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Coronal energy release by MHD avalanches: continuous driving

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Coronal energy release by MHD avalanches : continuous driving. / Reid, Jack; Hood, Alan William; Parnell, Clare Elizabeth; Browning, P. K.; Cargill, Peter.

In: Astronomy & Astrophysics, Vol. 615, 84, 18.07.2018.

Research output: Contribution to journalArticle

Harvard

Reid, J, Hood, AW, Parnell, CE, Browning, PK & Cargill, P 2018, 'Coronal energy release by MHD avalanches: continuous driving', Astronomy & Astrophysics, vol. 615, 84. https://doi.org/10.1051/0004-6361/201732399

APA

Reid, J., Hood, A. W., Parnell, C. E., Browning, P. K., & Cargill, P. (2018). Coronal energy release by MHD avalanches: continuous driving. Astronomy & Astrophysics, 615, [84]. https://doi.org/10.1051/0004-6361/201732399

Vancouver

Reid J, Hood AW, Parnell CE, Browning PK, Cargill P. Coronal energy release by MHD avalanches: continuous driving. Astronomy & Astrophysics. 2018 Jul 18;615. 84. https://doi.org/10.1051/0004-6361/201732399

Author

Reid, Jack ; Hood, Alan William ; Parnell, Clare Elizabeth ; Browning, P. K. ; Cargill, Peter. / Coronal energy release by MHD avalanches : continuous driving. In: Astronomy & Astrophysics. 2018 ; Vol. 615.

Bibtex - Download

@article{c0ab03bb51ac4e19a64a02db5672274b,
title = "Coronal energy release by MHD avalanches: continuous driving",
abstract = "Previous work has confirmed the concept of a magnetohydrodynamic (MHD) avalanche in pre-stressed threads within a coronal loop. We undertook a series of full, three-dimensional MHD simulations in order to create three threads by twisting the magnetic field through boundary motions until an instability ensues. We find that, following the original instability, one unstable thread can disrupt its neighbours with continued driving. A {\textquoteleft}bursty{\textquoteright} heating profile results, with a series of ongoing energy releases, but no evident steady state. For the first time using full MHD, we show that avalanches are a viable mechanism for the storing and release of magnetic energy in the solar corona, as a result of photospheric motions.",
keywords = "Sun: corona, Sun: magnetic fields, Magnetohydrodynamic (MHD), Methods: numerical",
author = "Jack Reid and Hood, {Alan William} and Parnell, {Clare Elizabeth} and Browning, {P. K.} and Peter Cargill",
note = "Funding: Carnegie Trust for the Universities of Scotland; Science and Technology Facilities Council (grants ST/N000609/1 and ST/P000428/1).",
year = "2018",
month = jul,
day = "18",
doi = "10.1051/0004-6361/201732399",
language = "English",
volume = "615",
journal = "Astronomy & Astrophysics",
issn = "0004-6361",
publisher = "EDP SCIENCES S A",

}

RIS (suitable for import to EndNote) - Download

TY - JOUR

T1 - Coronal energy release by MHD avalanches

T2 - continuous driving

AU - Reid, Jack

AU - Hood, Alan William

AU - Parnell, Clare Elizabeth

AU - Browning, P. K.

AU - Cargill, Peter

N1 - Funding: Carnegie Trust for the Universities of Scotland; Science and Technology Facilities Council (grants ST/N000609/1 and ST/P000428/1).

PY - 2018/7/18

Y1 - 2018/7/18

N2 - Previous work has confirmed the concept of a magnetohydrodynamic (MHD) avalanche in pre-stressed threads within a coronal loop. We undertook a series of full, three-dimensional MHD simulations in order to create three threads by twisting the magnetic field through boundary motions until an instability ensues. We find that, following the original instability, one unstable thread can disrupt its neighbours with continued driving. A ‘bursty’ heating profile results, with a series of ongoing energy releases, but no evident steady state. For the first time using full MHD, we show that avalanches are a viable mechanism for the storing and release of magnetic energy in the solar corona, as a result of photospheric motions.

AB - Previous work has confirmed the concept of a magnetohydrodynamic (MHD) avalanche in pre-stressed threads within a coronal loop. We undertook a series of full, three-dimensional MHD simulations in order to create three threads by twisting the magnetic field through boundary motions until an instability ensues. We find that, following the original instability, one unstable thread can disrupt its neighbours with continued driving. A ‘bursty’ heating profile results, with a series of ongoing energy releases, but no evident steady state. For the first time using full MHD, we show that avalanches are a viable mechanism for the storing and release of magnetic energy in the solar corona, as a result of photospheric motions.

KW - Sun: corona

KW - Sun: magnetic fields

KW - Magnetohydrodynamic (MHD)

KW - Methods: numerical

U2 - 10.1051/0004-6361/201732399

DO - 10.1051/0004-6361/201732399

M3 - Article

VL - 615

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

SN - 0004-6361

M1 - 84

ER -

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ID: 252750837

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