Observation of Magnetic Reconnection Driven by Granular Scale Advection

Zeng, Zhicheng; Cao, Wenda; Ji, Haisheng

doi:10.1088/2041-8205/769/2/l33

Cited by 16 publications

(14 citation statements)

References 20 publications

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“…We can trace their roots directly to the underlying photosphere and its magnetic field. With the help from the He I 10830 Å data and simultaneous high-resolution images of the photosphere, we report that these microeruptions are rooted in the area of intergranular lanes, which confirms previous results (Ji et al 2012;Zeng et al 2013;Wang et al 2021). Furthermore, they are situated on magnetic polarity inversion lines (PILs).…”

Section: Discussionsupporting

confidence: 89%

“…For a microeruption such as any of those in the present paper, a dark microeruption with or without a discernible microjet spire in He I 10830 Å images, high-resolution Hα or EUV images along with high-resolution magnetograms are needed to decide whether the microeruption is the product of a microfilament eruption. Aslo, many other works have been reported regarding how magnetic flux emergences and cancellations induce various recurring jets (e.g., Chae et al 1999;Zhang & Ji 2014;Liu et al 2016;Chifor et al 2008;Zeng et al 2013, for a more comprehensive review, see Raouafi et al 2016). Therefore, our observation supports the magnetic reconnection scenario for the two microjets.…”

Section: Discussionsupporting

confidence: 85%

“…• Zeng et al (2013) reported the association of a He I 10830 Å surge with the magnetic reconnection driven by advection of a rapidly developing large granule.…”

Section: Introductionmentioning

confidence: 99%

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Quasi-periodic microjets driven by granular advection as observed with high-resolution imaging at He I 10830 Å

Hong,

Wang,

2022

Preprint

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With high-resolution narrowband He I 10830 Å filtergrams from GST, we give an extensive analysis for 4 granular sized microeruptions which appear as the gentle ejection of material in He I 10830 Å band. The analysis was aided with the EUV data from AIA and line-of-sight magnetograms from HMI on board SDO. The microeruptions are situated on magnetic polarity inversion lines (PILs), and their roots are accurately traced down to intergranular lanes. Their durations are different, two microeruptions are repetitive microjets, lasting ∼ 50 and 27 minutes respectively, while the other two events are singular, lasting ∼ 5 minutes. For the two microjets, they are continuous and recurrent in He I 10830 Å band, and the recurrence is quasi-periodic with the period of ∼ 5 minutes. We found that only transient co-spatial EUV brightenings are observed for the longer duration microjets and EUV brightenings are absent for the two singular microeruptions. What is essential to the longer duration microjets is that granules with the concentration of positive magnetic field persistently transport the magnetic field to the PILs, canceling the opposite magnetic flux and making the base of the two microjets and the underlying granules migrate with the speed of ∼ 0.25 and 1.0 km s −1 . The observations support the scenario of magnetic reconnection for the quasi-periodic microjets and further show that the reconnection continuously generates multi-temperature components, especially the cool component with chromospheric temperature. In addition, the ongoing reconnection is modulated by p-mode oscillations inside the Sun.

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Section: Discussionsupporting

confidence: 89%

Section: Discussionsupporting

confidence: 85%

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Quasi-periodic microjets driven by granular advection as observed with high-resolution imaging at He I 10830 Å

Hong,

Wang,

2022

Preprint

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“…The observations have revealed the smallest scale magnetic activities in inter-granular lanes of the photosphere with their brightening going up into the local transition region. The finding was confirmed by further analysis to the same data set or similar observations (Zeng et al 2013;Hong et al 2017;Yang et al 2019). In the most recent work, Ji et al (2020) reported a possible correlation between the perturbations of magnetic field and He I 10830 Å absorption, both have a quasi-periodic nature.…”

Section: Introductionsupporting

confidence: 78%

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

Hashim,

Hong,

et al. 2020

Preprint

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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.

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“…During the past few years, NST studies have focused on fast imaging (no polarimetry yet in the following science highlights). For example, they studied rather rare three-ribbon flares (Wang et al 2014), sunspot oscillations (Yurchyshyn et al 2015), flux emergence coupled with a jet (Zeng et al 2013;Vargas Domínguez et al 2014), the eruption of a flux rope (Wang et al 2015), and the connection between small-scale events in the photosphere and subsequent coronal emission . From observations of a C-flare, Zeng et al (2014) concluded that the He 1083 nm triplet is formed primarily by photoionization of chromospheric plasma followed by radiative recombination.…”

Section: Its Instrumentation Consists Of Fast Imaging (Eg Broadbandmentioning

confidence: 99%

Prospects of Solar Magnetometry—From Ground and in Space

Kleint¹,

Gandorfer²

2015

Space Sci Rev

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In this review we present an overview of observing facilities for solar research, which are planned or will come to operation in near future. We concentrate on facilities, which harbor specific potential for solar magnetometry. We describe the challenges and science goals of future magnetic measurements, the status of magnetic field measurements at different major solar observatories, and provide an outlook on possible upgrades of future instrumentation.

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Observation of Magnetic Reconnection Driven by Granular Scale Advection

Cited by 16 publications

References 20 publications

Quasi-periodic microjets driven by granular advection as observed with high-resolution imaging at He I 10830 Å

Quasi-periodic microjets driven by granular advection as observed with high-resolution imaging at He I 10830 Å

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

Prospects of Solar Magnetometry—From Ground and in Space

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