Giant Chromospheric Anemone Jet Observed with
                    <i>Hinode</i>
                    and Comparison with Magnetohydrodynamic Simulations: Evidence of Propagating Alfvén Waves and Magnetic Reconnection

Nishizuka, Naoto; Shimizu, Masaki; Nakamura, Tahei; Otsuji, Kenichi; Okamoto, Takenori J.; Katsukawa, Y.; Shibata, Kazunari

doi:10.1086/591445

Cited by 178 publications

(179 citation statements)

References 40 publications

(52 reference statements)

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“…This results in the ejection of cool plasma (10 000 K) that had been supported by the field. Magnetohydrodynamic simulations of this scenario describe the observations well (Yokoyama & Shibata 1995;Nishizuka et al 2008;Moreno-Insertis et al 2008). Ejected jet material accelerated by the J × B force will have a velocity of the order of the Alfvén speed.…”

Section: Introductionmentioning

confidence: 73%

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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Section: Introductionmentioning

confidence: 73%

Hard X-ray emission from a flare-related jet

Bain¹,

Fletcher²

2009

A&A

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“…The speeds of the outflows were estimated to be in the range from 200 to 800 km s −1 . Hot jets observed in soft X-rays precede cool jets observed in the optical band (Nishizuka et al 2008).…”

Section: Introductionmentioning

confidence: 93%

Propagating transverse waves in soft X-ray coronal jets

Farahani¹,

Doorsselaere²,

Verwichte³

et al. 2009

A&A

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Aims. The theoretical model for magnetohydrodynamic (MHD) modes guided by a field-aligned plasma cylinder with a steady flow is adapted to interpret transverse waves observed in solar coronal hot jets, discovered with Hinode/XRT in terms of fast magnetoacoustic kink modes. Methods. Dispersion relations for linear magnetoacoustic perturbations of a plasma jet of constant cross-section surrounded by static magnetised plasma are used to determine the phase and group speeds of guided transverse waves and their relationship with the physical parameters of the jet and the background plasma. The structure of the perturbations in the macroscopic parameters of the plasma inside and outside the jet, and the phase relations between them are also established. Results. We obtained a convenient expansion for the long wave-length limit of the phase and group speeds and have shown that transverse waves observed in soft-X-ray solar coronal jets are adequately described in terms of fast magnetoacoustic kink modes by a magnetic cylinder model, which includes the effect of a steady flow. In the observationally determined range of parameters, the waves are not found to be subject to either the Kelvin-Helmholtz instability or the negative energy wave instability, and hence they are likely to be excited at the source of the jet.

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“…They interpreted the increase of the radiance in the cooler spectral lines as emitted from the falling back plasma of the cooling down jet. Nishizuka et al (2008) reported on simultaneous cool emission (∼10 4 K) in Ca ii H images from the Solar Optical Telescope (SOT) onboard Hinode and hot emission (1.3 × 10 6 K) in Fe xii 195 Å images from the Extreme-ultraviolet Imaging Telescope (EIT) and movie are only available in electronic form at http://www.aanda.org onboard the Solar and Heliospheric Observatory (SoHO) as well as in X-ray Telescope (XRT) images (Al_poly filter with a temperature response with a maximum at 5 × 10 6 K) from a "giant" jet. From their observations of a current-sheet-like structure seen in all three instruments, they concluded that magnetic reconnection is occurring in the transition region or upper chromosphere.…”

Section: Introductionmentioning

confidence: 99%

Dynamics and plasma properties of an X-ray jet from SUMER, EIS, XRT, and EUVI A & B simultaneous observations

Madjarska

2010

A&A

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Context. Small-scale transient phenomena in the quiet Sun are believed to play an important role in coronal heating and solar wind generation. One of them, called "X-ray jet", is the subject of our study. Aims. We intend to investigate the dynamics, evolution, and physical properties of this phenomenon. Methods. We combine multi-instrument observations obtained simultaneously with the SUMER spectrometer onboard SoHO, with EIS and XRT onboard Hinode, and with EUVI/SECCHI onboard the Ahead and Behind STEREO spacecrafts. We derive plasma parameters such as temperatures and densities as well as dynamics by using spectral lines formed in the temperature range from 10 000 K to 12 MK. We also use an image difference technique to investigate the evolution of the complex structure of the studied phenomenon.Results. With the available unique combination of data we were able to establish that the formation of a jet-like event is triggered by not one, but several energy depositions, which are most probably originating from magnetic reconnection. Each energy deposition is followed by the expulsion of pre-existing or newly reconnected loops and/or collimated flow along open magnetic field lines. We derived in great detail the dynamic process of X-ray jet formation and evolution. For the first time we also found spectroscopically a temperature of 12 MK (Fe xxiii 263.76 Å) and density of 4 × 10 10 cm −3 in the quiet Sun, obtained from a pair of Fe xii lines with a maximum formation temperature of 1.3 × 10 6 K, in an energy deposition region. We point out a problem concerning an uncertainty in using the SUMER Mg x 624.9 Å line for coronal diagnostics. We clearly identified two types of up-flow: one collimated up-flow along open magnetic field lines and a plasma cloud formed from the expelled BP loops. We also report a cooler down-flow along closed magnetic field lines. A comparison is made with a model developed by Moreno-Insertis et al. (2008).

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Giant Chromospheric Anemone Jet Observed with Hinode and Comparison with Magnetohydrodynamic Simulations: Evidence of Propagating Alfvén Waves and Magnetic Reconnection

Cited by 178 publications

References 40 publications

Hard X-ray emission from a flare-related jet

Hard X-ray emission from a flare-related jet

Propagating transverse waves in soft X-ray coronal jets

Dynamics and plasma properties of an X-ray jet from SUMER, EIS, XRT, and EUVI A & B simultaneous observations

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