Velocities and Temperatures of an Ellerman Bomb and Its Associated Features

Yang, Heesu; Chae, Jongchul; Lim, Eun-Kyung; Park, Hyungmin; Cho, Kyuhyoun; Maurya, Ram Ajor; Song, Donguk; Kim, Yeon Han; Goode, Philip R.

doi:10.1007/s11207-013-0354-0

Cited by 40 publications

(56 citation statements)

References 26 publications

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“…These temperature enhancements lead to intensity enhancements in the wings of the Hα and Ca II 8542 Å lines. Other EB studies also find similar temperature enhancements (200-3000 K) in the photosphere/temperature minimum region (Georgoulis et al 2002;Isobe et al 2007;Yang et al 2013;Hong et al 2014;Li et al 2015).…”

Section: Introductionsupporting

confidence: 60%

Solar Ellerman Bombs in 1D Radiative Hydrodynamics

Reid

Mathioudakis

Kowalski

et al. 2017

ApJL

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Recent observations from the Interface Region Imaging Spectrograph appear to show impulsive brightenings in high temperature lines, which when combined with simultaneous ground-based observations in Hα, appear cospatial to Ellerman Bombs (EBs). We use the RADYN one-dimensional radiative transfer code in an attempt to try and reproduce the observed line profiles and simulate the atmospheric conditions of these events. Combined with the MULTI/RH line synthesis codes, we compute the Hα, Ca II 8542 Å, and Mg II h and k lines for these simulated events and compare them to previous observations. Our findings hint that the presence of superheated regions in the photosphere (>10,000 K) is not a plausible explanation for the production of EB signatures. While we are able to recreate EB-like line profiles in Hα, Ca II 8542 Å, and Mg II h and k, we cannot achieve agreement with all of these simultaneously.

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Section: Introductionsupporting

confidence: 60%

Solar Ellerman Bombs in 1D Radiative Hydrodynamics

Reid

Mathioudakis

Kowalski

et al. 2017

ApJL

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“…These temperature enhancements lead to intensity enhancements in the wings of the Hα and Ca II 8542 Å lines, while the line cores are formed higher in the chromosphere. Other studies of EBs also find similar temperature enhancements ranging from 200 to 3000 K in the photosphere/temperature minimum region (Georgoulis et al 2002;Isobe et al 2007;Yang et al 2013;Hong et al 2014;Li et al 2015).…”

Section: Introductionsupporting

confidence: 59%

Magnetic Flux Cancellation in Ellerman Bombs

Reid

Mathioudakis

Doyle

et al. 2016

ApJ

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Ellerman Bombs (EBs) are often found to be co-spatial with bipolar photospheric magnetic fields. We use Hα imaging spectroscopy along with Fe I 6302.5 Å spectropolarimetry from the Swedish 1 m Solar Telescope (SST), combined with data from the Solar Dynamic Observatory, to study EBs and the evolution of the local magnetic fields at EB locations. EBs are found via an EB detection and tracking algorithm. Using NICOLE inversions of the spectropolarimetric data, we find that, on average, (3.43 ± 0.49) × 10 24 erg of stored magnetic energy disappears from the bipolar region during EB burning. The inversions also show flux cancellation rates of 10 14 -10 15 Mx sand temperature enhancements of 200 K at the detection footpoints. We investigate the near-simultaneous flaring of EBs due to co-temporal flux emergence from a sunspot, which shows a decrease in transverse velocity when interacting with an existing, stationary area of opposite polarity magnetic flux, resulting in the formation of the EBs. We also show that these EBs can be fueled further by additional, faster moving, negative magnetic flux regions.

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“…Georgoulis et al( 2002) used high-resolution chromospheric Hα filtergrams and found that the temperature enhancement of EBs is ∼ 2 × 10 3 K. Furthermore, using high-resolution Hα images, Berlicki et al( 2010) found that the temperature increase could be as high as 3000 K. Mass motion is another feature associated with EBs. It was found that some EBs have an upward motion with a velocity of several km s −1 (Kurokawa et al 1982;Dara et al 1997;Yang et al 2013). Some observations of EBs at the solar limb also found up-flows (Kurokawa et al 1982;Nelson et al 2015).…”

Section: Introductionmentioning

confidence: 98%

Diagnostics of Ellerman bombs with high-resolution spectral data

Fang

Guo

et al. 2015

Res. Astron. Astrophys.

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Ellerman bombs (EBs) are tiny brightenings often observed near sunspots. The most impressive characteristic of the EB spectra is the two emission bumps in both wings of the Hα and Ca II 8542Å lines. High-resolution spectral data of three small EBs were obtained on 2013 June 6 with the largest solar telescope, the 1.6 meter New Solar Telescope (NST), at the Big Bear Solar Observatory. The characteristics of these EBs are analyzed. The sizes of the EBs are in the range of 0.3 ′′ -0.8 ′′ and their durations are only 3-5 minutes. Our semi-empirical atmospheric models indicate that the heating occurs around the temperature minimum region with a temperature increase of 2700-3000 K, which is surprisingly higher than previously thought. The radiative and kinetic energies are estimated to be as high as 5×10 25 -3.0×10 26 ergs despite the small size of these EBs. Observations of the magnetic field show that the EBs appeared just in a parasitic region with mixed polarities and accompanied by mass motions. Nonlinear force-free field extrapolation reveals that the three EBs are connected with a series of magnetic field lines associated with bald patches, which strongly implies that these EBs should be produced by magnetic reconnection in the solar lower atmosphere. According to the lightcurves and the estimated magnetic reconnection rate, we propose that there is a three phase process in EBs: pre-heating, flaring and cooling phases.

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Velocities and Temperatures of an Ellerman Bomb and Its Associated Features

Cited by 40 publications

References 26 publications

Solar Ellerman Bombs in 1D Radiative Hydrodynamics

Solar Ellerman Bombs in 1D Radiative Hydrodynamics

Magnetic Flux Cancellation in Ellerman Bombs

Diagnostics of Ellerman bombs with high-resolution spectral data

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