Aaron Reid

Aaron Reid

Queen's University Belfast

H-index: 13

Europe-United Kingdom

About Aaron Reid

Aaron Reid, With an exceptional h-index of 13 and a recent h-index of 11 (since 2020), a distinguished researcher at Queen's University Belfast, specializes in the field of Solar Physics, Astronomy, Magnetic Reconnection.

His recent articles reflect a diverse array of research interests and contributions to the field:

The F-CHROMA grid of 1D RADYN flare models

Flare-induced photospheric velocity diagnostics

Critical Science Plan for the Daniel K. Inouye Solar Telescope (DKIST)

Flare-induced Sunquake Signatures in the Ultraviolet as Observed by the Atmospheric Imaging Assembly

Non-LTE inversions of a confined X2. 2 flare-I. The vector magnetic field in the photosphere and chromosphere

Constraining the magnetic vector in the quiet solar photosphere and the impact of instrumental degradation

Temporal evolution of small-scale internetwork magnetic fields in the solar photosphere (Corrigendum)

Chromospheric Bubbles in Solar Flares

Aaron Reid Information

University

Queen's University Belfast

Position

PDRA @

Citations(all)

561

Citations(since 2020)

385

Cited By

316

hIndex(all)

13

hIndex(since 2020)

11

i10Index(all)

14

i10Index(since 2020)

12

Email

University Profile Page

Queen's University Belfast

Aaron Reid Skills & Research Interests

Solar Physics

Astronomy

Magnetic Reconnection

Top articles of Aaron Reid

The F-CHROMA grid of 1D RADYN flare models

Authors

Mats Carlsson,Lyndsay Fletcher,Joel Allred,Petr Heinzel,Jana Kašparová,Adam Kowalski,Mihalis Mathioudakis,Aaron Reid,Paulo JA Simões

Journal

Astronomy & Astrophysics

Published Date

2023/5/1

Context. Solar flares are the result of the sudden release of magnetic energy in the corona. Much of this energy goes into accelerating charged particles to high velocity. These particles travel along the magnetic field and the energy is dissipated when the density gets high enough, primarily in the solar chromosphere. Modelling this region is difficult because the radiation energy balance is dominated by strong, optically thick spectral lines.Aims. Our aim is to provide the community with realistic simulations of a flaring loop with an emphasis on the detailed treatment of the chromospheric energy balance. This will enable a detailed comparison of existing and upcoming observations with synthetic observables from the simulations, thereby elucidating the complex interactions in a flaring chromosphere.Methods. We used the 1D radiation hydrodynamics code RADYN to perform simulations of the effect of a beam of …

Flare-induced photospheric velocity diagnostics

Authors

Aaron J Monson,Mihalis Mathioudakis,Aaron Reid,Ryan Milligan,David Kuridze

Journal

The Astrophysical Journal

Published Date

2021/6/29

We present radiative-hydrodynamic simulations of solar flares generated by the RADYN and RH codes to study the perturbations induced in photospheric Fe i lines by electron beam heating. We investigate how variations in the beam parameters result in discernible differences in the induced photospheric velocities. Line synthesis revealed a significant chromospheric contribution to the line profiles resulting in an apparent red asymmetry by as much as 40 ms− 1 close to the time of maximum beam heating, which was not reflective of the upflow velocities that arose from the radiative-hydrodynamic simulations at those times. The apparent redshift to the overall line profile was produced by significant chromospheric emission that was blueshifted by as much as 400 ms− 1 and fills in the blue side of the near-stationary photospheric absorption profile. The velocity information that can be retrieved from photospheric line …

Critical Science Plan for the Daniel K. Inouye Solar Telescope (DKIST)

Authors

Mark P Rast,Nazaret Bello González,Luis Bellot Rubio,Wenda Cao,Gianna Cauzzi,Edward DeLuca,Bart De Pontieu,Lyndsay Fletcher,Sarah E Gibson,Philip G Judge,Yukio Katsukawa,Maria D Kazachenko,Elena Khomenko,Enrico Landi,Valentín Martínez Pillet,Gordon JD Petrie,Jiong Qiu,Laurel A Rachmeler,Matthias Rempel,Wolfgang Schmidt,Eamon Scullion,Xudong Sun,Brian T Welsch,Vincenzo Andretta,Patrick Antolin,Thomas R Ayres,KS Balasubramaniam,Istvan Ballai,Thomas E Berger,Stephen J Bradshaw,Ryan J Campbell,Mats Carlsson,Roberto Casini,Rebecca Centeno,Steven R Cranmer,Serena Criscuoli,Craig DeForest,Yuanyong Deng,Robertus Erdélyi,Viktor Fedun,Catherine E Fischer,Sergio J González Manrique,Michael Hahn,Louise Harra,Vasco MJ Henriques,Neal E Hurlburt,Sarah Jaeggli,Shahin Jafarzadeh,Rekha Jain,Stuart M Jefferies,Peter H Keys,Adam F Kowalski,Christoph Kuckein,Jeffrey R Kuhn,David Kuridze,Jiajia Liu,Wei Liu,Dana Longcope,Mihalis Mathioudakis,RT James McAteer,Scott W McIntosh,David E McKenzie,Mari Paz Miralles,Richard J Morton,Karin Muglach,Chris J Nelson,Navdeep K Panesar,Susanna Parenti,Clare E Parnell,Bala Poduval,Kevin P Reardon,Jeffrey W Reep,Thomas A Schad,Donald Schmit,Rahul Sharma,Hector Socas-Navarro,Abhishek K Srivastava,Alphonse C Sterling,Yoshinori Suematsu,Lucas A Tarr,Sanjiv Tiwari,Alexandra Tritschler,Gary Verth,Angelos Vourlidas,Haimin Wang,Yi-Ming Wang,NSO,DKIST project,and DKIST instrument scientists,DKIST Science Working Group,DKIST Critical Science Plan Community

Journal

Solar Physics

Published Date

2021/4

The National Science Foundation’s Daniel K. Inouye Solar Telescope (DKIST) will revolutionize our ability to measure, understand, and model the basic physical processes that control the structure and dynamics of the Sun and its atmosphere. The first-light DKIST images, released publicly on 29 January 2020, only hint at the extraordinary capabilities that will accompany full commissioning of the five facility instruments. With this Critical Science Plan (CSP) we attempt to anticipate some of what those capabilities will enable, providing a snapshot of some of the scientific pursuits that the DKIST hopes to engage as start-of-operations nears. The work builds on the combined contributions of the DKIST Science Working Group (SWG) and CSP Community members, who generously shared their experiences, plans, knowledge, and dreams. Discussion is primarily focused on those issues to which DKIST will …

Flare-induced Sunquake Signatures in the Ultraviolet as Observed by the Atmospheric Imaging Assembly

Authors

Sean Quinn,Mihalis Mathioudakis,Christopher J Nelson,Ryan O Milligan,Aaron Reid,David B Jess

Journal

The Astrophysical Journal

Published Date

2021/10/8

Sunquakes (SQs) have been routinely observed in the solar photosphere, but it is only recently that signatures of these events have been detected in the chromosphere. We investigate whether signatures of SQs are common in ultraviolet (UV) continua that sample the solar plasma several hundred km above where SQs are typically detected. We analyze observations from the Solar Dynamics Observatory's Atmospheric Imaging Assembly (SDO/AIA) 1600 and 1700 Å passbands, for SQ signatures induced by the flares of Solar Cycle 24. We base our analysis on the 62 SQs detected in the recent statistical study presented by Sharykin & Kosovichev. We find that 9 out of 62 SQ candidates produced a response that is clearly detected in running-difference images from the AIA 1600 and 1700 Å channels. A binary frequency filter with a width of 2 mHz, centered on 6 mHz, was applied to the data. The first signature of …

Non-LTE inversions of a confined X2. 2 flare-I. The vector magnetic field in the photosphere and chromosphere

Authors

Gregal JM Vissers,Sanja Danilovic,Jaime de la Cruz Rodríguez,Jorrit Leenaarts,Roberta Morosin,CJ Díaz Baso,A Reid,Jens Pomoell,DJ Price,S Inoue

Journal

Astronomy & Astrophysics

Published Date

2021/1/1

Context Obtaining an accurate measurement of magnetic field vector in the solar atmosphere is essential for studying changes in field topology during flares and reliably modelling space weather.Aims We tackle this problem by applying various inversion methods to a confined X2.2 flare that occurred in NOAA AR 12673 on 6 September 2017 and comparing the photospheric and chromospheric magnetic field vector with the results of two numerical models of this event.Methods We obtained the photospheric magnetic field from Milne-Eddington and (non-)local thermal equilibrium (non-LTE) inversions of Hinode SOT/SP Fe I 6301.5 Å and 6302.5 Å. The chromospheric field was obtained from a spatially regularised weak-field approximation (WFA) and non-LTE inversions of Ca II 8542 Å observed with CRISP at the Swedish 1 m Solar Telescope. We investigated the field strengths and photosphere-to …

Constraining the magnetic vector in the quiet solar photosphere and the impact of instrumental degradation

Authors

Ryan James Campbell,Sergiy Shelyag,C Quintero Noda,Michail Mathioudakis,PH Keys,Aaron Reid

Journal

Astronomy & Astrophysics

Published Date

2021/10/1

Context With the advent of next generation high resolution telescopes, our understanding of how the magnetic field is organized in the internetwork (IN) photosphere is likely to advance significantly.Aims We aim to evaluate the extent to which we can retrieve accurate information about the magnetic vector in the IN photosphere using inversion techniques.Methods We use a snapshot produced from high resolution three-dimensional magnetohydrodynamic (MHD) simulations and employ the Stokes Inversions based on Response functions (SIR) code to produce synthetic observables in the same near infrared spectral window as observed by the GREGOR Infrared Spectrograph (GRIS), which contains the highly magnetically sensitive photospheric Fe I line pair at 15 648.52 Å and 15 652.87 Å. We then use a parallelized wrapper to SIR to perform nearly 14 million inversions of the synthetic spectra to test how well …

Temporal evolution of small-scale internetwork magnetic fields in the solar photosphere (Corrigendum)

Authors

RJ Campbell,M Mathioudakis,M Collados,PH Keys,A Asensio Ramos,CJ Nelson,D Kuridze,A Reid

Journal

Astronomy & Astrophysics

Published Date

2021/8/1

We correct a typographical error in the original paper. Figures 10, 12, 14, 15, and 16 contain a table in the top right panel with four columns and four rows of values. The line of sight velocity, vLOS, values for scheme 1 inversions (in the fourth row, first column and second column) are inserted the wrong way around. The values themselves are correct, but printed in the wrong column. All other values in the tables remain unaffected, and none of the paper’s discussions or conclusions are impacted. We provide corrected versions of Figs. 10, 12, 14, 15, and 16 in Figs. 1, 2, 3, 4, and 5, respectively.

Chromospheric Bubbles in Solar Flares

Authors

Aaron Reid,Bogdan Zhigulin,Mats Carlsson,Mihalis Mathioudakis

Journal

The Astrophysical Journal Letters

Published Date

2020/5/12

We analyze a grid of radiative hydrodynamic simulations of solar flares to study the energy balance and response of the atmosphere to nonthermal electron beam heating. The appearance of chromospheric bubbles is one of the most notable features that we find in the simulations. These pockets of chromospheric plasma get trapped between the transition region and the lower atmosphere as it is superheated by the particle beam. The chromospheric bubbles are seen in the synthetic spectra, appearing as an additional component to Balmer line profiles with high Doppler velocities as high as 200 km s− 1. Their signatures are also visible in the wings of Ca ii 8542 Å line profiles. These bubbles of chromospheric plasma are driven upward by a wave front that is induced by the shock of energy deposition, and require a specific heating rate and atmospheric location to manifest.

High-resolution spectropolarimetric observations of the temporal evolution of magnetic fields in photospheric bright points

Authors

Peter H Keys,Aaron Reid,Mihalis Mathioudakis,Sergiy Shelyag,Vasco MJ Henriques,Rebecca L Hewitt,Dario Del Moro,Shahin Jafarzadeh,David B Jess,Marco Stangalini

Journal

Astronomy & Astrophysics

Published Date

2020/1/1

Context Magnetic bright points (MBPs) are dynamic, small-scale magnetic elements often found with field strengths of the order of a kilogauss within intergranular lanes in the photosphere.Aims Here we study the evolution of various physical properties inferred from inverting high-resolution full Stokes spectropolarimetry data obtained from ground-based observations of the quiet Sun at disc centre.Methods Using automated feature-tracking algorithms, we studied 300 MBPs and analysed their temporal evolution as they evolved to kilogauss field strengths. These properties were inferred using both the NICOLE and SIR Stokes inversion codes. We employ similar techniques to study radiative magnetohydrodynamical simulations for comparison with our observations.Results Evidence was found for fast (∼30−100 s) amplification of magnetic field strength (by a factor of 2 on average) in MBPs during their evolution in …

An Introduction to Photospheric Flare Line Diagnostics

Authors

Aaron Monson,Mihalis Mathioudakis,R Milligan,Aaron Reid,David Kuridze

Journal

AGU Fall Meeting Abstracts

Published Date

2020/12

In preparation for solar cycle 25, we present radiative hydrodynamic flare models from the F-CHROMA archive constructed using the RADYN and RH codes. We simulate potential observable perturbations seen in the line-of-sight velocity and heating induced in the photosphere during a flare. Many works have focused on the recreation of chromospheric spectral line profiles as the atmosphere rapidly heats and expands due to the injection of energy from magnetic reconnection. This extreme heating mechanism can permeate through the upper atmosphere and affect the lowest levels of the solar atmosphere. This results in an observable brightening and Doppler shifting of spectral lines formed in the deepest regions, though the extent of this photospheric reaction is still not fully characterised. We investigate how variations in the properties of a solar flare-accelerated electron beam result in discernible asymmetries …

UK Solar Physics

Authors

Richard Morton

Journal

Institutions

Published Date

2018/10/15

The history and present state of large-scale magnetohydrodynamic modeling of the solar corona and the solar wind with steady or quasi-steady coronal physics is reviewed. We put the evolution of ideas leading to the recognition of the existence of an expanding solar atmosphere into historical context. The development and main features of the first generation of global corona and solar wind models are described in detail. This historical perspective is also applied to the present suite of global corona and solar wind models. We discuss the evolution of new ideas and their implementation into numerical simulation codes. We point out the scientific and computational challenges facing these models and discuss the ways various groups tried to overcome these challenges. Next, we discuss the latest, state-of-the art models and point to the expected next steps in modeling the corona and the interplanetary medium.

See List of Professors in Aaron Reid University(Queen's University Belfast)

Aaron Reid FAQs

What is Aaron Reid's h-index at Queen's University Belfast?

The h-index of Aaron Reid has been 11 since 2020 and 13 in total.

What are Aaron Reid's top articles?

The articles with the titles of

The F-CHROMA grid of 1D RADYN flare models

Flare-induced photospheric velocity diagnostics

Critical Science Plan for the Daniel K. Inouye Solar Telescope (DKIST)

Flare-induced Sunquake Signatures in the Ultraviolet as Observed by the Atmospheric Imaging Assembly

Non-LTE inversions of a confined X2. 2 flare-I. The vector magnetic field in the photosphere and chromosphere

Constraining the magnetic vector in the quiet solar photosphere and the impact of instrumental degradation

Temporal evolution of small-scale internetwork magnetic fields in the solar photosphere (Corrigendum)

Chromospheric Bubbles in Solar Flares

...

are the top articles of Aaron Reid at Queen's University Belfast.

What are Aaron Reid's research interests?

The research interests of Aaron Reid are: Solar Physics, Astronomy, Magnetic Reconnection

What is Aaron Reid's total number of citations?

Aaron Reid has 561 citations in total.

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