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Title: ELLERMAN BOMBS WITH JETS: CAUSE AND EFFECT

Abstract

Ellerman Bombs (EBs) are thought to arise as a result of photospheric magnetic reconnection. We use data from the Swedish 1 m Solar Telescope to study EB events on the solar disk and at the limb. Both data sets show that EBs are connected to the foot points of forming chromospheric jets. The limb observations show that a bright structure in the Hα blue wing connects to the EB initially fueling it, leading to the ejection of material upwards. The material moves along a loop structure where a newly formed jet is subsequently observed in the red wing of Hα. In the disk data set, an EB initiates a jet which propagates away from the apparent reconnection site within the EB flame. The EB then splits into two, with associated brightenings in the inter-granular lanes. Micro-jets are then observed, extending to 500 km with a lifetime of a few minutes. Observed velocities of the micro-jets are approximately 5–10 km s{sup −1}, while their chromospheric counterparts range from 50 to 80 km s{sup −1}. MURaM simulations of quiet Sun reconnection show that micro-jets with properties similar to those of the observations follow the line of reconnection in the photosphere, with associatedmore » Hα brightening at the location of increased temperature.« less

Authors:
;  [1]; ;  [2];  [3];  [4]
  1. Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, BT7 1NN, Northern Ireland (United Kingdom)
  2. School of Physics, Trinity College Dublin, Dublin 2 (Ireland)
  3. Armagh Observatory, College Hill, Armagh, BT61 9DG (United Kingdom)
  4. Monash Centre for Astrophysics, School of Mathematical Sciences, Monash University, Clayton, Victoria, 3800 (Australia)
Publication Date:
OSTI Identifier:
22522400
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 805; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; FLAMES; HYDROGEN; JETS; LIFETIME; MAGNETIC FIELDS; MAGNETIC RECONNECTION; MAGNETOHYDRODYNAMICS; PHOTOSPHERE; SUN; TELESCOPES; VELOCITY

Citation Formats

Reid, A., Mathioudakis, M., Scullion, E., Gallagher, P., Doyle, J. G., and Shelyag, S., E-mail: areid29@qub.ac.uk. ELLERMAN BOMBS WITH JETS: CAUSE AND EFFECT. United States: N. p., 2015. Web. doi:10.1088/0004-637X/805/1/64.
Reid, A., Mathioudakis, M., Scullion, E., Gallagher, P., Doyle, J. G., & Shelyag, S., E-mail: areid29@qub.ac.uk. ELLERMAN BOMBS WITH JETS: CAUSE AND EFFECT. United States. doi:10.1088/0004-637X/805/1/64.
Reid, A., Mathioudakis, M., Scullion, E., Gallagher, P., Doyle, J. G., and Shelyag, S., E-mail: areid29@qub.ac.uk. Wed . "ELLERMAN BOMBS WITH JETS: CAUSE AND EFFECT". United States. doi:10.1088/0004-637X/805/1/64.
@article{osti_22522400,
title = {ELLERMAN BOMBS WITH JETS: CAUSE AND EFFECT},
author = {Reid, A. and Mathioudakis, M. and Scullion, E. and Gallagher, P. and Doyle, J. G. and Shelyag, S., E-mail: areid29@qub.ac.uk},
abstractNote = {Ellerman Bombs (EBs) are thought to arise as a result of photospheric magnetic reconnection. We use data from the Swedish 1 m Solar Telescope to study EB events on the solar disk and at the limb. Both data sets show that EBs are connected to the foot points of forming chromospheric jets. The limb observations show that a bright structure in the Hα blue wing connects to the EB initially fueling it, leading to the ejection of material upwards. The material moves along a loop structure where a newly formed jet is subsequently observed in the red wing of Hα. In the disk data set, an EB initiates a jet which propagates away from the apparent reconnection site within the EB flame. The EB then splits into two, with associated brightenings in the inter-granular lanes. Micro-jets are then observed, extending to 500 km with a lifetime of a few minutes. Observed velocities of the micro-jets are approximately 5–10 km s{sup −1}, while their chromospheric counterparts range from 50 to 80 km s{sup −1}. MURaM simulations of quiet Sun reconnection show that micro-jets with properties similar to those of the observations follow the line of reconnection in the photosphere, with associated Hα brightening at the location of increased temperature.},
doi = {10.1088/0004-637X/805/1/64},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 805,
place = {United States},
year = {2015},
month = {5}
}