A Study of Polar Jet Parameters Based on Hinode XRT Observations

Savcheva, Antonia; Cirtain, Jonathan; DeLuca, E. E.; Lundquist, L. L.; Golub, L.; Weber, Mark; Shimojo, Masataka; Shibasaki, Κ.; Sakao, Taro; Narukage, Noriyuki; Tsuneta, S.; Kano, Ryouhei

doi:10.1093/pasj/59.sp3.s771

Cited by 184 publications

(206 citation statements)

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“…This is consistent with the maximum apparent jet flow speeds reported by Shimojo et al (1996) and Savcheva et al (2007). Typical velocities within our main curtain-like spray were somewhat lower, with dimensionless values 0.3 » , scaling to 3 10 7 cm s −1 .…”

Section: ( ) »´-supporting

confidence: 90%

“…Typical velocities within our main curtain-like spray were somewhat lower, with dimensionless values 0.3 » , scaling to 3 10 7 cm s −1 . This falls within the ranges of velocities reported by Shimojo et al (1996) and Savcheva et al (2007), and is consistent with the jet speeds reported by Shibata et al (1992) Table 1 for the typical jet duration, peak kinetic energy, and peak reconnection rate we obtain, respectively, The duration of our quiet Sun jet is roughly the mean of the large range of jet lifetimes reported by Shimojo et al (1996) ( 2 10 2 »´-2 10 4 s) and is at the high end of the range reported by Savcheva et al (2007) ( 2 10 2 »´-2 10 3 s). Its kinetic energy is near the upper end of the range reported by Shibata et al (1992) ( 1 10 28 »´erg).…”

Section: ( ) »´-supporting

confidence: 90%

“…The strengths of the coronal-loop (B cl ) and parasitic-polarity (B pp ) fields then are Y =´. For the typical jet duration, peak kinetic energy, and peak reconnection rate we obtain, respectively, The duration of our active-region jet is at the low end of the range of jet lifetimes reported by Shimojo et al (1996) and Savcheva et al (2007), and somewhat shorter than the observed jet shown in Figure 1. Its kinetic energy is near the mean of the range reported by Shibata et al (1992) ( 1 10 25 »´-1 10 28 erg).…”

Section: ( ) »´-mentioning

confidence: 50%

“…Cool surges and hot jets are sometimes observed together, in close association in space and time (Canfield et al 1996). Subsequent improvements in the spatial resolutions and temporal cadences of space-borne instruments have enabled more detailed studies of jets and surges from the Solar and Heliospheric Observatory (SOHO; e.g., Wang et al 1998), the Transition Region and Coronal Explorer (e.g., Chae et al 1999), the Solar-Terrestrial Relations Observatory (e.g., Patsourakos et al 2008), Hinode (e.g., Cirtain et al 2007;Savcheva et al 2007;Nishizuka et al 2008;Török et al 2009;Moore et al 2010Moore et al , 2013Liu et al 2011), the Solar Dynamics Observatory (SDO; e.g., Shen et al 2011;Guo et al 2013;Lee et al 2013;Schmieder et al 2013;Zheng et al 2013), and the Interface Region Imaging Spectrograph (e.g., Tian et al 2014;Cheung et al 2015).…”

Section: Introductionmentioning

confidence: 99%

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Simulations of Solar Jets Confined by Coronal Loops

Wyper

DeVore

2016

ApJ

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Coronal jets are collimated, dynamic events that occur over a broad range of spatial scales in the solar corona. In the open magnetic field of coronal holes, jets form quasi-radial spires that can extend far out into the heliosphere, while in closed-field regions the jet outflows are confined to the corona. We explore the application of the embedded-bipole model to jets occurring in closed coronal loops. In this model, magnetic free energy is injected slowly by footpoint motions that introduce twist within the closed dome of the jet source region, and is released rapidly by the onset of an ideal kink-like instability. Two length scales characterize the system: the width (N) of the jet source region and the footpoint separation (L) of the coronal loop that envelops the jet source. We find that both the conditions for initiation and the subsequent dynamics are highly sensitive to the ratio L/N. The longest-lasting and most energetic jets occur along long coronal loops with large L/N ratios, and share many of the features of open-field jets, while smaller L/N ratios produce shorter-duration, less energetic jets that are affected by reflections from the far-loop footpoint. We quantify the transition between these behaviors and show that our model replicates key qualitative and quantitative aspects of both quiet Sun and active-region loop jets. We also find that the reconnection between the closed dome and surrounding coronal loop is very extensive: the cumulative reconnected flux at least matches the total flux beneath the dome for small L/N, and is more than double that value for large L/N.

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Section: ( ) »´-supporting

confidence: 90%

Section: ( ) »´-supporting

confidence: 90%

Section: ( ) »´-mentioning

confidence: 50%

Section: Introductionmentioning

confidence: 99%

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Simulations of Solar Jets Confined by Coronal Loops

Wyper

DeVore

2016

ApJ

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“…Recent observations by the X-ray Telescope (XRT; Golub et al 2007) on board Hinode (Kosugi et al 2007) revealed the dynamic behavior of jets in polar coronal holes (Savcheva et al 2007;Shimojo et al 2007). Detailed analysis of XRT observations in coronal holes indicated that X-ray jets occurred with a high frequency of 60 events per day.…”

Section: Introductionmentioning

confidence: 99%

Distribution of jets and magnetic fields in a coronal hole

Kamio

Hara

Watanabe

et al. 2009

A&A

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Context. Recent observations of ubiquitous jets in coronal holes suggest that they play an important role in coronal heating and solar wind acceleration. Aims. The aim of our study is to understand the magnetic connectivity and the formation of jets in coronal holes. The study of jets also helps to understand the magnetic field configuration in the coronal hole. Methods. A coordinated observation between EIS and SUMER was carried out in a polar coronal hole to investigate both the transition region and the corona. Spectropolarimeter (SP) data allowed us to examine the relationship between the distribution of jets and magnetic fields in the photosphere. Results. Coronal jets as well as explosive events and cool upflows were identified from EIS and SUMER data. The location of these events are correlated with network fields in the photosphere. Conclusions. Footpoints of coronal jets are connected to patches of vertical kG fields in the photosphere, which are thought to anchor open fields in the upper corona. Explosive events and cool upflows occur in network regions which harbor low-lying fields in the transition region.

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A 17 June 2011 polar jet and its presence in the background solar wind

Jackson

Yang

et al. 2016

JGR Space Physics

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High‐speed jet responses in the polar solar wind are enigmatic. Here we measure a jet response that emanates from the southern polar coronal hole on 17 June 2011 at the extreme speed of over 1200 km/s. This response was recorded from the Sun‐Earth line in Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) and Large Angle and Spectrometric Coronagraph/C2 and both Solar TErrestrial RElations Observatory Extreme Ultraviolet Imager and COR2 coronagraphs when the three spacecraft were situated ~90° from one another. These certify the coronal 3‐D location of the response that is associated with an existing solar plume structure and show its high speed to distances of over 14 RS. This jetting is associated with magnetic flux changes in the polar region as measured by the SDO/Helioseismic and Magnetic Imager instrumentation over a period of several hours. The fastest coronal response observed can be tracked to a time near the period of greatest flux changes and to the onset of the brightest flaring in AIA. This high‐speed response can be tracked directly as a small patch of outward moving brightness in coronal images as in Yu et al. (2014) where three slower events were followed from the perspective of Earth. This accumulated jet response has the largest mass and energy we have yet seen in 3‐D reconstructions from Solar Mass Ejection Imager observations, and its outward motion is certified for the first time using interplanetary scintillation observations. This jet response is surrounded by similar high‐speed patches, but these are smoothed out in Ulysses polar measurements, we speculate about how these dynamic activities relate to solar wind acceleration.

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A Study of Polar Jet Parameters Based on Hinode XRT Observations

Cited by 184 publications

References 9 publications

Simulations of Solar Jets Confined by Coronal Loops

Simulations of Solar Jets Confined by Coronal Loops

Distribution of jets and magnetic fields in a coronal hole

A 17 June 2011 polar jet and its presence in the background solar wind

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