Observation and Modeling of Solar Jets

Shen, Yuandeng

doi:10.48550/arxiv.2101.04846

Cited by 2 publications

(3 citation statements)

References 306 publications

(534 reference statements)

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“…Some of the bright points are accompanied by upsurges of plasma (i.e., jets Raouafi et al 2016;Shen 2021), which are illustrated more clearly by the synthetic AIA images from the side view in Figure 3. This is similar to the relation between coronal jets and bright points found in observations (see e.g., Doschek et al 2010;Zhang et al 2016;Mou et al 2018;Panesar et al 2020, and references therein).…”

Section: Bright Points Jets and Campfiresmentioning

confidence: 93%

“…This figure is also a frame of the animation showing the temporal evolution during this time period. Jets are ubiquitously observed on the Sun from the chromosphere to the corona (Raouafi et al 2016;Shen 2021). An intriguing event seen during this period is a fast propagating jet coming out from the core of the active region.…”

Section: Euv Emission Above Developed Active Regionsmentioning

confidence: 99%

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A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona

Chen¹,

Rempel²,

Fan

2021

Preprint

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We present a comprehensive radiative magnetohydrodynamic simulation of the quiet Sun and large solar active regions. The 197 Mm wide simulation domain spans from the uppermost convection zone to over 100 Mm in the solar corona. Sophisticated treatments of radiative transfer and conduction transport provide the necessary realism for synthesizing observables to compare with remote sensing observations of the Sun. This model self-consistently reproduces observed features of the quiet Sun, emerging and developed active regions, and solar flares up to M class. Here, we report an overview on the first results. The surface magnetoconvection yields an upward Poynting flux that is dissipated in the corona and heats the plasma to over one million K. The quiescent corona also presents ubiquitous propagating waves, jets, and bright points with sizes down to 2 Mm. Magnetic flux bundles generated in a solar convective dynamo emerge into the photosphere and gives rise to strong and complex active regions with Over 10 23 Mx magnetic flux. The coronal free magnetic energy, which is about 18% of the total magnetic energy, accumulates to about 10 33 erg. The coronal magnetic field is not forcefree, as the Lorentz force needs to balance the pressure force and viscous stress as well as to drive magnetic field evolution. Emission measure from log 10 T = 4.5 to log 10 T > 7 provides a comprehensive view on structures and dynamics in the active region corona, such as coronal loops in various lengths and temperatures, mass circulation by evaporation and condensation, and eruptions from jets to large-scale mass ejections.

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Section: Bright Points Jets and Campfiresmentioning

confidence: 93%

Section: Euv Emission Above Developed Active Regionsmentioning

confidence: 99%

A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona

Chen¹,

Rempel²,

Fan

2021

Preprint

View full text Add to dashboard Cite

show abstract

“…Small-scale jets with lower energy budgets and shorter lifetimes include spicules (De Pontieu et al 2004;Samanta et al 2019), chromospheric jets (Shibata et al 2007;Liu et al 2009;Tian et al 2014a), bidirectional plasma jets related to explosive events (Innes et al 1997;Li et al 2018a), coronal nanojets (Antolin et al 2020) and mini-jets . Large-scale jets with higher energy budgets and longer lifetimes include Hα surges (Schmieder et al 1995;Liu & Kurokawa 2004) and coronal jets (Cirtain et al 2007;Savcheva et al 2007;Shimojo et al 2007;Raouafi et al 2016;Shen 2021). Coronal jets are transient collimated outflows propagating along open magnetic field or large-scale closed loops (Shibata et al 1992(Shibata et al , 1994Zhang et al 2012;Huang et al 2012Huang et al , 2020.…”

Section: Introductionmentioning

confidence: 99%

Spectroscopic observations of a flare-related coronal jet

Zhang,

Huang,

Hou

et al. 2021

Preprint

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Context. Coronal jets are ubiquitous in active regions (ARs) and coronal holes. Aims. In this paper, we study a coronal jet related to a C3.4 circular-ribbon flare in active region 12434 on 2015 October 16. Methods. The flare and jet were observed in ultraviolet (UV) and extreme ultraviolet (EUV) wavelengths by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). The line-of-sight (LOS) magnetograms of the photosphere were observed by the Helioseismic and Magnetic Imager (HMI) on board SDO. The whole event was covered by the Interface Region Imaging Spectrograph (IRIS) during its imaging and spectroscopic observations. Soft X-ray (SXR) fluxes of the flare were recorded by the GOES spacecraft. Hard X-ray (HXR) fluxes at 4−50 keV were obtained from observations of RHESSI and Fermi. Radio dynamic spectra of the flare were recorded by the ground-based stations belonging to the e-Callisto network. Results. Two minifilaments were located under a 3D fan-spine structure before flare. The flare was generated by the eruption of one filament. The kinetic evolution of the jet was divided into two phases: a slow rise phase at a speed of ∼131 km s −1 and a fast rise phase at a speed of ∼363 km s −1 in the plane-of-sky. The slow rise phase may correspond to the impulsive reconnection at the breakout current sheet. The fast rise phase may correspond to magnetic reconnection at the flare current sheet. The transition between the two phases occurred at ∼09:00:40 UT. The blueshifted Doppler velocities of the jet in the Si iv 1402.80 Å line range from -34 to -120 km s −1 . The accelerated high-energy electrons are composed of three groups. Those propagating upward along open field generate type III radio bursts, while those propagating downward produce HXR emissions and drive chromospheric condensation observed in the Si iv line. The electrons trapped in the rising filament generate a microwave burst lasting for ≤40 s. Bidirectional outflows at the base of jet are manifested by significant line broadenings of the Si iv line. The blueshifted Doppler velocities of outflows range from -13 to -101 km s −1 . The redshifted Doppler velocities of outflows range from ∼17 to ∼170 km s −1 . Conclusions. Our multiwavelength observations of the flare-related jet are in favor of the breakout jet model and are important for understanding the acceleration and transport of nonthermal electrons.

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Observation and Modeling of Solar Jets

Cited by 2 publications

References 306 publications

A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona

A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona

Spectroscopic observations of a flare-related coronal jet

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