Spectropolarimetric investigation of an Ellerman bomb: 1. Observations

Kondrashova, N.

doi:10.3103/s0884591316010050

Cited by 8 publications

(2 citation statements)

References 22 publications

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“…Isobe, Tripathi, and Archontis, 2007;Archontis and Hood, 2009). Detailed modeling of expected DKIST spectropolarimetric measurements in the photosphere and chromosphere will enable careful comparisons between the simulated and observed plasma flows and magnetic-field evolution at the Ellerman-bomb sites (Socas-Navarro et al, 2006;Kondrashova, 2016) to determine if the existence of such large-scale structures is implicated by observations of the Sun. Additionally, direct detection of the brightness temperature excess at Ellerman-bomb sites and in the surrounding atmosphere will be possible with coordinated observations using DKIST and radio instruments such as the ALMA.…”

Section: Flux Emergence Into the Non-eruptive Solar Atmospherementioning

confidence: 99%

Critical Science Plan for the Daniel K. Inouye Solar Telescope (DKIST)

Rast¹,

González²,

Rubio³

et al. 2021

Sol Phys

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The National Science Foundation’s Daniel K. Inouye Solar Telescope (DKIST) will revolutionize our ability to measure, understand, and model the basic physical processes that control the structure and dynamics of the Sun and its atmosphere. The first-light DKIST images, released publicly on 29 January 2020, only hint at the extraordinary capabilities that will accompany full commissioning of the five facility instruments. With this Critical Science Plan (CSP) we attempt to anticipate some of what those capabilities will enable, providing a snapshot of some of the scientific pursuits that the DKIST hopes to engage as start-of-operations nears. The work builds on the combined contributions of the DKIST Science Working Group (SWG) and CSP Community members, who generously shared their experiences, plans, knowledge, and dreams. Discussion is primarily focused on those issues to which DKIST will uniquely contribute.

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Section: Flux Emergence Into the Non-eruptive Solar Atmospherementioning

confidence: 99%

Critical Science Plan for the Daniel K. Inouye Solar Telescope (DKIST)

Rast¹,

González²,

Rubio³

et al. 2021

Sol Phys

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“…Most of these spectral lines are low-temperature lines, suggesting that EBs are small, low-temperature solar activities. Several studies based on the inversion of the radiative properties of the Hα and Ca II lines using semi-empirical or two-cloud models further indicate that the EBs are usually located in the upper photosphere or the low chromosphere, and the temperature in EBs should be 600-3000 K higher than its surroundings (e.g., Fang et al 2006;Berlicki & Heinzel 2014;Hong et al 2014;Kondrashova 2016). EBs are more likely to occur in active regions near magnetic-field polarity inversion lines, and are accompanied by magnetic flux cancellation, suggesting that their formation is due to magnetic reconnection (Matsumoto et al 2008;Nelson et al 2013;Peter et al 2014;Reid et al 2016;Tian et al 2016;Shen et al 2022).…”

Section: Introductionmentioning

confidence: 99%

A magnetic reconnection model for the hot explosion with both ultraviolet and Hα wing emissions

Cheng,

Ni,

Chen

et al. 2024

A&A

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Ellerman bombs (EBs) with significant Halpha wing emissions and ultraviolet bursts (UV bursts) with strong Si IV emissions are two kinds of small transient brightening events that occur in the low solar atmosphere. The statistical observational results indicate that about 20<!PCT!> of the UV bursts connect with EBs. While some promising models exist for the formation mechanism of colder EBs in conjunction with UV bursts, the topic remains an area of ongoing research and investigation. We numerically investigated the magnetic reconnection process between the emerging arch magnetic field and the lower atmospheric background magnetic field. We aim to find out if the hot UV emissions and much colder Halpha wing emissions can both appear in the same reconnection process and how they are located in the reconnection region. The open-source code NIRVANA was applied to perform the 2.5D magnetohydrodynamic (MHD) simulation. We developed the related sub-codes to include the more realistic radiative cooling process for the photosphere and chromosphere and the time-dependent ionization degree of hydrogen. The initial background magnetic field is 600 G, and the emerged magnetic field in the solar atmosphere is of the same magnitude, meaning that it results in a low- beta magnetic reconnection environment. We also used the radiative transfer code RH1.5D to synthesize the Si IV and Halpha spectral line profiles based on the MHD simulation results. Magnetic reconnection between emerged and background magnetic fields creates a thin, curved current sheet, which then leads to the formation of plasmoid instability and the nonuniform density distributions. Initially, the temperature is below 8,000 K. As the current sheet becomes more vertical, denser plasmas are drained by gravity, and hotter plasmas above 20,000 K appear in regions with lower plasma density. The mix of hot tenuous and much cooler dense plasmas in the turbulent reconnection region can appear at about the same height, or even in the same plasmoid. Through the reconnection region, the synthesized Si IV emission intensity can reach above 10$^6$ erg s$^ $ sr$^ $ cm$^ $ and the spectral line profile can be wider than 100 km s$^ $, the synthesized Halpha line profile also show the similar characteristics of a typical EB. The turbulent current sheet is always in a dense plasma environment with an optical depth larger than 6.5times 10$^ $ due to the emerged magnetic field pushing high-density plasmas upward. Our simulation results indicate that the cold EB and hot UV burst can both appear in the same reconnection process in the low chromosphere, the EB can either appear several minutes earlier than the UV burst, or they can simultaneously appear at the similar altitude in a turbulent reconnection region below the middle chromosphere.

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Spectral study of Ellerman bombs. The photosphere

Pasechnik¹

2018

Kinemat. fiz. nebesnyh tel (Online)

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Spectropolarimetric investigation of an Ellerman bomb: 1. Observations

Cited by 8 publications

References 22 publications

Critical Science Plan for the Daniel K. Inouye Solar Telescope (DKIST)

Critical Science Plan for the Daniel K. Inouye Solar Telescope (DKIST)

A magnetic reconnection model for the hot explosion with both ultraviolet and Hα wing emissions

Spectral study of Ellerman bombs. The photosphere

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