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

Chen, Yajie; Xu, Zhi; Xiang, Yanjuan; Fang, Yu-Liang; Yang, Zihao

doi:10.1186/s40562-017-0096-1

Cited by 8 publications

(12 citation statements)

References 28 publications

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“…In the absence of Hα observations, the 1700 Å continuum can be used as a proxy for EBs (e.g., Vissers et al 2013;Chen et al 2017;Danilovic et al 2017). We searched for EB signatures in AIA 1700 Å using the EBDETECT 3 code (Vissers et al 2019a).…”

Section: Ellerman Bombs As Sub-canopy Eventsmentioning

confidence: 99%

ALMA observations of transient heating in a solar active region

Santos

Rodríguez

White

et al. 2020

A&A

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Aims. We aim to investigate the temperature enhancements and formation heights of solar active-region brightenings such as Ellerman bombs (EBs), ultraviolet bursts (UVBs), and flaring active-region fibrils (FAFs) using interferometric observations in the millimeter (mm) continuum provided by the Atacama Large Millimeter/submillimeter Array (ALMA). Methods. We examined 3 mm signatures of heating events identified in Solar Dynamics Observatory observations of an active region and compared the results with synthetic spectra from a 3D radiative magnetohydrodynamic simulation. We estimated the contribution from the corona to the mm brightness using differential emission measure analysis. Results. We report the null detection of EBs in the 3 mm continuum at ∼1.2″ spatial resolution, which is evidence that they are sub-canopy events that do not significantly contribute to heating the upper chromosphere. In contrast, we find the active region to be populated with multiple compact, bright, flickering mm-bursts – reminiscent of UVBs. The high brightness temperatures of up to ∼14 200 K in some events have a contribution (up to ∼7%) from the corona. We also detect FAF-like events in the 3 mm continuum. These events show rapid motions of > 10 kK plasma launched with high plane-of-sky velocities (37 − 340 km s−1) from bright kernels. The mm FAFs are the brightest class of warm canopy fibrils that connect magnetic regions of opposite polarities. The simulation confirms that ALMA should be able to detect the mm counterparts of UVBs and small flares and thus provide a complementary diagnostic for localized heating in the solar chromosphere.

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Section: Ellerman Bombs As Sub-canopy Eventsmentioning

confidence: 99%

ALMA observations of transient heating in a solar active region

Santos

Rodríguez

White

et al. 2020

A&A

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“…The enhancement of the FUV continuum is the most striking feature in our EB simulations. Previous observations confirmed that EBs are visible in the FUV continuum at 1600 Å and 1700 Å (Vissers et al 2013;Rezaei & Beck 2015;Tian et al 2016;Chen et al 2017). And it is very promising to detect EBs from these wavebands (Vissers et al 2019a).…”

Section: The Fuv Continuum Enhancement Of Ebsmentioning

confidence: 68%

“…There have been observations of EBs in 1400 Å, 1600 Å, and 1700 Å images (Vissers et al 2015;Tian et al 2016;Chen et al 2017;Ortiz et al 2020), yet we still expect more to statistically check the visibility in all these three FUV bands, with a particular combination of IRIS and AIA observations. The response of the Hα line in UV bursts (Hansteen et al 2017;Ortiz et al 2020) is also an interesting topic for future observations.…”

Section: Discussionmentioning

confidence: 95%

“…Ellerman bombs (EBs) are one of them that were first observed by Ellerman (1917), with typical features of enhanced Hα line wings and an undisturbed line center. Subsequent observations showed that EBs are also visible in many other spectral lines or continua, including the line wings of the Ca II 8542 Å line (Fang et al 2006;Vissers et al 2013;Yang et al 2013), the Ca II H and K lines (Matsumoto et al 2008b;Rezaei & Beck 2015), the He I D 3 and 10830 Å lines (Libbrecht et al 2017), and the Mg II triplet lines (Vissers et al 2015;Hansteen et al 2017;Hong et al 2017a), as well as the G band (Herlender & Berlicki 2011;Nelson et al 2013b) and ultraviolet continua at 1600 Å and 1700 Å (Vissers et al 2013;Rezaei & Beck 2015;Tian et al 2016;Chen et al 2017). Yet jiehong@nju.edu.cn EBs are invisible in neutral metal lines (Rutten et al 2015) and coronal lines (Vissers et al 2013;Tian et al 2016).…”

Section: Introductionmentioning

confidence: 98%

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Revisiting the Spectral Features of Ellerman Bombs and UV Bursts. I. Radiative Hydrodynamic Simulations

Hong,

Li,

Ding

et al. 2021

Preprint

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Ellerman bombs (EBs) and UV bursts are both small-scale solar activities that occur in active regions. They are now believed to form at different heights in the lower atmosphere. In this paper, we use one-dimensional radiative hydrodynamic simulations to calculate various line profiles in response to heating in different atmospheric layers. We confirm that heating in the upper photosphere to the lower chromosphere can generate spectral features of typical EBs, while heating in the mid to upper chromosphere can generate spectral features of typical UV bursts. The intensity evolution of the Hα line wing in EBs shows a rise-plateau pattern, while that of the Si IV 1403 Å line center in UV bursts shows a rise-fall pattern. However, the predicted enhancement of FUV continuum near 1400 Å for EBs is rarely reported and requires further observations to check it. With two heating sources or an extended heating source in the atmosphere, both EB and UV burst features could be reproduced simultaneously.

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“…Chen et al(2017) [85] have carried out a statistical study on the visibility of EBs in the AIA 1700 Å images by using NVST Hα core and off-band images. There are 145 EBs that were identified from Hα wing images, in which 74 EBs (about 51%) can be clearly identified as bright points (BPs) in the AIA 1700 Å images.…”

Section: Ellerman Bombsmentioning

confidence: 99%

Research progress based on observations of the New Vacuum Solar Telescope

Yan

Liu

Zhang

et al. 2019

Preprint

Self Cite

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The purpose of this paper is to introduce the main scientific results made by the one-meter New Vacuum Solar Telescope (NVST), which was put into commission on 2010. NVST is one of the large aperture solar telescopes in the world, located on the shore of Fuxian lake of Yunnan province in China, aiming at serving solar physicists by providing them with high resolution photospheric and chromospheric observational data. Based on the data from NVST and complementary observations from space (e.g., Hinode, SDO and IRIS, etc), dozens of scientific papers have been published with a wide range of topics concentrating mainly on dynamics and activities of fine-scale magnetic structures and their roles in the eruptions of active-region filaments and flares. The achievements include dynamic characteristics of photospheric bright points, umbral dots, penumbral waves, and sunspot/light bridge oscillation, observational evidence of small-scale magnetic reconnection, and fine-scale dynamic structure of prominences. All these new results will shed light on the better understanding of solar eruptive activities. Data release, observation proposals, and future research subjects are introduced and discussed.

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

Cited by 8 publications

References 28 publications

ALMA observations of transient heating in a solar active region

ALMA observations of transient heating in a solar active region

Revisiting the Spectral Features of Ellerman Bombs and UV Bursts. I. Radiative Hydrodynamic Simulations

Research progress based on observations of the New Vacuum Solar Telescope

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