetic flux cancellation is also apparent in one of the footpoints, and is concentrated in the chromosphere. This event more closely resembles that of an Ellerman Bomb, though placed slightly higher in the atmosphere than what is typically observed.

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“…More recently, it has also been found that some EBs correspond to small-scale compact brightenings in the 1700 Å images taken by the Atmospheric Imaging Assembly (AIA, Lemen et al 2012) onboard the solar dynamics observatory (SDO) (Vissers et al 2013;Tian et al 2016;Zhao et al 2017;Toriumi et al 2017 Peter et al 2014;Vissers et al 2015;Cho et al 2015;Tian et al 2016;Grubecka et al 2016). However, it is still under debate whether such intense heating is directly caused by the EBs or not (e.g., Lei et al 2016;Reid et al 2017;Berlicki and Heinzel 2014;Fang et al 2017;Hong et al 2017;Danilovic 2017;Hansteen et al 2017). …”

Section: Introductionmentioning

confidence: 99%

Ellerman bombs observed with the new vacuum solar telescope and the atmospheric imaging assembly onboard the solar dynamics observatory

Chen

Xiang

et al. 2017

Geosci. Lett.

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Ellerman bombs (EBs) are believed to be small-scale reconnection events occurring around the temperature minimum region in the solar atmosphere. They are often identified as significant enhancements in the extended Hα wings without obvious signatures in the Hα core. Here we explore the possibility of using the 1700 Å images taken by the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) to study EBs. From the Hα wing images obtained with the New Vacuum Solar Telescope (NVST) on 2015 May 2, we have identified 145 EBs and 51% of them clearly correspond to the bright points (BPs) in the AIA 1700 Å images. If we resize the NVST images using a linear interpolation to make the pixel sizes of the AIA and NVST images the same, some previously identified EBs disappear and about 71% of the remaining EBs are associated with BPs. Meanwhile, 66% of the compact brightenings in the AIA 1700 Å images can be identified as EBs in the Hα wings. The intensity enhancements of the EBs in the Hα wing images reveal a linear correlation with those of the BPs in the AIA 1700 Å images. Our study suggests that a significant fraction of EBs can be observed with the AIA 1700 Å filter, which is promising for large-sample statistical study of EBs as the seeing-free and full-disk SDO/AIA data are routinely available.

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Solar Ellerman Bombs in 1D Radiative Hydrodynamics

Cited by 29 publications

References 38 publications

RADYN Simulations of Non-thermal and Thermal Models of Ellerman Bombs

RADYN Simulations of Non-thermal and Thermal Models of Ellerman Bombs

Chromospheric Inversions of a Micro-flaring Region

Ellerman bombs observed with the new vacuum solar telescope and the atmospheric imaging assembly onboard the solar dynamics observatory

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