Precise timing of solar flare footpoint sources from mid-infrared observations

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dc.contributor.authorSimoes P.J.A.
dc.contributor.authorFletcher L.
dc.contributor.authorHudson H.S.
dc.contributor.authorKerr G.S.
dc.contributor.authorPenn M.
dc.contributor.authorLopez K.F.
dc.date.accessioned2024-08-01T06:16:36Z
dc.date.available2024-08-01T06:16:36Z
dc.date.issued2024
dc.description.abstract© 2024 The Author(s)Solar flares are powerful particle accelerators, and in the accepted standard flare model most of the flare energy is transported from a coronal energy-release region by accelerated electrons that stop collisionally in the chromosphere, heating and ionizing the plasma, producing a broad-band enhancement to the solar radiative output. We present a time-delay analysis of the infrared (IR) emission from two chromospheric sources in the flare SOL2014-09-24T17:50 taken at the McMath–Pierce telescope. By cross-correlating the intensity signals, measured with 1 s cadence, from the two spatially resolved IR sources we find a delay of 0.75 ± 0.07 s at 8.2 μm, where the uncertainties are quantified by a Monte Carlo analysis. The sources correlate well in brightness but have a time lag larger than can be reasonably explained by the energy transport dominated by non-thermal electrons precipitating from a single acceleration site in the corona. If interpreted as a time-of-flight difference between electrons travelling to each footpoint, we estimate time delays between 0.14 and 0.42 s, for a reconnection site at the interior quasi-separatrix layer, or at the null-point of the spine-fan topology inferred for this event. We employed modelling of electron transport via time-dependent Fokker–Planck and radiative hydrodynamic simulations to evaluate other possible sources of time-delay in the generation of the IR emission, such as differing ionization time-scales under different chromospheric conditions. Our results demonstrate that they are also unable to account for this discrepancy. This flare appears to require energy transport by some means other than electron beams originating in the corona.
dc.description.firstpage705
dc.description.issuenumber1
dc.description.lastpage718
dc.description.volume532
dc.identifier.doi10.1093/mnras/stae1511
dc.identifier.issnNone
dc.identifier.urihttps://dspace.mackenzie.br/handle/10899/39039
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsAcesso Aberto
dc.subject.otherlanguagemethods: data analysis
dc.subject.otherlanguageradiation: dynamics
dc.subject.otherlanguageSun: activity
dc.subject.otherlanguageSun: chromosphere
dc.subject.otherlanguageSun: flares
dc.titlePrecise timing of solar flare footpoint sources from mid-infrared observations
dc.typeArtigo
local.scopus.citations0
local.scopus.eid2-s2.0-85197262378
local.scopus.subjectEnergy-transport
local.scopus.subjectInfrared emissions
local.scopus.subjectMethods. Data analysis
local.scopus.subjectMidinfrared
local.scopus.subjectRadiation dynamics
local.scopus.subjectSolar flare
local.scopus.subjectSun: activity
local.scopus.subjectSun: Chromosphere
local.scopus.subjectSun:flares
local.scopus.subjectTime-delays
local.scopus.updated2024-09-01
local.scopus.urlhttps://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85197262378&origin=inward
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