Observations of X-Ray Jets Using Yohkoh Soft X-Ray Telescope

Shibata, Kazunari; Ishido, Y.; Acton, L. W.; Strong, K. T.; Hirayama, T.; Uchida, Yutaka; McAllister, A. H.; Matsumoto, R.; Tsuneta, S.; Shimizu, Toshifumi; Hara, Hirohisa; Sakurai, Takashi; Ichimoto, Kiyoshi; Nishino, Y.; Ogawara, Y.

doi:10.1017/s0252921100029341

Cited by 70 publications

(120 citation statements)

References 4 publications

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“…In the X-ray range, Yohkoh/SXT frequently observed small-scale SXR ejecta, including erupting loops, blobs that were interpreted as plasmoids (with typical speeds of ≈ 500 km s -1 ; see e.g., Shibata et al, 1995;Ohyama and Shibata, 1998), and jets (e.g., Shibata et al, 1992;Alexander and Fletcher, 1999). There has been evidence for the generation of metric type II bursts by these rapidly expanding loops, plasmoids, and jets (Gopalswamy et al, 1997;Klein et al, 1999;Gopalswamy et al, 2001b;Klassen et al, 2003).…”

Section: Small-scale Ejectamentioning

confidence: 99%

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

168

140

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Large-scale, globally propagating wave-like disturbances have been observed in the solar chromosphere and by inference in the corona since the 1960s. However, detailed analysis of these phenomena has only been conducted since the late 1990s. This was prompted by the availability of high-cadence coronal imaging data from numerous spaced-based instruments, which routinely show spectacular globally propagating bright fronts. Coronal waves, as these perturbations are usually referred to, have now been observed in a wide range of spectral channels, yielding a wealth of information. Many findings have supported the "classical" interpretation of the disturbances: fast-mode MHD waves or shocks that are propagating in the solar corona. However, observations that seemed inconsistent with this picture have stimulated the development of alternative models in which "pseudo waves" are generated by magnetic reconfiguration in the framework of an expanding coronal mass ejection. This has resulted in a vigorous debate on the physical nature of these disturbances. This review focuses on demonstrating how the numerous observational findings of the last one and a half decades can be used to constrain our models of large-scale coronal waves, and how a coherent physical understanding of these disturbances is finally emerging. 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: Small-scale Ejectamentioning

confidence: 99%

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

168

140

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“…In particular, we now know that the term "quiet Sun" is not really adequate to describe the coronal field even outside of ARs, since numerous dynamic phenomena on small scales are known to occur there (Schadee et al 1983;Parker 1988;Shibata et al 1992). Chesny et al (2013) found the first evidence for sigmoidal (i.e., S shaped) loops in the QS using SDO/AIA data.…”

Section: Small-scale Dynamicsmentioning

confidence: 99%

“…Moreover, the influence of the individual jets was discernible as fine structures in the solar wind flow at a distance of one AU. Later, X-ray jets were observed by Shibata et al (1992Shibata et al ( , 1994, although not necessarily in quiet-Sun regions. Yokoyama and Shibata (1995) carried out 2D resistive MHD simulations including a simplified convection zone, photosphere, chromosphere and corona.…”

Section: Jetsmentioning

confidence: 99%

The magnetic field in the solar atmosphere

Wiegelmann

Thalmann

Solanki

2014

Astron Astrophys Rev

182

125

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This publication provides an overview of magnetic fields in the solar atmosphere with the focus lying on the corona. The solar magnetic field couples the solar interior with the visible surface of the Sun and with its atmosphere. It is also responsible for all solar activity in its numerous manifestations. Thus, dynamic phenomena such as coronal mass ejections and flares are magnetically driven. In addition, the field also plays a crucial role in heating the solar chromosphere and corona as well as in accelerating the solar wind. Our main emphasis is the magnetic field in the upper solar atmosphere so that photospheric and chromospheric magnetic structures are mainly discussed where relevant for higher solar layers. Also, the discussion of the solar atmosphere and activity is limited to those topics of direct relevance to the magnetic field. After giving a brief overview about the solar magnetic field in general and its global structure, we discuss in more detail the magnetic field in active regions, the quiet Sun and coronal holes.

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“…This has been proposed as the process that heats both the non-flare [e.g., Parker, 1972Parker, , 1979Parker, , 1983Sturrock and Uchida, 1981;van Ballegooijen, 1986;Antiochos, 1990] and flare corona [e.g., Sweet, 1958;Parker, 1963;Petschek, 1964;Carmichael, 1964;Sturrock, 1966] Second, reconnection can produce strong mass motions, the so-called reconnection jets. These have been proposed [Karpen, Antiochos, and DeVore, 1995, 1998] as the explanation for a large variety of transient dynamic phenomena ranging from spicules [e.g., Blake and Sturrock, 1985] to explosive events [Dere et al, 1991] to large surges and sprays [e.g., Rust, 1968;Herant et al, 1991;Schmeider et al, 1994;Yokohama and Shibata, 1996] and X-ray jets [Shibata et al, 1992]. Third, reconnection can lead to the acceleration of non-thermal particles.…”

Section: Introductionmentioning

confidence: 99%

The role of magnetic reconnection in solar activity

Antiochos¹,

DeVore²

1999

Geophysical Monograph Series

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Abstract. We argue that magnetic reconnection plays the determining role in many of the various manifestations of solar activity. In particular, it is the trigger mechanism for the most energetic of solar events, coronal mass ejections and eruptive flares. We propose that in order to obtain explosive eruptions, magnetic reconnection in the corona must have an "on-off" nature, and show that reconnection in a sheared multi-polar field configuration does have this property. Numerical simulation results which support this model are presented, and implications for coronal mass ejections/eruptive flare prediction are discussed.

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Observations of X-Ray Jets Using Yohkoh Soft X-Ray Telescope

Cited by 70 publications

References 4 publications

Large-scale Globally Propagating Coronal Waves

Large-scale Globally Propagating Coronal Waves

The magnetic field in the solar atmosphere

The role of magnetic reconnection in solar activity

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