The influence of flux rope heating models on solar prominence formation

被引:18
作者
Brughmans, N. [1 ]
Jenkins, J. M. [1 ]
Keppens, R. [1 ]
机构
[1] Katholieke Univ Leuven, Ctr Math Plasma Astrophys, Celestijnenlaan 200B, B-3001 Leuven, Belgium
基金
欧洲研究理事会;
关键词
Sun:; filaments; prominences; -; Sun; atmosphere; corona - magnetohydrodynamics (MHD); THERMAL-INSTABILITY; MAGNETIC-STRUCTURE; MPI-AMRVAC; CONDENSATION; SCHEME; SYSTEMS; GAS;
D O I
10.1051/0004-6361/202244071
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Context. Prominences are cool, dense clouds suspended within the solar corona. Their in situ formation through the levitation-condensation mechanism is a textbook example of the thermal instability, where a slight energy imbalance leads to a runaway process resulting in condensed filamentary structures embedded within the concave-up portions of a flux rope. The detailed interplay between local radiative losses and the global heating of the solar corona is investigated here for prominence-forming flux rope structures. Aims. We begin by exploring the influence of two classes of commonly adopted heating models on the formation behaviour of solar prominences. These models consider either an exponential variation dependent on height alone, or local density and magnetic field conditions. We highlight and address some of the limitations inherent to these early approximations by proposing a new, dynamic 2D flux rope heating model that qualitatively accounts for the 3D topology of the twisted flux rope field. Methods. We performed 2.5D grid-adaptive numerical simulations of prominence formation via the levitation-condensation mechanism. A linear force-free arcade is subjected to shearing and converging motions, leading to the formation of a flux rope containing material that may succumb to thermal instability. The eventual formation and subsequent evolution of prominence condensations was then quantified as a function of the specific background heating prescription adopted. For the simulations that consider the topology of the flux rope, reduced heating was considered within a dynamically evolving ellipse that traces the flux rope cross-section. This ellipse is centred on the flux rope axis and tracked during runtime using an approach based on the instantaneous magnetic field curvature. Results. We find that the nature of the heating model is clearly imprinted on the evolution and morphology of any resulting prominences: one large, low-altitude condensation is obtained for the heating model based on local parameters, while the exponential model leads to the additional formation of smaller blobs throughout the flux rope which then relocate as they tend towards achieving hydrostatic equilibrium. Finally, a study of the condensation process in phase space reveals a non-isobaric evolution with an eventual recovery of uniform pressure balance along flux surfaces.
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页数:17
相关论文
共 76 条
[1]   A MODEL FOR THE FORMATION OF SOLAR PROMINENCES [J].
ANTIOCHOS, SK ;
KLIMCHUK, JA .
ASTROPHYSICAL JOURNAL, 1991, 378 (01) :372-377
[2]   Prominence oscillations [J].
Arregui, Inigo ;
Oliver, Ramon ;
Luis Ballester, Jose .
LIVING REVIEWS IN SOLAR PHYSICS, 2018, 15
[3]   MAGNETIC SHEAR .4. HALE REGIONS 16740, 16815, AND 16850 [J].
ATHAY, RG ;
KLIMCHUK, JA ;
JONES, HP ;
ZIRIN, H .
ASTROPHYSICAL JOURNAL, 1986, 303 (02) :884-&
[4]   Thermal Properties of Coronal Cavities [J].
Bak-Steslicka, Urszula ;
Gibson, Sarah E. ;
Steslicki, Marek .
SOLAR PHYSICS, 2019, 294 (11)
[5]   Toward detailed prominence seismology II. Charting the continuous magnetohydrodynamic spectrum [J].
Blokland, J. W. S. ;
Keppens, R. .
ASTRONOMY & ASTROPHYSICS, 2011, 532
[6]   Toward detailed prominence seismology I. Computing accurate 2.5D magnetohydrodynamic equilibria [J].
Blokland, J. W. S. ;
Keppens, R. .
ASTRONOMY & ASTROPHYSICS, 2011, 532
[7]  
Brughmans N., 2022, EPS PLASMA PHYS C P
[8]   Compact third-order limiter functions for finite volume methods [J].
Cada, Miroslav ;
Torrilhon, Manuel .
JOURNAL OF COMPUTATIONAL PHYSICS, 2009, 228 (11) :4118-4145
[9]   Magnetic maps of prominences from full Stokes analysis of the He I D3 line [J].
Casini, R ;
Ariste, AL ;
Tomczyk, S ;
Lites, BW .
ASTROPHYSICAL JOURNAL, 2003, 598 (01) :L67-L70
[10]   Thermal instabilities: Fragmentation and field misalignment of filament fine structure [J].
Claes, N. ;
Keppens, R. ;
Xia, C. .
ASTRONOMY & ASTROPHYSICS, 2020, 636