Coronal Heating Driven by a Magnetic Gradient Pumping Mechanism in Solar Plasmas

Tan, Baolin

doi:10.1088/0004-637x/795/2/140

Cited by 12 publications

(15 citation statements)

References 59 publications

(67 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The existence of Alfven waves is worthy of further research using detailed phase analysis for these magnetic perturbations. The observations seems also support magnetic gradient pumping (MGP) mechanism (Tan 2014). In the MGP mechanism, the magnetic gradient may drive the energetic particles to move upward from the underlying solar atmosphere and form hot upflows.…”

Section: Discussionsupporting

confidence: 59%

Observation of solar coronal heating powered by magneto-acoustic oscillations in a moss region

Hashim,

Hong,

et al. 2020

Preprint

View full text Add to dashboard Cite

In this paper, we report the observed temporal correlation between extremeviolet (EUV) emission and magneto-acoustic oscillations in a EUV moss region, which is the footpoint region only connected by magnetic loops with million-degree plasma. The result is obtained from a detailed multi-wavelength data analysis to the region with the purpose of resolving fine-scale mass and energy flows that come from the photosphere, pass through the chromosphere and finally heat solar transition region or the corona. The data set covers three atmospheric levels on the Sun, consisting of high-resolution broadband imaging at TiO 7057 Å and the line of sight magnetograms for the photosphere, high-resolution narrow-band images at Helium I 10830 Å for the chromosphere and EUV images at 171 Å for the corona. The 10830 Å narrow band images and the TiO 7057 Å broad-band images are from a much earlier observation on July 22, 2012 with the 1.6 meter aperture Goode Solar Telescope (GST) at Big Bear Solar Observatory (BBSO) and the EUV 171 Å images and the magnetograms are from observations made by Atmospheric Imaging Assembly (AIA) or Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO). We report following new phenomena: 1) Repeated injections of chromospheric material shown as 10830 Å absorption are squirted out from inter-granular lanes with the period of ∼ 5 minutes. 2) EUV emissions are found to be periodically modulated with the similar periods of ∼ 5 minutes. 3) Around the injection area where 10830 Å absorption is enhanced, both EUV emissions and the strength of magnetic field are remarkably stronger. 4) The peaks on the time profile of the EUV emissions are found to be in sync with oscillatory peaks of the stronger magnetic field in the region. These findings may give a series of strong evidences supporting the scenario that coronal heating is powered by magneto-acoustic waves.

show abstract

Section: Discussionsupporting

confidence: 59%

Observation of solar coronal heating powered by magneto-acoustic oscillations in a moss region

Hashim,

Hong,

et al. 2020

Preprint

View full text Add to dashboard Cite

show abstract

“…Therefore, we find further evidence supporting speculations that radiative to magnetic energy coupling descriptions possibly exhibit a wavelength dependence, particularly as such aligns with the recent numerical simulations of Equation 1 to cool main sequence stars by Alvarado-Gómez et al (2016), for EUV, soft X-ray, and X-ray portions of the spectrum. However, as additionally highlighted above, it can not be ruled out such observations could be suggestive of the presence of an additional plasma 2000); Pevtsov et al (2003) heating component, possibly married to the dominant mechanism (e.g., Tan 2014;Uritsky & Davila 2014).…”

Section: Magnetic Energy Redistributionmentioning

confidence: 95%

Solar Atmospheric Magnetic Energy Coupling: Broad Plasma Conditions and Spectrum Regimes

Orange¹,

Chesny

Gendre

et al. 2016

ApJ

View full text Add to dashboard Cite

Solar variability investigations that include magnetic energy coupling are paramount to solving many key solar/stellar physics problems, particularly for understanding the temporal variability of magnetic energy redistribution and heating processes. Using three years of observations from the Solar Dynamics Observatory's Atmospheric Imaging Assembly and Heliosemic Magnetic Imager; radiative and magnetic fluxes were measured from gross features and at full-disk scales, respectively. Magnetic energy coupling analyses support radiative flux descriptions via a plasma heating connectivity of dominant (magnetic) and diffuse components, specifically of the predominantly closed field corona. Our work shows that this relationship favors an energetic redistribution efficiency across large temperature gradients, and potentially sheds light on the long withstanding issue of diffuse unresolved low corona emission. The intimacy of magnetic energy redistribution and plasma conditions revealed by this work holds significant insight for the field of stellar physics, as we have provided possible means for probing distant sources in currently limited and/or undetectable radiation distributions.

show abstract

“…Therefore, there are magnetic gradients (∇B) in such plasma loops, and the direction of the gradient is always downward, as seen in Figure 1. According to the MGP mechanism [20,21], the upward magnetic-gradient force (F m = −µ∇B, here µ = 1 2 mv 2 t B is the magnetic moment) will drive energetic particles to move upward and form an energetic upflow in the plasma loop, extracting the energetic particles and kinetic energy from both footpoints of the loop and conveying and transporting them to accumulate around the looptop. At the same time, the deficit of energetic particles near both footpoints can be replenished by the convection motion of the hot plasmas in the solar interior.…”

Section: Transport and Accumulate Areas Of Coronal Plasma Loopsmentioning

confidence: 99%

“…Universe 2021, 7, 378 2 of 13 (2020) applied the magnetic-gradient pumping (MGP) mechanism [20] to demonstrate the evolution of flaring plasma loops [21]: the magnetic-gradient force may drive energetic particle upflow, which carries and conveys kinetic energy from the lower solar atmosphere with strong magnetic field to move upwards, accumulate and increase the temperature and plasma pressure around a looptop with relatively weak magnetic fields, produce plasma ballooning instability, and finally, trigger magnetic reconnection and the following violent flaring eruption.…”

Section: Introductionmentioning

confidence: 99%

The Early Evolution of Solar Flaring Plasma Loops

Tan

2021

Universe

Self Cite

View full text Add to dashboard Cite

Plasma loops are the elementary structures of solar flaring active regions and dominate the whole process of flaring eruptions. Standard flare models explain evolution and eruption after magnetic reconnection around the hot cusp-structure above the top of plasma loops very well; however, the early evolution of plasma loops before the onset of magnetic reconnection is poorly understood. Considering that magnetic gradients are ubiquitous in solar plasma loops, this work applies the magnetic-gradient pumping (MGP) mechanism to study the early evolution of flaring plasma loops. The results indicate that early evolution depends on the magnetic field distribution and the geometry of the plasma loops, which dominate the balance between the accumulation and dissipation of the energy around loop tops. Driven by MGP process, both of the density and temperature as well as the plasma β value around the looptop will increase in the early phase of the plasma loop’s evolution. In fact, the solar plasma loops will have two distinct evolutionary results: low, initially dense plasma loops with relatively strong magnetic fields tend to be stable for their maximum β value, which is always smaller than the critical value β<βc, while the higher, initially diluted solar plasma loops with relatively weak magnetic fields tend to be unstable for their β values, exceeding the critical value β>βc at a time of about one hour after the formation of the solar-magnetized plasma loop. The latter may produce ballooning instability and may finally trigger the following magnetic reconnection and eruptions. These physical scenarios may provide us with a new viewpoint to understand the nature and origin of solar flares.

show abstract

Coronal Heating Driven by a Magnetic Gradient Pumping Mechanism in Solar Plasmas

Cited by 12 publications

References 59 publications

Observation of solar coronal heating powered by magneto-acoustic oscillations in a moss region

Observation of solar coronal heating powered by magneto-acoustic oscillations in a moss region

Solar Atmospheric Magnetic Energy Coupling: Broad Plasma Conditions and Spectrum Regimes

The Early Evolution of Solar Flaring Plasma Loops

Contact Info

Product

Resources

About