Solar Ellerman Bombs in 1D Radiative Hydrodynamics

A. Reid; M. Mathioudakis; A. Kowalski; J. G. Doyle; J. C. Allred

doi:10.3847/2041-8213/835/2/L37

Solar Ellerman Bombs in 1D Radiative Hydrodynamics

A. Reid, M. Mathioudakis, A. Kowalski, J. G. Doyle, J. C. Allred

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Abstract

Recent observations from the Interface Region Imaging Spectrograph (IRIS) appear to show impulsive brightenings in high temperature lines, which when combined with simultaneous ground based observations in Hα, appear co-spatial to Ellerman Bombs (EBs). We use the RADYN 1-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 A, and Mg II h & 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 A, and Mg II h & k, we cannot achieve agreement with all of these simultaneously.

Original language	English
Journal	The Astrophysical Journal. Letters
Volume	835
Issue number	L37
DOIs	https://doi.org/10.3847/2041-8213/835/2/L37
Publication status	Published - 02 Feb 2017

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Solar Ellerman Bombs in 1D Radiative Hydrodynamics
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title = "Solar Ellerman Bombs in 1D Radiative Hydrodynamics",

abstract = "Recent observations from the Interface Region Imaging Spectrograph (IRIS) appear to show impulsive brightenings in high temperature lines, which when combined with simultaneous ground based observations in Hα, appear co-spatial to Ellerman Bombs (EBs). We use the RADYN 1-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 A, and Mg II h & 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 A, and Mg II h & k, we cannot achieve agreement with all of these simultaneously.",

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T1 - Solar Ellerman Bombs in 1D Radiative Hydrodynamics

AU - Reid, A.

AU - Mathioudakis, M.

AU - Kowalski, A.

AU - Doyle, J. G.

AU - Allred, J. C.

PY - 2017/2/2

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N2 - Recent observations from the Interface Region Imaging Spectrograph (IRIS) appear to show impulsive brightenings in high temperature lines, which when combined with simultaneous ground based observations in Hα, appear co-spatial to Ellerman Bombs (EBs). We use the RADYN 1-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 A, and Mg II h & 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 A, and Mg II h & k, we cannot achieve agreement with all of these simultaneously.

AB - Recent observations from the Interface Region Imaging Spectrograph (IRIS) appear to show impulsive brightenings in high temperature lines, which when combined with simultaneous ground based observations in Hα, appear co-spatial to Ellerman Bombs (EBs). We use the RADYN 1-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 A, and Mg II h & 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 A, and Mg II h & k, we cannot achieve agreement with all of these simultaneously.

U2 - 10.3847/2041-8213/835/2/L37

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