A gigantic coronal jet ejected from a compact active region in a coronal hole

Shibata, Katsunori M.; Nitta, N.; Strong, K. T.; Matsumoto, R.; Yokoyama, T.; Hirayama, T.; Hudson, H. S.; Ogawara, Y.

doi:10.1086/187470

Cited by 192 publications

(170 citation statements)

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“…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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Section: Jetsmentioning

confidence: 99%

The magnetic field in the solar atmosphere

Wiegelmann

Thalmann

Solanki

2014

Astron Astrophys Rev

182

125

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“…Thus, the plasma of these outflow jets has been heated by the slow-mode shocks (Cargill & Priest 1982). Such jets are apparently seen in the soft X-ray and/or EUV images of the Sun (Shibata et al 1992(Shibata et al , 1994Wang et al 2007). If the speed of this outflow jet is super-Alfvénic, a fast magnetosonic shock, also called termination shock can be established thanks to the deceleration of the jet during its penetration into the surrounding plasma.…”

Section: Introductionmentioning

confidence: 99%

Budget of energetic electrons during solar flares in the framework of magnetic reconnection

Mann

Warmuth

2011

A&A

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Context. Among other things, solar flares are accompanied by the production of energetic electrons as seen in the nonthermal radio and X-ray radiation of the Sun. Observations of the RHESSI satellite show that 10 32 −10 36 nonthermal electrons are produced per second during flares. They are related to an energy flux in the range 10 18 −10 22 W. These electrons play an important role, since they carry a substantial part of the energy released during a flare. Aims. In which way so many electrons are accelerated up to high energies during a fraction of a second is still an open question. By means of radio and hard X-ray data, we investigate under which conditions this acceleration happens in the corona. Methods. The flare is considered in the framework of magnetic reconnection. The conditions in the acceleration region in the corona are deduced by using the conservation of the total electron number and energy. Results. In the inflow region of the magnetic reconnection site, there are typical electron number densities of about 2.07×10 9 cm −3 and magnetic fields of about 46 G. These are regions with high Alfvén speeds of about 2200 km s −1 . Then, sufficient energetic electrons (as required by the RHESSI observations) are only generated if the plasma inflow towards the reconnection site has Alfvén-Mach numbers in the range 0.1−1, which can lead to a super-Alfvénic outflow with speeds up to 3100 km s −1 .

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“…It has been shown that jets are spatially correlated with active regions, X-ray bright points and regions of emerging flux and can be associated with small footpoint flares (Shibata et al 1992(Shibata et al , 1994. Several studies of X-ray jets (Shimojo et al 1996;Canfield et al 1996) yielded characteristic properties such as length and width observed to be in the range of a few 10 4 -10 5 km and 5 × 10 3 -10 5 km respectively.…”

Section: Introductionmentioning

confidence: 99%

Hard X-ray emission from a flare-related jet

Bain¹,

Fletcher²

2009

A&A

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Aims. We aim to understand the physical conditions in a jet event which occurred on the 22nd of August 2002, paying particular attention to evidence for non-thermal electrons in the jet material. Methods. We investigate the flare impulsive phase using multiwavelength observations from the Transition Region and Coronal Explorer (TRACE) and the Reuven Ramaty High Energy Spectroscopic Imager (RHESSI) satellite missions, and the ground-based Nobeyama Radioheliograph (NoRH) and Radio Polarimeters (NoRP). Results.We report what we believe to be the first observation of hard X-ray emission formed in a coronal jet. We present radio observations which confirm the presence of non-thermal electrons present in the jet at this time. The evolution of the event is best compared with the magnetic reconnection jet model in which emerging magnetic field interacts with the pre-existing coronal field. We calculate an apparent jet velocity of ∼500 km s −1 which is consistent with model predictions for jet material accelerated by the J × B force resulting in a jet velocity of the order of the Alfvén speed (∼100-1000 km s −1 ).

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A gigantic coronal jet ejected from a compact active region in a coronal hole

Cited by 192 publications

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The magnetic field in the solar atmosphere

The magnetic field in the solar atmosphere

Budget of energetic electrons during solar flares in the framework of magnetic reconnection

Hard X-ray emission from a flare-related jet

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