Observational Evidence of Magnetic Reconnection for Brightenings and Transition Region Arcades in IRIS Observations

Zhao, Jie; Schmieder, B.; Li, Hui; Pariat, É.; Zhu, Xiaoshuai; Li, Feng; Grubecka, M.

doi:10.3847/1538-4357/836/1/52

Cited by 45 publications

(51 citation statements)

References 94 publications

(109 reference statements)

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“…Dynamical events, such as chromospheric jets (e.g., Liu et al 2009;Morton 2012;Bharti et al 2013;Tian et al 2014), Ellerman Bombs (e.g., Fang et al 2006;Hong et al 2014;Nelson et al 2015) and type II white light flares (e.g., Ding et al 1994Ding et al , 1999, are all related to magnetic reconnection in the partially ionized low atmosphere. Improvements in the angular resolution of solar telescopes have allowed many small scale magnetic reconnection events in the low solar atmosphere to be observed (e.g., Yang et al 2015;Xue et al 2016;Zhao et al 2017). The high temperature compact bright points which have UV counterparts that are frequently observed with the Interface Region Imaging Spectrograph (IRIS) (Peter et al 2014;Vissers et al 2015;Grubecka et al 2016;Tian et al 2016) are known as IRIS bombs.…”

Section: Introductionmentioning

confidence: 99%

Magnetic Reconnection in Strongly Magnetized Regions of the Low Solar Chromosphere

Lukin

Murphy

et al. 2018

ApJ

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Magnetic reconnection in strongly magnetized regions around the temperature minimum region of the low solar atmosphere is studied by employing MHD-based simulations of a partially ionized plasma within a reactive 2.5D multi-fluid model. It is shown that in the absence of magnetic nulls in a low β plasma the ionized and neutral fluid flows are well-coupled throughout the reconnection region. However, non-equilibrium ionization-recombination dynamics play a critical role in determining the structure of the reconnection region, lead to much lower temperature increases and a faster magnetic reconnection rate as compared to simulations that assume plasma to be in ionization-recombination equilibrium. The rate of ionization of the neutral component of the plasma is always faster than recombination within the current sheet region even when the initial plasma β is as high as β 0 = 1.46. When the reconnecting magnetic field is in excess of a kilogauss and the plasma β is lower than 0.0145, the initially weakly ionized plasmas can become fully ionized within the reconnection region and the current sheet can be strongly heated to above 2.5 × 10 4 K, even as most of the collisionally dissipated magnetic energy is radiated away. The Hall effect increases the reconnection rate slightly, but in the absence of magnetic nulls it does not result in significant asymmetries or change the characteristics of the reconnection current sheet down to meter scales.

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Section: Introductionmentioning

confidence: 99%

Magnetic Reconnection in Strongly Magnetized Regions of the Low Solar Chromosphere

Lukin

Murphy

et al. 2018

ApJ

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“…Qiu et al (2000) first noticed that some EBs have signatures in the 1600 Å images obtained with the transition region and coronal explorer (TRACE, Handy et al 1999). 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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“…A recent study by Zhao et al (2016) suggests that these waves can propagate further up into the corona.…”

Section: Dynamics In the Tr Above Sunspotsmentioning

confidence: 99%

The transition region above sunspots

Samanta

Zhang

2018

Geosci. Lett.

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Over decades, sunspots and their fine structures have been studied in detail at the photospheric level with different ground-based telescopes, as the surface of the Sun primarily emits light in the visible wavelengths. For a very long period, the upper atmosphere above the sunspot regions, especially the transition region (TR) above sunspots where the plasma emits light in the far ultraviolet (FUV) and extreme ultraviolet (EUV), has been poorly understood. In the past decades after the development of space instrumentations, FUV and EUV observations have uncovered many secrets of the TR above sunspots. In this paper, we present a brief review of research results about the TR structures and dynamics obtained through imaging and spectroscopic observations of sunspots in the past ~ 20 years. Though these observations have gathered remarkable and detailed information and greatly improved our understanding of the TR above the sunspots, paradoxically, they leave us with many new questions which should be answered in the future.

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Observational Evidence of Magnetic Reconnection for Brightenings and Transition Region Arcades in IRIS Observations

Cited by 45 publications

References 94 publications

Magnetic Reconnection in Strongly Magnetized Regions of the Low Solar Chromosphere

Magnetic Reconnection in Strongly Magnetized Regions of the Low Solar Chromosphere

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

The transition region above sunspots

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