| 2023 |
| |
| Terradas, J. & Neukirch, T. | Three-dimensional solar active region magnetohydrostatic models and their stability using Euler potentials |
| 2022 |
| Allanson, O., Elsden, T., Watt, C. & Neukirch, T. | Weak Turbulence and Quasilinear Diffusion for Relativistic Wave-Particle Interactions Via a Markov Approach |
| Archer, M. O., Southwood, D. J., Hartinger, M. D., Rastaetter, L. & Wright, A. N. | How a realistic magnetosphere alters the polarizations of surface, fast magnetosonic, and Alfvén waves |
| De Pontieu, B., Testa, P., Martínez-Sykora, J., Antolin, P., Karampelas, K., Hansteen, V., Rempel, M., Cheung, M. C. M., Reale, F., Danilovic, S., Pagano, P., Polito, V., De Moortel, I., Nóbrega-Siverio, D., Van Doorsselaere, T., Petralia, A., Asgari-Targhi, M., Boerner, P., Carlsson, M., Chintzoglou, G. & 7 others. | Probing the physics of the solar atmosphere with the Multi-slit Solar Explorer (MUSE). I. Coronal heating |
| Elsden, T. & Wright, A. N. | Polarisation properties of 3-D field line resonances |
| Howson, T. A. & De Moortel, I. | The effects of driving time scales on coronal heating in a stratified atmosphere |
| Madjarska, M., Mackay, D. H., Galsgaard, K., Wiegelmann, T. & Xie, H. | Eruptions from coronal bright points: a spectroscopic view by IRIS of a mini-filament eruption, QSL reconnection, and reconnection-driven outflows |
| Moreno-Insertis, F., Nóbrega-Siverio, D., Priest, E. R. & Hood, A. W. | Ambipolar diffusion: self-similar solutions and MHD code testing. Cylindrical symmetry |
| Pascoe, D. J., Van Doorsselaere, T. & De Moortel, I. | Coronal seismology using damping of propagating kink waves |
| Wright, A., Degeling, A. & Elsden, T. | Resonance maps for 3D Alfvén waves in a compressed dipole field |
| 2021 |
| Banerjee, D., Krishna Prasad, S., Pant, V., McLaughlin, J. A., Antolin, P., Magyar, N., Ofman, L., Tian, H., Van Doorsselaere, T., De Moortel, I.& Wang, T. J. | Magnetohydrodynamic waves in open coronal structures |
Fyfe, L., Howson, T. A., De Moortel, I.,
Pant, V. & Van Doorsselaere, T. | Investigating coronal wave energy estimates using synthetic non-thermal line widths |
| Fyfe, LE., Howson, TA. & De Moortel, I. | Forward modelling of heating within a coronal arcade |
| Howson, T. A., De Moortel, I. & Pontin, D. | Magnetic reconnection and the Kelvin-Helmholtz instability in the solar corona |
| Johnston, C. D.; Cargill, P. J.; Antolin, P.; Hood, A. W.; De Moortel, I.; Bradshaw, S. J. | The effects of numerical resolution, heating timescales and background heating on thermal non-equilibrium in coronal loops |
Johnston, C. D., Hood, A. W., De Moortel, I.,
Pagano, P. & Howson, T. A. | A fast multi-dimensional magnetohydrodynamic formulation of the transition region adaptive conduction (TRAC) method |
| Lehmann, L. T., Hussain, G. A. J., Vidotto, A., Jardine, M. M. & Mackay, D. H. | Identifying solar-like magnetic cycles with Zeeman-Doppler-Imaging (ZDI) |
| Mackay, D. H. | Solar prominences |
| Mackay, D. H. & Yeates, A. | A comparison of sparse and non-sparse techniques for electric-field inversion from normal-component magnetograms |
| Prokopyszyn, APK., Wright, AN. & Hood, AW. | Line-tied boundary conditions can cause resonant absorption models to generate unphysically large boundary layers |
| Parnell, C et al | Critical Science Plan for the Daniel K. Inouye Solar Telescope (DKIST) |
| Reid, J., Cargill, P., Johnston, C. D. & Hood, A. W. | Linking computational models to follow the evolution of heated coronal plasma |
| Threlfall, J., Reid, J. & Hood, A. W. | Can multi-threaded flux tubes in coronal arcades support a magnetohydrodynamic avalanche? |
| Viall, N., De Moortel, I., Downs, C., Klimchuk, J. A., Parenti, S. & Reale, F. | The heating of the solar corona |
| Yardley, S. L., Mackay, D. H. & Green, L. | Simulating the coronal evolution of bipolar active regions to investigate the formation of flux ropes |
Yardley, S. L., Pagano, P., Mackay, D. H.
& Upton, L. | Determining the source and eruption dynamics of a stealth CME using NLFFF modelling and MHD simulations |
| Zahid, Z., Parnell, C. E. & Qamar, A. | 3D non-driven magnetic reconnection at multiple separators |
| 2020 |
| Borissov, A., Neukirch, T., Kontar, E.,Threlfall, J. & Parnell, C. | Particle acceleration with anomalous pitch angle scattering in 3D separator reconnection |
| De Moortel, I., Falconer, I. & Stack, R., | Alfvén on heating by waves |
| Elsden, T. & Wright, A. | Evolution of high-m poloidal Alfvén waves in a dipole magnetic field |
| Fyfe, L., Howson, T. A. & De Moortel, I. | Forward modelling of MHD Waves in braided magnetic fields |
| Howson, T. A., De Moortel, I. & Fyfe, L. | The effects of driving time scales on heating in a coronal arcade |
| Howson, T. A., De Moortel, I. & Reid, J. | Phase mixing and wave heating in a complex coronal plasma |
Johnston, C. D., Cargill, P. J., Hood, A. W., De Moortel, I., Bradshaw, S. J. & Vaseekar, A. C.
| Modelling the solar transition region using an adaptive conduction method |
| Lehmann, L. T., Hussain, G. A. J., Vidotto, A., Jardine, M. M. & Mackay, D. H. | Identifying solar-like magnetic cycles with Zeeman-Doppler-Imaging (ZDI) |
| Love, T., Neukirch, T. & Parnell, C. E. | Analyzing AIA flare observations using convolutional neural networks |
| Lund, K., Jardine, M., Lehmann, L. T., Mackay, D. H., See, Vidotto, A. A., Donati, J-F., Fares, R., Folsom, C. P., Jeffers, S., Marsden, S. C., Morin, J. & Petit, P. | Measuring stellar magnetic helicity density |
| Mackay, D. H., Schmieder, B., Lopez Ariste, A. & Su, Y. | Modelling and observations: a comparison of the magnetic field properties in a prominence |
Madjarska, M., Galsgaard, K., Mackay, D. H.,
Koleva, K. & Dechev, M. | Eruptions from coronal hole bright points: observations and non-potential modeling |
Meyer, K. A., Mackay, D. H.,
Talpeanu, D-C., Upton, L. & West, M. | Investigation of the middle corona with SWAP and a data-driven non-potential coronal magnetic field model |
| Neukirch, T., Vasko, I. Y., Artemyev, A. V. & Allanson, O. | Kinetic models of tangential discontinuities in the solar wind |
| Neukirch, T., Wilson, F. & Allanson, O. | A family of Vlasov-Maxwell equilibrium distribution functions describing a transition from the Harris sheet to the force-free Harris sheet |
| Olshevsky, V., Pontin I, D., Williams, B., Parnell, C. E., Fu, H. S., Liu, Y., Yao, S. & Khotyaintsev V, Y. | A comparison of methods for finding magnetic nulls in simulations and in situ observations of space plasmas |
| Pagano, P., Bemporad, A. & Mackay, D. H. | Hydrogen non-equilibrium ionisation effects in coronal mass ejections |
| Pagano, P., De Moortel, I. & Morton,R. | Effect of coronal loop structure on wave heating by phase mixing |
| Patsourakos, S., Vourlidas, A., Török, T., Kliem, B., Antiochos, S. K., Archontis, V., Aulanier, G., Cheng, X., Chintzoglou, G., Georgoulis, M. K., Green, L. M., Leake, J. E., Moore, R., Nindos, A., Syntelis, P., Yardley, S. L., Yurchyshyn, V. & Zhang, J | Decoding the pre-eruptive magnetic field configurations of coronal mass ejections |
| Reid, J., Cargill, P., Hood, A. W., Parnell, C. E. & Arber, T. D. | Coronal energy release by MHD avalanches: heating mechanisms |
| Reid, J., Parnell, C. E., Hood, A. W. & Browning, P. K. | Determining whether the squashing factor, Q, would be a good indicator of reconnection in a resistive MHD experiment devoid of null points |
| Threlfall, J., Wright, A. N. & Hood, A. W. | How is helicity (and twist) partitioned in magnetohydrodynamic simulations of reconnecting magnetic flux tubes? |
| Van Damme, H. J., De Moortel, I., Pagano, P. & Johnston, C. D. | Chromospheric evaporation and phase mixing of Alfvén waves in coronal loops |
| Van Doorsselaere, T., Srivastava, A. K., Antolin, P., Magyar, N., Vasheghani Farahani, S., Tian, H., Kolotkov, D., Ofman, L., Guo, M., Arregui, I., De Moortel, I. & Pascoe, D. | Coronal heating by MHD waves |
| Wiegelmann, T., Neukirch, T., Nickeler, D. & Chifu, I. | An optimization principle for computing stationary MHD equilibria with solar wind flow |
| Wright, A. N. & Elsden, T. | Simulations of MHD wave propagation and coupling in a 3D magnetosphere |