Evidence for Alfvén Waves in Solar X-ray Jets

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

doi:10.1126/science.1147050

Cited by 418 publications

(403 citation statements)

References 11 publications

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“…Over the about 20 years since the model was proposed, the quality of coronal observations has enormously improved and we may ask what the new data added to our knowledge of plume development. A phenomenon that emerged from HINODE XRT (Kano et al, 2004) observations is an unpredicted high frequency of polar X-ray jets (Cirtain et al, 2007): these phenomena share some properties with plumes, as they are transient, originate because of flux emergence, and are seen at network boundaries. Opposite to the fuzzy appearance of plumes, they look as collimated, sharp edged, plasma beams: however, we do not know whether the plume haziness is real or it is a consequence of an inadequate low spatial resolution and background effects.…”

Section: The Birth Of Plumesmentioning

confidence: 99%

Solar Coronal Plumes

Poletto

2015

Living Rev. Sol. Phys.

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Polar plumes are thin long ray-like structures that project beyond the limb of the Sun polar regions, maintaining their identity over distances of several solar radii. Plumes have been first observed in white-light (WL) images of the Sun, but, with the advent of the space era, they have been identified also in X-ray and UV wavelengths (XUV) and, possibly, even in in situ data. This review traces the history of plumes, from the time they have been first imaged, to the complex means by which nowadays we attempt to reconstruct their 3-D structure. Spectroscopic techniques allowed us also to infer the physical parameters of plumes and estimate their electron and kinetic temperatures and their densities. However, perhaps the most interesting problem we need to solve is the role they cover in the solar wind origin and acceleration: Does the solar wind emanate from plumes or from the ambient coronal hole wherein they are embedded? Do plumes have a role in solar wind acceleration and mass loading? Answers to these questions are still somewhat ambiguous and theoretical modeling does not provide definite answers either. Recent data, with an unprecedented high spatial and temporal resolution, provide new information on the fine structure of plumes, their temporal evolution and relationship with other transient phenomena that may shed further light on these elusive features. Article RevisionsLiving Reviews supports two ways of keeping its articles up-to-date:Fast-track revision. A fast-track revision provides the author with the opportunity to add short notices of current research results, trends and developments, or important publications to the article. A fast-track revision is refereed by the responsible subject editor. If an article has undergone a fast-track revision, a summary of changes will be listed here.Major update. A major update will include substantial changes and additions and is subject to full external refereeing. It is published with a new publication number.For detailed documentation of an article's evolution, please refer to the history document of the article's online version at http://dx

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Section: The Birth Of Plumesmentioning

confidence: 99%

Solar Coronal Plumes

Poletto

2015

Living Rev. Sol. Phys.

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“…Recent observations from Hinode reveal that jets of various sizes occur in the solar atmosphere with a much greater frequency than previously thought. These include X-ray coronal jets (Cirtain et al 2007) and a newly discovered class of fast 50-150 km s −1 spicules (de Pontieu et al 2007Pontieu et al , 2009. Figure 4 is an example of one such highly collimated structure that may survive to SPP distances.…”

Section: Sources Of the Solar Windmentioning

confidence: 99%

Solar Wind Electrons Alphas and Protons (SWEAP) Investigation: Design of the Solar Wind and Coronal Plasma Instrument Suite for Solar Probe Plus

et al. 2015

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The Solar Wind Electrons Alphas and Protons (SWEAP) Investigation on SolarProbe Plus is a four sensor instrument suite that provides complete measurements of the electrons and ionized helium and hydrogen that constitute the bulk of solar wind and coronal plasma. SWEAP consists of the Solar Probe Cup (SPC) and the Solar Probe Analyzers (SPAN). SPC is a Faraday Cup that looks directly at the Sun and measures ion and electron fluxes and flow angles as a function of energy. SPAN consists of an ion and electron electrostatic analyzer (ESA) on the ram side of SPP (SPAN-A) and an electron ESA on the anti-ram side (SPAN-B). The SPAN-A ion ESA has a time of flight section that enables it to sort particles by their mass/charge ratio, permitting differentiation of ion species. SPAN-A and -B are rotated relative to one another so their broad fields of view combine like the seams on a baseball to view the entire sky except for the region obscured by the heat shield and covered by SPC. Observations by SPC and SPAN produce the combined field of view and measurement capabilities required to fulfill the science objectives of SWEAP and Solar Probe Plus. SWEAP measurements, in concert with magnetic and electric fields, energetic particles, and white light contextual imaging will enable discovery and understanding of solar wind acceleration and formation, coronal and solar wind heating, and particle acceleration in the inner heliosphere of the solar system. SPC and SPAN are managed by the SWEAP Electronics Module (SWEM), which distributes power, formats onboard data products, and serves as a single electrical interface to the spacecraft. SWEAP data products include ion and electron velocity distribution functions with high energy and angular resolution. Full resolution data are stored within the SWEM, enabling high resolution observations of structures such as shocks, reconnection events, and other transient structures to be selected for download after the fact. This paper describes the implementation of the SWEAP Investigation, the driving requirements for the suite, expected performance of the instruments, and planned data products, as of mission preliminary design review.

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“…Some of these brightness enhancements were associated with X-ray jets. This interesting aspect is not relevant for this communication but is discussed elsewhere (e.g., Cirtain et al 2007). Figure 3 shows a radiance map in the spectral line Fe xii 19.5 nm obtained with EIS.…”

Section: Observations By Eis and Xrtmentioning

confidence: 99%

Multi-spacecraft observations of polar coronal plumes

Curdt

Wilhelm

Feng

et al. 2008

A&A

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Aims. Coronal plumes, along with their structure and rôle in the acceleration of the fast solar wind, are of considerable importance in understanding the physics of the solar atmosphere, in particular, when contrasted with the adjacent plasma, the so-called interplume regions. Methods. Observations of coronal plumes in a coronal hole were obtained with the help of spectrographs and imagers on Hinode, SOHO, STEREO, TRACE, and with ground-based instrumentation. The measurements were performed by a large international team in April 2007. Results. First results of this study from Hinode, SOHO, and STEREO are presented here, at the level of observational facts, leaving the task of detailed analysis to the future.

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Evidence for Alfvén Waves in Solar X-ray Jets

Cited by 418 publications

References 11 publications

Solar Coronal Plumes

Solar Coronal Plumes

Solar Wind Electrons Alphas and Protons (SWEAP) Investigation: Design of the Solar Wind and Coronal Plasma Instrument Suite for Solar Probe Plus

Multi-spacecraft observations of polar coronal plumes

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