THE THREE-DIMENSIONAL ANALYSIS OF<i>HINODE</i>POLAR JETS USING IMAGES FROM LASCO C2, THE<i>STEREO</i>COR2 CORONAGRAPHS, AND SMEI

Yu, Hsiu-Shan; Jackson, B. V.; Buffington, A.; Hick, P. P.; Shimojo, Masataka; Sako, N.

doi:10.1088/0004-637x/784/2/166

Cited by 33 publications

(47 citation statements)

References 43 publications

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“…Moore et al (2011) argue, however, that if spicules are driven by the same processes that drive coronal jets, then, owing to the abundance of spicules, the sum of the energies of coronal jets and those of spicules might be sufficient for powering the corona. Our results also agree with recent work by Yu et al (2014), who estimated the contribution of coronal jets to the solar wind energy…”

Section: Summary and Discussionsupporting

confidence: 93%

Physical properties of solar polar jets

Paraschiv

Бемпорад

Sterling

2015

A&A

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Aims. The target of this work is to investigate the physical nature of polar jets in the solar corona and their possible contribution to coronal heating and solar wind flow based on the analysis of X-ray images acquired by the Hinode XRT telescope. We estimate the different forms of energy associated with many of these small-scale eruptions, in particular the kinetic energy and enthalpy. Methods. Two Hinode XRT campaign datasets focusing on the two polar coronal holes were selected to analyze the physical properties of coronal jets; the analyzed data were acquired using a series of three XRT filters. Typical kinematical properties (e.g., length, thickness, lifetime, ejection rate, and velocity) of 18 jets are evaluated from the observed sequences, thus providing information on their possible contribution to the fast solar wind flux escaping from coronal holes. Electron temperatures and densities of polar-jet plasmas are also estimated using ratios of the intensities observed in different filters. Results. We find that the largest amount of energy eventually provided to the corona is thermal. The energy due to waves may also be significant, but its value is comparatively uncertain. The kinetic energy is lower than thermal energy, while other forms of energy are comparatively low. Lesser and fainter events seem to be hotter, thus the total contribution by polar jets to the coronal heating could have been underestimated so far. The kinetic energy flux is usually around three times smaller than the enthalpy counterpart, implying that this energy is converted into plasma heating more than in plasma acceleration. This result suggests that the majority of polar jets are most likely not escaping from the Sun and that only cooler ejections could possibly have enough kinetic energy to contribute to the total solar wind flow.

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Section: Summary and Discussionsupporting

confidence: 93%

Physical properties of solar polar jets

Paraschiv

Бемпорад

Sterling

2015

A&A

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“…M equals the order-of-magnitude estimate obtained from UVCS observations at 1.7 R ⊙ by Corti et al (2007). In contrast, both M and E are about one order of magnitude smaller than the mass and kinetic energy estimated by Yu et al (2014).…”

Section: Total Mass and Energy And Comparison To Observationsmentioning

confidence: 57%

“…These are only ∼ 1/10 of the heliospheric mass and kinetic energy estimates by Yu et al (2014), but those authors considered three of the largest jets during a three-week Hinode campaign (Sako et al 2013). On the other hand, M agrees with the order-of-magnitude estimate by Corti et al (2007) obtained at r = 1.7 R ⊙ .…”

Section: Discussionmentioning

confidence: 99%

“…Coronagraph and in-situ observations revealed that coronal jets can produce signatures in the outer corona, sometimes even at Earth or beyond (St. Cyr et al 1997;Wang et al 1998;Wood et al 1999;Corti et al 2007;Neugebauer 2012;Janvier et al 2014;Yu et al 2014). It was therefore suggested that they contribute to powering the corona and solar wind (e.g., Shibata et al 2007;Cirtain et al 2007).…”

Section: Introductionmentioning

confidence: 99%

“…Pucci et al (2013) obtained a "crude estimate" for the energy budget of coronal jets, which was ∼ 10 4 times smaller than required for maintaining the SW. Cirtain et al (2007) suggested a masscontribution of coronal jets to the SW of ≈10 %, though Young (2015) remarked that this value should be 2.5 times smaller. Using heliospheric images from SMEI (Jackson et al 2004), Yu et al (2014) estimated mass and energy contributions of 3.2 % and 1.6 %, respectively. Finally, Paraschiv et al (2015) estimated the energy provided by coronal jets to be less than 1 % of what is required to heat a polar coronal hole.…”

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confidence: 99%

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The Contribution of Coronal Jets to the Solar Wind

Lionello

Török

Titov

et al. 2016

ApJL

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Transient collimated plasma eruptions in the solar corona, commonly known as coronal (or X-ray) jets, are among the most interesting manifestations of solar activity. It has been suggested that these events contribute to the mass and energy content of the corona and solar wind, but the extent of these contributions remains uncertain. We have recently modeled the formation and evolution of coronal jets using a three-dimensional (3D) magnetohydrodynamic (MHD) code with thermodynamics in a large spherical domain that includes the solar wind. Our model is coupled to 3D MHD flux-emergence simulations, i.e, we use boundary conditions provided by such simulations to drive a time-dependent coronal evolution. The model includes parametric coronal heating, radiative losses, and thermal conduction, which enables us to simulate the dynamics and plasma properties of coronal jets in a more realistic manner than done so far. Here we employ these simulations to calculate the amount of mass and energy transported by coronal jets into the outer corona and inner heliosphere. Based on observed jet-occurrence rates, we then estimate the total contribution of coronal jets to the mass and energy content of the solar wind to (0.4 − 3.0) % and (0.3-1.0) %, respectively. Our results are largely consistent with the few previous rough estimates obtained from observations, supporting the conjecture that coronal jets provide only a small amount of mass and energy to the solar wind. We emphasize, however, that more advanced observations and simulations are needed to substantiate this conjecture.

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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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THE THREE-DIMENSIONAL ANALYSIS OFHINODEPOLAR JETS USING IMAGES FROM LASCO C2, THESTEREOCOR2 CORONAGRAPHS, AND SMEI

Cited by 33 publications

References 43 publications

Physical properties of solar polar jets

Physical properties of solar polar jets

The Contribution of Coronal Jets to the Solar Wind

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

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