Statistical Analysis of Small Ellerman Bomb Events

Nelson, C. J.; Doyle, J. G.; Erdélyi, R.; Huang, Zhaoqin; Madjarska, M. S.; Mathioudakis, M.; Mumford, Stuart; Reardon, K.

doi:10.1007/s11207-012-0222-3

Cited by 48 publications

(52 citation statements)

References 29 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…A skeleton version of this code was adapted to test its functionality in comparison with other existing codes. This resulted in finding a similar amount of EB detections arcsec −2 s −1 as in previous studies (Nelson et al 2013a;Vissers et al 2013). Using the co-aligned spectropolarimetric data from the SST, it was shown that the code produced a higher proportion of strong, bipolar detections when an impulsive criterion was applied.…”

Section: Discussionsupporting

confidence: 75%

“…The quiet-Sun profile was taken over an area of 200 pixels 2 (11.84″ 2 ), centered about the position X = 43 216, Y = 20 128, seen in the red box of Figure 1. The intensity threshold for the grown area is the same as that of Nelson et al (2013a). The size criterion was added to ensure that no small-scale anomalies were picked up as detections.…”

Section: Eb Detection and Trackingmentioning

confidence: 99%

“…Adapting our algorithm to match their criteria yields 3294 detections, most of which are extremely short-lived, small-scale, low-intensity brightenings. Nelson et al (2013a) . The 130 detections is fairly similar to the 116 detected using the criteria adopted in this work.…”

Section: Eb Detection and Trackingmentioning

confidence: 99%

“…The statistical study of Nelson et al (2013a) applied a similar method to the results of an automated detection algorithm for EBs and found a lower total radiative energy of 10 22 -10 25 erg, with peak radiative loss rates of 10 21 -10 23 erg s −1 . In this paper, we use high spatial and temporal resolution Hα imaging spectroscopy along with Fe I 6302.5 Å imaging spectropolarimetry from the Swedish 1 m Solar Telescope (SST) to study EBs and their associated flux cancellation rates.…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Magnetic Flux Cancellation in Ellerman Bombs

Reid

Mathioudakis

Doyle

et al. 2016

ApJ

Self Cite

View full text Add to dashboard Cite

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.

show abstract

Section: Discussionsupporting

confidence: 75%

Section: Eb Detection and Trackingmentioning

confidence: 99%

Section: Eb Detection and Trackingmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Magnetic Flux Cancellation in Ellerman Bombs

Reid

Mathioudakis

Doyle

et al. 2016

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…Georgoulis et al( 2002) obtained a higher energy of EBs to be 3×10 28 ergs. However, using a similar value of the net radiative loss rate and taking the height of a EB to be 100 km, Nelson et al ( 2013) estimated the EB energies being in the range of 2 × 10 22 -4 ×10 25 ergs, which is three to four orders of magnitude lower than that in Georgoulis et al( 2002). To elucidate the physical mechanism of EBs, spectral data with high spatial and temporal resolutions are imperative.…”

Section: Introductionmentioning

confidence: 99%

Diagnostics of Ellerman bombs with high-resolution spectral data

Fang

Guo

et al. 2015

Res. Astron. Astrophys.

View full text Add to dashboard Cite

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.

show abstract

Magnetic Flux Emergence Along the Solar Cycle

Schmieder

Archontis

Pariat

2015

Space Sciences Series of ISSI

View full text Add to dashboard Cite

Flux emergence plays an important role along the solar cycle. Magnetic flux emergence builds sunspot groups and solar activity. The sunspot groups contribute to the large scale behaviour of the magnetic field over the 11 year cycle and the reversal of the North and South magnetic polarity every 22 years. The leading polarity of sunspot groups is opposite in the North and South hemispheres and reverses for each new solar cycle. However the hemispheric rule shows the conservation of sign of the magnetic helicity with positive and negative magnetic helicity in the South and North hemispheres, respectively. MHD models of emerging flux have been developed over the past twenty years but have not yet succeeded to reproduce solar observations. The emergence of flux occurs through plasma layers of very high gradients of pressure and changing of modes from a large β to a low β plasma (<1). With the new armada of high spatial and temporal resolution instruments on the ground and in space, emergence of magnetic flux is observed in tremendous detail and followed during their transit through the upper atmosphere. Signatures of flux emergence in the corona depend on the pre-existing magnetic configuration and on the strength of the emerging flux. We review in this paper new and established models as well as the recent observations.

show abstract

Statistical Analysis of Small Ellerman Bomb Events

Cited by 48 publications

References 29 publications

Magnetic Flux Cancellation in Ellerman Bombs

Magnetic Flux Cancellation in Ellerman Bombs

Diagnostics of Ellerman bombs with high-resolution spectral data

Magnetic Flux Emergence Along the Solar Cycle

Contact Info

Product

Resources

About