Poynting Flux of MHD Modes in Magnetic Solar Vortex Tubes DOI Creative Commons
Samuel Skirvin, V. Fedun, M. Goossens

et al.

The Astrophysical Journal, Journal Year: 2024, Volume and Issue: 975(2), P. 176 - 176

Published: Nov. 1, 2024

Abstract Magnetic flux tubes in the presence of background rotational flows, known as solar vortex tubes, are abundant throughout atmosphere and may act conduits for MHD waves to transport magnetic energy upper atmosphere. We aim investigate Poynting associated with these within tubes. model a tube straight azimuthal velocity component. The wave solutions equilibrium configuration obtained using Shooting Eigensolver SolAr Magnetohydrostatic Equilibria code we derive an expression vertical component flux, S z , modes. In addition, present 2D visualizations spatial structure different modes under flow strengths. show that increases when compared no flow. When strength is greater than 100 times perturbation, non-axisymmetric (∣ m ∣ > 0) by over 1000% absence Furthermore, fundamental property vortices, namely they cannot solely produce upward untwisted tube, meaning any observed must arise from perturbations, such waves.

Language: Английский

Magnetohydrodynamic Poynting Flux Vortices in the Solar Atmosphere and Their Role in Concentrating Energy DOI Creative Commons
Suzana S. A. Silva, G. Verth, Erico L. Rempel

et al.

The Astrophysical Journal, Journal Year: 2024, Volume and Issue: 963(1), P. 10 - 10

Published: Feb. 21, 2024

Abstract The nature of energy generation, transport, and effective dissipation responsible for maintaining a hot solar upper atmosphere is still elusive. Poynting flux vital parameter describing the direction magnitude flow, which mainly used in physics estimating upward generated by photospheric plasma motion. This study presents pioneering 3D mapping magnetic transport within numerically simulated atmosphere. By calculating Finite Time Lyapunov Exponent velocity, defined as ratio to density, we precisely identify sources destinations flow throughout reveals presence barriers lower atmosphere, restricting amount from photosphere reaching chromosphere corona. Interacting kinematic vortices create channels, breaking through these allowing three times more input motions reach than before formed. vortex system also substantially alters mapping, acting source deposition energy, leading localized concentration. Furthermore, our results show that transported following vortical motion: vortex. In regions where coexist, they favor conditions ohmic viscous heating, since naturally large gradients velocity fields over small spatial scales. Hence, promotes local temperatures around million Kelvins.

Language: Английский

Citations

5
Magnetic Tornado Properties: A Substantial Contribution to the Solar Coronal Heating via Efficient Energy Transfer DOI Creative Commons
Hidetaka Kuniyoshi, Munehito Shoda, Haruhisa Iijima

et al.

The Astrophysical Journal, Journal Year: 2023, Volume and Issue: 949(1), P. 8 - 8

Published: May 1, 2023

Abstract In solving the solar coronal heating problem, it is crucial to comprehend mechanisms by which energy conveyed from photosphere corona. Recently, magnetic tornadoes, characterized as coherent, rotating magnetic-field structures extending corona, have drawn growing interest a possible means of efficient transfer. Despite its acknowledged importance, underlying physics tornadoes remains elusive. this study, we conduct three-dimensional radiative magnetohydrodynamic simulation that encompasses upper convective layer and extends into with view investigating how are generated efficiently transfer We find single event flux concentration merger on gives rise formation tornado. The Poynting transferred corona found be four times greater in presence tornado, compared absence. This increase attributed reduction loss chromosphere, resulting weakened magnetic-energy cascade. Based an evaluation fraction merging events, our results suggest contribute approximately 50% regions where strength 10 G. Potentially, contribution could even areas stronger field.

Language: Английский

Citations

13
Optimization of a centrifugal pump with high efficiency and low noise based on fast prediction method and vortex control DOI
Zhiyi Yuan, Yongxue Zhang, Wenbo Zhou

et al.

Energy, Journal Year: 2023, Volume and Issue: 289, P. 129835 - 129835

Published: Dec. 11, 2023

Language: Английский

Citations

12
Sound-vortex conversion on droplets: Kinematic model of sound activated vortices DOI
Hui Wang

Physics of Fluids, Journal Year: 2025, Volume and Issue: 37(1)

Published: Jan. 1, 2025

The rapid pace of urbanization across the globe has led to proliferation various urban infrastructure. They generate aerodynamic noise, posing significant challenges planning and residents' comfort. Despite Lighthill's mathematical analogy, current noise control applications rely heavily on wind tunnel tests computer simulations. Physical mechanisms behind aeroacoustic have yet be validated elucidated experimentally. This work observed geometry sound-activated vortices determined their streamline velocity distribution. theoretical results are consistent with experimental observations, offering a kinematic model for sound activated vortices. experimentally improves understanding provides development strategies.

Language: Английский

Citations

0
Photospheric Swirls in a Quiet-Sun Region DOI Creative Commons

Quan Xie,

Jiajia Liu, C. J. Nelson

et al.

The Astrophysical Journal, Journal Year: 2025, Volume and Issue: 979(1), P. 27 - 27

Published: Jan. 15, 2025

Abstract Swirl-shaped flow structures have been observed throughout the solar atmosphere, in both emission and absorption, at different altitudes locations, are believed to be associated with magnetic structures. However, distribution patterns of such swirls, especially their spatial positions, remain unclear. Using Automated Swirl Detection Algorithm, we identified swirls from high-resolution photospheric observations, centered on Fe i 630.25 nm, a quiet region near Sun's central meridian by Swedish 1-m Solar Telescope. Via detailed study locations detected small-scale an average radius ~300 km, found that most them located lanes between mesogranules (which diameter ~5.4 Mm) instead commonly intergranular lanes. The squared rotation, expansion/contraction vector speeds, proxy kinetic energy all follow Gaussian distributions. Their rotation speed, circulation positively correlated radius. All these results suggest scales across observational 56 . ″ 5 × 57 field view could share same triggering mechanism preferred scales. A comparison our previous work suggests number is local concentrations, stressing again close relation concentrations: should correlate strength concentrations.

Language: Английский

Citations

0
Crewed Venus Program for Interplanetary Discoveries (CVPID): A Space Mission Concept for the Exploration of Venus With Human Enabled Robotics DOI

Isra Bilal,

Thomas G. Butler,

Randi Byars

et al.

AIAA SCITECH 2022 Forum, Journal Year: 2025, Volume and Issue: unknown

Published: Jan. 3, 2025

Language: Английский

Citations

0
Seven decades of exploring planetary interiors with rotating convection experiments DOI Creative Commons
Alban Pothérat, Susanne Horn

Comptes Rendus Physique, Journal Year: 2025, Volume and Issue: 25(S3), P. 1 - 55

Published: Feb. 25, 2025

Language: Английский

Citations

0
Alfvén Pulse in a Chromospheric Magnetic Tube and Generation of the Super-Dreicer Electric Field DOI

N. A. Emelyanov,

Vl. V. Kocharovsky

Solar Physics, Journal Year: 2025, Volume and Issue: 300(3)

Published: March 1, 2025

Language: Английский

Citations

0
Effects of magnetic–vortical interactions on magnetic splitting DOI
Linlin Kang, Yanru Wang, Zhongzheng Jiang

et al.

Journal of Fluid Mechanics, Journal Year: 2025, Volume and Issue: 1009

Published: April 21, 2025

We propose an analytical approach based on the Frenet–Serret (FL) frame field, where FL and corresponding curvature torsion are defined at each point along magnetic field lines, to investigate evolution of tubes their interaction with vortex in magnetohydrodynamics. Within this framework, simplified expressions for Lorentz force, its curl, dynamics flux helicity derived. further perform direct numerical simulations linkage between effect initial angle $\theta$ , ranging from $0^{\,\circ}$ $45^{\,\circ}$ evolution. Our results show that non-zero generate forces, which turn produce dipole vortices. These vortices lead splitting into smaller structures, releasing energy. Both exhibit quasi-Lagrangian behaviour, maintaining similar shapes during consistent relative positions over time. A tube strength comparable tube, kinetic energy induced by is same order as can inhibit disrupting formation dipoles. Additionally, minor variations angular configuration significantly influence large-scale flow structures.

Language: Английский

Citations

0
Propagation of untwisting solar jets from the low-beta corona into the super-Alfvénic wind: testing a solar origin scenario for switchbacks DOI Creative Commons
J. Touresse, É. Pariat, C. Froment

et al.

Astronomy and Astrophysics, Journal Year: 2024, Volume and Issue: 692, P. A71 - A71

Published: Oct. 18, 2024

Parker Solar Probe's (PSP) discovery of the prevalence switchbacks (SBs), localised magnetic deflections in nascent solar wind, has sparked interest uncovering their origins. A prominent theory suggests these SBs originate lower corona through reconnection processes, closely linked to jet phenomena. Jets are impulsive events, observed across scales and atmosphere layers, associated with release twist helicity. This study examines whether self-consistent jets can form propagate into super-Alfv\'enic assesses impact distinct wind profiles on dynamics, determines if jet-induced untwisting waves display signatures typical SBs. We employed parametric 3D numerical MHD simulations using ARMS code model generation jets. Our focuses propagation atmospheric plasma $\beta$ Alfv\'en velocity profiles, including a wind. findings show that coronal Notable structures such as leading Alfv\'enic wave trailing dense-jet region were consistently diverse atmospheres. The dynamics significantly influenced by variations, changes affecting group ratio structures. U-loops, prevalent at onset, do not persist low-$\beta$ corona, but SB-like signatures. However, full-reversal observed. These may explain absence full reversal sub-Alfv\'enic illustrate jet-like shedding light possible SB formation processes.

Language: Английский

Citations

3