FLARE-ASSOCIATED TYPE III RADIO BURSTS AND DYNAMICS OF THE EUV JET FROM SDO/AIA AND<i>RHESSI</i>OBSERVATIONS

Chen, Naihwa; Ip, W.-H.; Innes, D. E.

doi:10.1088/0004-637x/769/2/96

Cited by 26 publications

(31 citation statements)

References 27 publications

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“…in the photosphere (Hα, Ca II K surges), chromosphere (UV), transition region (EUV) and corona (X-ray). Jets can occur in different environments such as coronal holes (CHs; Young & Muglach 2014a,b), and active regions (ARs; Innes et al 2011;Chen et al 2013;Schmieder et al 2013;Chandra et al 2015), where they have different manifestations.…”

Section: Introductionmentioning

confidence: 99%

“…The statistical study of X-ray jets (Shimojo et al 1996) observed by Soft X-ray Telescope (SXT; Tsuneta et al 1991) onboard Yohkoh (Ogawara et al 1991) Movies are available in electronic form at http://www.aanda.org showed that jets most often occur in the western periphery of the leading spot. Other high-resolution observations showed that jets that occur at the periphery of the active regions/sunspots are mostly associated with a nonthermal type-III radio burst which is known to be produced by energetic electrons that gyrate along the open magnetic field lines (Kundu et al 1995;Raulin et al 1996;Innes et al 2011;Chen et al 2013;Chandra et al 2015). Also, it has been observed that the accelerated electrons which have access to open field lines produce impulsive, electron/ 3 He-rich solar energetic particle (SEP) events in the interplanetary medium (Nitta et al 2008;Wang et al 2006) and the accelerated electrons which are trapped in closed field lines travel downwards, lose their energies owing to collision, and produce hard X-ray emission (HXR; Glesener et al 2012;Chen et al 2013).…”

Section: Introductionmentioning

confidence: 99%

“…The temperatures of jets have been studied by using two techniques that are based on different approaches -the filter-ratio method which assumes a single temperature along the line of sight (LOS; e.g., Shimojo & Shibata 2000;Nisticò et al 2011;Madjarska 2011;Madjarska et al 2012;Matsui et al 2012;Pucci et al 2013;Young & Muglach 2014a) and the differential emission measure (DEM) method which assumes a multi-thermal plasma along the LOS (e.g., Doschek et al 2010;Chandrashekhar et al 2014;Kayshap et al 2013;Chen et al 2013;Sun et al 2014). Nisticò et al (2011) report the temperature of CH jets as ranging from 0.8 to 1.3 MK using the filter-ratio method applied to STEREO/SECCHI data; whereas Pucci et al (2013) find the temperature of the jet to be 1.7 MK.…”

Section: Introductionmentioning

confidence: 99%

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Multiwavelength study of 20 jets that emanate from the periphery of active regions

Mulay

Tripathi

Zanna

et al. 2016

A&A

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Aims. We present a multiwavelength analysis of 20 EUV jets which occurred at the periphery of active regions close to sunspots. We discuss the physical parameters of the jets and their relation with other phenomena such as Hα surges, nonthermal type-III radio bursts and hard X-ray (HXR) emission. Methods. These jets were observed between August 2010 and June 2013 by the Atmospheric Imaging Assembly (AIA) instrument that is onboard the Solar Dynamic Observatory (SDO). We selected events that were observed on the solar disk within +/-60• latitude. Using AIA wavelength channels that are sensitive to coronal temperatures, we studied the temperature distribution in the jets using the line of sight (LOS) differential emission measure (DEM) technique. We also investigated the role of the photospheric magnetic field using the LOS magnetogram data from the Helioseismic and Magnetic Imager (HMI) onboard SDO. Results. It has been observed that most of the jets originated from the western periphery of active regions. Their lifetimes range from 5 to 39 min with an average of 18 min and their velocities range from 87 to 532 km s −1 with an average of 271 km s −1 . All the jets are co-temporally associated with Hα surges. Most of the jets are co-temporal with nonthermal type-III radio bursts observed by the Wind/WAVES spacecraft in the frequency range from 20 kHz to 13 MHz. We confirm the source region of these bursts using the potential field source surface (PFSS) technique. Using Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) observations, we found that half of the jets produced HXR emission and they often shared the same source region as the HXR emission (6−12 keV). Ten out of 20 events showed that the jets originated in a region of flux cancellation and six jets in a region of flux emergence. Four events showed flux emergence and then cancellation during the jet evolution. DEM analyses showed that for most of the spires of the jets, the DEM peaked at around log T [K] = 6.2/6.3 (∼2 MK). In addition, we derived an emission measure and a lower limit of electron density at the location of the spire (jet 1: log EM = 28.6, N e = 1.3 × 10 10 cm −3 ; jet 2: log EM = 28.0, N e = 8.6 × 10 9 cm −3 ) and the footpoint (jet 1 -log EM = 28.6, N e = 1.1 × 10 10 cm −3 ; jet 2: log EM = 28.1, N e = 8.4 × 10 9 cm −3 ). These results are in agreement with those obtained earlier by studying individual active region jets. Conclusions. The observation of flux cancellation, the association with HXR emission and emission of nonthermal type-III radio bursts, suggest that the initiation and therefore, heating is taking place at the base of the jet. This is also supported by the high temperature plasma revealed by the DEM analysis in the jet footpoint (peak in the DEM at log T [K] = 6.5). Our results provide substantial constraints for theoretical modeling of the jets and their thermodynamic nature.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Multiwavelength study of 20 jets that emanate from the periphery of active regions

Mulay

Tripathi

Zanna

et al. 2016

A&A

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“…The calculated temperature may represent the average temperature of the plasmas along the LOS. The other method is differential emission measure (DEM) based on the multi-thermal nature of the plasmas along the LOS (Doschek et al 2010;Chandrashekhar 2014b;Kayshap et al 2013;Chen et al 2013;Sun et al 2014b), which is more realistic and reasonable. Occasionally, hard X-ray (HXR) sources could be detected at the bottom of jets, and the hot thermal component could be isolated during the fittings to perform temperature diagnostic (Bain & Fletcher 2009;Krucker et al 2011;Glesener et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Blobs in recurring extreme-ultraviolet jets

Zhang

2014

A&A

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Context. Coronal jets are one type of ubiquitous small-scale activity that is caused by magnetic reconnection in the solar corona. They are often associated with cool surges in the chromosphere. Aims. In this paper, we report our discovery of blobs in the recurrent and homologous jets that occurred at the western edge of the NOAA active region 11259 on 2011 July 22. Methods. The jets were observed in the seven extreme-ultraviolet (EUV) filters of the Atmospheric Imaging Assembly instrument aboard the Solar Dynamics Observatory. Using the base-difference images of the six filters (94, 131, 171, 211, 193, and 335 Å), we carried out the differential emission measure (DEM) analyses to explore the thermodynamic evolutions of the jets. The jets were accompanied by cool surges observed in the Hα line center of the ground-based telescope in the Big Bear Solar Observatory. Results. The jets that had lifetimes of 20−30 min recurred at the same place for three times with an interval of 40−45 min. Interestingly, each of the jets intermittently experienced several upward eruptions at the speed of 120−450 km s −1 . After reaching the maximum heights, they returned back to the solar surface, showing near-parabolic trajectories. The falling phases were more evident in the low-T filters than in the high-T filters, indicating that the jets experienced cooling after the onset of eruptions. We identified bright and compact blobs in the jets during their rising phases. The simultaneous presence of blobs in all the EUV filters were consistent with the broad ranges of the DEM profiles of the blobs (5.5 ≤ log T ≤ 7.5), indicating their multi-thermal nature. The median temperatures of the blobs were ∼2.3 MK. The blobs that were ∼3 Mm in diameter had lifetimes of 24−60 s. Conclusions. To our knowledge, this is the first report of blobs in coronal jets. We propose that these blobs are plasmoids created by the magnetic reconnection as a result of tearing-mode instability and are ejected out along the jets.

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“…Many papers report a significant delay between jet formation and flux emergence in contrast to recent 3D Early observations of X-ray jets associated with bursts of metric radio emission implied that the jet mechanism was able to accelerate sub-relativistic electrons along dense corona structures (Aurass et al 1994;Kundu et al 1995;Raulin et al 1996). Further confirmation came from observations of jets which were co-incident with hard X-rays from their footpoints (Chen et al 2013;Krucker et al 2011;Nitta 1997;Nitta et al 2008) and from the jet itself (Bain & Fletcher 2009;Glesener et al 2012).…”

Section: Introductionmentioning

confidence: 98%

Observations of solar X‐ray and EUV jets and their related phenomena

et al. 2016

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Solar jets are fast‐moving, elongated brightenings related to ejections seen in both images and spectra on all scales from barely visible chromospheric jets to coronal jets extending up to a few solar radii. The largest, most powerful jets are the source of type III radio bursts, energetic electrons and ions with greatly enhanced 3He and heavy element abundances. The frequent coronal jets from polar and equatorial coronal holes may contribute to the solar wind. The primary acceleration mechanism for all jets is believed to be release of magnetic stress via reconnection; however the energy buildup depends on the jets' source environment. In this review, we discuss how certain features of X‐ray and EUV jets, such as their repetition rate and association with radio emission, depends on their underlying photospheric field configurations (active regions, polar and equatorial coronal holes, and quiet Sun). (© 2016 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)

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FLARE-ASSOCIATED TYPE III RADIO BURSTS AND DYNAMICS OF THE EUV JET FROM SDO/AIA ANDRHESSIOBSERVATIONS

Cited by 26 publications

References 27 publications

Multiwavelength study of 20 jets that emanate from the periphery of active regions

Multiwavelength study of 20 jets that emanate from the periphery of active regions

Blobs in recurring extreme-ultraviolet jets

Observations of solar X‐ray and EUV jets and their related phenomena

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