A cancellation nanoflare model for solar chromospheric and coronal heating

E. R. Priest; L. P. Chitta; P. Syntelis

doi:10.3847/2041-8213/aad4fc

A cancellation nanoflare model for solar chromospheric and coronal heating

E. R. Priest, L. P. Chitta, P. Syntelis

Applied Mathematics

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Abstract

Nanoflare models for heating the solar corona usually assume magnetic braiding and reconnection as the source of the energy. However, recent observations at record spatial resolution from the SUNRISE balloon mission suggest that photospheric magnetic flux cancellation is much more common than previously realized. We therefore examine the possibility of three-dimensional reconnection driven by flux cancellation as a cause of chromospheric and coronal heating. In particular, we estimate how the heights and amount of energy release produced by flux cancellation depend on flux size, flux cancellation speed, and overlying field strength.

Original language	English
Article number	L24
Number of pages	7
Journal	Astrophysical Journal Letters
Volume	862
Issue number	2
DOIs	https://doi.org/10.3847/2041-8213/aad4fc
Publication status	Published - 1 Aug 2018

Keywords

Magnetohydrodynamics: MHD
Magnetic reconnection
Sun: atmosphere
Sun: chromosphere
Sun: corona
Sun: magnetic fields

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10.3847/2041-8213/aad4fc

Priest_2018_AJ_cancellationnanoflaremodel_VoR
© 2018. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://doi.org/10.3847/2041-8213/aad4fc
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title = "A cancellation nanoflare model for solar chromospheric and coronal heating",

abstract = "Nanoflare models for heating the solar corona usually assume magnetic braiding and reconnection as the source of the energy. However, recent observations at record spatial resolution from the SUNRISE balloon mission suggest that photospheric magnetic flux cancellation is much more common than previously realized. We therefore examine the possibility of three-dimensional reconnection driven by flux cancellation as a cause of chromospheric and coronal heating. In particular, we estimate how the heights and amount of energy release produced by flux cancellation depend on flux size, flux cancellation speed, and overlying field strength.",

keywords = "Magnetohydrodynamics: MHD, Magnetic reconnection, Sun: atmosphere, Sun: chromosphere, Sun: corona, Sun: magnetic fields",

author = "Priest, {E. R.} and Chitta, {L. P.} and P. Syntelis",

note = "L.P.C. received funding from the European Union{\textquoteright}s Horizon 2020 research and innovation programme under the Marie Sk{\l}odowska-Curie grant agreement No. 707837. The German contribution to SUNRISE and its reflight was funded by the Max Planck Foundation, the Strategic Innovations Fund of the President of the Max Planck Society (MPG), DLR, and private donations by supporting members of the Max Planck Society. The Spanish contribution was funded by the Ministerio de Econom{\'i}a y Competitividad under Projects ESP2013-47349-C6 and ESP2014-56169-C6, partially using European FEDER funds.",

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doi = "10.3847/2041-8213/aad4fc",

language = "English",

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TY - JOUR

T1 - A cancellation nanoflare model for solar chromospheric and coronal heating

AU - Priest, E. R.

AU - Chitta, L. P.

AU - Syntelis, P.

N1 - L.P.C. received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 707837. The German contribution to SUNRISE and its reflight was funded by the Max Planck Foundation, the Strategic Innovations Fund of the President of the Max Planck Society (MPG), DLR, and private donations by supporting members of the Max Planck Society. The Spanish contribution was funded by the Ministerio de Economía y Competitividad under Projects ESP2013-47349-C6 and ESP2014-56169-C6, partially using European FEDER funds.

PY - 2018/8/1

Y1 - 2018/8/1

N2 - Nanoflare models for heating the solar corona usually assume magnetic braiding and reconnection as the source of the energy. However, recent observations at record spatial resolution from the SUNRISE balloon mission suggest that photospheric magnetic flux cancellation is much more common than previously realized. We therefore examine the possibility of three-dimensional reconnection driven by flux cancellation as a cause of chromospheric and coronal heating. In particular, we estimate how the heights and amount of energy release produced by flux cancellation depend on flux size, flux cancellation speed, and overlying field strength.

AB - Nanoflare models for heating the solar corona usually assume magnetic braiding and reconnection as the source of the energy. However, recent observations at record spatial resolution from the SUNRISE balloon mission suggest that photospheric magnetic flux cancellation is much more common than previously realized. We therefore examine the possibility of three-dimensional reconnection driven by flux cancellation as a cause of chromospheric and coronal heating. In particular, we estimate how the heights and amount of energy release produced by flux cancellation depend on flux size, flux cancellation speed, and overlying field strength.

KW - Magnetohydrodynamics: MHD

KW - Magnetic reconnection

KW - Sun: atmosphere

KW - Sun: chromosphere

KW - Sun: corona

KW - Sun: magnetic fields

UR - https://arxiv.org/abs/1807.08161

U2 - 10.3847/2041-8213/aad4fc

DO - 10.3847/2041-8213/aad4fc

M3 - Article

SN - 2041-8205

VL - 862

JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

IS - 2

M1 - L24

ER -

A cancellation nanoflare model for solar chromospheric and coronal heating

Abstract

Keywords

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