Emergence of non-twisted magnetic fields in the Sun: jets and atmospheric response

P. Syntelis; V. Archontis; C. Gontikakis; K. Tsinganos

doi:10.1051/0004-6361/201423781

Emergence of non-twisted magnetic fields in the Sun: jets and atmospheric response

P. Syntelis^*, V. Archontis, C. Gontikakis, K. Tsinganos

^*Corresponding author for this work

Applied Mathematics

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Abstract

Aims. We study the emergence of a non-twisted flux tube from the solar interior into the solar atmosphere. We investigate whether the length of the buoyant part of the flux tube (i.e. λ) affects the emergence of the field and the dynamics of the evolving magnetic flux system.

Methods. We perform three-dimensional (3D), time-dependent, resistive, compressible magnetohydrodynamic (MHD) simulations using the Lare3D code.

Results. We find that there are considerable differences in the dynamics of the emergence of a magnetic flux tube when λ is varied. In the solar interior, for larger values of λ, the rising magnetic field emerges faster and expands more due to its lower magnetic tension. As a result, its field strength decreases and its emergence above the photosphere occurs later than in the smaller λ case. However, in both cases, the emerging field at the photosphere becomes unstable in two places, forming two magnetic bipoles that interact dynamically during the evolution of the system. Most of the dynamic phenomena occur at the current layer, which is formed at the interface between the interacting bipoles. We find the formation and ejection of plasmoids, the onset of successive jets from the interface, and the impulsive heating of the plasma in the solar atmosphere. We discuss the triggering mechanism of the jets and the atmospheric response to the emergence of magnetic flux in the two cases.

Original language	English
Article number	A10
Pages (from-to)	1-15
Number of pages	15
Journal	Astronomy & Astrophysics
Volume	584
Early online date	13 Nov 2015
DOIs	https://doi.org/10.1051/0004-6361/201423781
Publication status	Published - Dec 2015

Keywords

Sun: activity
Sun: interior
Sun: magnetic fields
Magnetohydrodynamics (MHD)
Methods: numerical

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10.1051/0004-6361/201423781Licence: CC BY

Syntelis_2015_A&A_Non-twistedMagneticFields_CC
© ESO, 2015. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
Final published version, 4.38 MBLicence: CC BY

Solar & Magnetospheric Plasma Theory: Solar and Magnetospheric plasma theory
Hood, A. W. (PI), Neukirch, T. (CoI) & Roberts, B. (CoI)
Science & Technology Facilities Council
1/04/10 → 31/03/15
Project: Standard

Cite this

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title = "Emergence of non-twisted magnetic fields in the Sun: jets and atmospheric response",

abstract = "Aims. We study the emergence of a non-twisted flux tube from the solar interior into the solar atmosphere. We investigate whether the length of the buoyant part of the flux tube (i.e. λ) affects the emergence of the field and the dynamics of the evolving magnetic flux system.Methods. We perform three-dimensional (3D), time-dependent, resistive, compressible magnetohydrodynamic (MHD) simulations using the Lare3D code.Results. We find that there are considerable differences in the dynamics of the emergence of a magnetic flux tube when λ is varied. In the solar interior, for larger values of λ, the rising magnetic field emerges faster and expands more due to its lower magnetic tension. As a result, its field strength decreases and its emergence above the photosphere occurs later than in the smaller λ case. However, in both cases, the emerging field at the photosphere becomes unstable in two places, forming two magnetic bipoles that interact dynamically during the evolution of the system. Most of the dynamic phenomena occur at the current layer, which is formed at the interface between the interacting bipoles. We find the formation and ejection of plasmoids, the onset of successive jets from the interface, and the impulsive heating of the plasma in the solar atmosphere. We discuss the triggering mechanism of the jets and the atmospheric response to the emergence of magnetic flux in the two cases.",

keywords = "Sun: activity, Sun: interior, Sun: magnetic fields, Magnetohydrodynamics (MHD), Methods: numerical",

author = "P. Syntelis and V. Archontis and C. Gontikakis and K. Tsinganos",

note = "The authors acknowledge support by the EU (IEF-272549 grant) and the Royal Society. The present research has been co-financed by the European Union (European Social Fund-ESF) and Greek national funds through the Operational Program “Education and Lifelong Learning” of the National Strategic Reference Framework (NSRF) – Research Funding Program: Thales. Investing in knowledge society through the European Social Fund. This research has also been carried out in the frame of the research program of the RCAAM of the Academy of Athens and has been co-financed by the Program “IKY Scholarships” of the Greek national funds through the Operational Program Education and Lifelong Learning of the NSRF through the European Social Fund of ESPA 2007-2013. Finally, the work reported in this article was additionally supported by the SOLARNET project, funded by the European Commisions FP7 Capacities Program, under the Grant Agreement 312495. The simulations were performed on the STFC and SRIF funded UKMHD cluster, at the University of St Andrews.",

year = "2015",

month = dec,

doi = "10.1051/0004-6361/201423781",

language = "English",

volume = "584",

pages = "1--15",

journal = "Astronomy & Astrophysics",

issn = "1432-0746",

publisher = "EDP SCIENCES S A",

}

TY - JOUR

T1 - Emergence of non-twisted magnetic fields in the Sun

T2 - jets and atmospheric response

AU - Syntelis, P.

AU - Archontis, V.

AU - Gontikakis, C.

AU - Tsinganos, K.

N1 - The authors acknowledge support by the EU (IEF-272549 grant) and the Royal Society. The present research has been co-financed by the European Union (European Social Fund-ESF) and Greek national funds through the Operational Program “Education and Lifelong Learning” of the National Strategic Reference Framework (NSRF) – Research Funding Program: Thales. Investing in knowledge society through the European Social Fund. This research has also been carried out in the frame of the research program of the RCAAM of the Academy of Athens and has been co-financed by the Program “IKY Scholarships” of the Greek national funds through the Operational Program Education and Lifelong Learning of the NSRF through the European Social Fund of ESPA 2007-2013. Finally, the work reported in this article was additionally supported by the SOLARNET project, funded by the European Commisions FP7 Capacities Program, under the Grant Agreement 312495. The simulations were performed on the STFC and SRIF funded UKMHD cluster, at the University of St Andrews.

PY - 2015/12

Y1 - 2015/12

N2 - Aims. We study the emergence of a non-twisted flux tube from the solar interior into the solar atmosphere. We investigate whether the length of the buoyant part of the flux tube (i.e. λ) affects the emergence of the field and the dynamics of the evolving magnetic flux system.Methods. We perform three-dimensional (3D), time-dependent, resistive, compressible magnetohydrodynamic (MHD) simulations using the Lare3D code.Results. We find that there are considerable differences in the dynamics of the emergence of a magnetic flux tube when λ is varied. In the solar interior, for larger values of λ, the rising magnetic field emerges faster and expands more due to its lower magnetic tension. As a result, its field strength decreases and its emergence above the photosphere occurs later than in the smaller λ case. However, in both cases, the emerging field at the photosphere becomes unstable in two places, forming two magnetic bipoles that interact dynamically during the evolution of the system. Most of the dynamic phenomena occur at the current layer, which is formed at the interface between the interacting bipoles. We find the formation and ejection of plasmoids, the onset of successive jets from the interface, and the impulsive heating of the plasma in the solar atmosphere. We discuss the triggering mechanism of the jets and the atmospheric response to the emergence of magnetic flux in the two cases.

AB - Aims. We study the emergence of a non-twisted flux tube from the solar interior into the solar atmosphere. We investigate whether the length of the buoyant part of the flux tube (i.e. λ) affects the emergence of the field and the dynamics of the evolving magnetic flux system.Methods. We perform three-dimensional (3D), time-dependent, resistive, compressible magnetohydrodynamic (MHD) simulations using the Lare3D code.Results. We find that there are considerable differences in the dynamics of the emergence of a magnetic flux tube when λ is varied. In the solar interior, for larger values of λ, the rising magnetic field emerges faster and expands more due to its lower magnetic tension. As a result, its field strength decreases and its emergence above the photosphere occurs later than in the smaller λ case. However, in both cases, the emerging field at the photosphere becomes unstable in two places, forming two magnetic bipoles that interact dynamically during the evolution of the system. Most of the dynamic phenomena occur at the current layer, which is formed at the interface between the interacting bipoles. We find the formation and ejection of plasmoids, the onset of successive jets from the interface, and the impulsive heating of the plasma in the solar atmosphere. We discuss the triggering mechanism of the jets and the atmospheric response to the emergence of magnetic flux in the two cases.

KW - Sun: activity

KW - Sun: interior

KW - Sun: magnetic fields

KW - Magnetohydrodynamics (MHD)

KW - Methods: numerical

U2 - 10.1051/0004-6361/201423781

DO - 10.1051/0004-6361/201423781

M3 - Article

SN - 1432-0746

VL - 584

SP - 1

EP - 15

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A10

ER -

Emergence of non-twisted magnetic fields in the Sun: jets and atmospheric response

Abstract

Keywords

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Projects

Solar & Magnetospheric Plasma Theory: Solar and Magnetospheric plasma theory

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