Chromospheric Anemone Jets as Evidence of Ubiquitous Reconnection

Shibata, Kazunari; Nakamura, Tahei; Matsumoto, Takuma; Otsuji, Kenichi; Okamoto, Takenori J.; Nishizuka, Naoto; Kawate, Tomoko; Watanabe, Hiroko; Nagata, Shinji; Ueno, S.; Kitai, Reizaburo; Nozawa, Satoshi; Tsuneta, S.; Suematsu, Y.; Ichimoto, Kiyoshi; Shimizu, Toshifumi; Katsukawa, Y.; Tarbell, T. D.; Berger, Thomas; Lites, B. W.; Shine, R. A.; Title, A. M.

doi:10.1126/science.1146708

Cited by 392 publications

(394 citation statements)

References 24 publications

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“…If the generation mechanism is magnetic reconnection in the chromosphere (e.g. Shibata et al, 2007;Yurchyshyn, Abramenko, and Goode, 2013;Deng et al, 2015;Ni et al, 2015), it would indicate that there is no significant difference of magnetic structures in the chromospheric layers of CH and QS. In CH, it is probably small chromospheric loops that reconnect with open flux in the network.…”

Section: Resultsmentioning

confidence: 99%

Statistical Study of Network Jets Observed in the Solar Transition Region: a Comparison Between Coronal Holes and Quiet-Sun Regions

et al. 2016

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Recent IRIS observations have revealed a prevalence of intermittent small-scale jets with apparent speeds of 80 -250 km s −1 , emanating from smallscale bright regions inside network boundaries of coronal holes. We find that these network jets appear not only in coronal holes but also in quiet-sun regions. Using IRIS 1330Å (C II) slit-jaw images, we extract several parameters of these network jets, e.g. apparent speed, length, lifetime and increase in foot-point brightness. Using several observations, we find that some properties of the jets are very similar but others are obviously different between the quiet sun and coronal holes. For example, our study shows that the coronal-hole jets appear to be faster and longer than those in the quiet sun. This can be directly attributed to a difference in the magnetic configuration of the two regions with open magnetic field lines rooted in coronal holes and magnetic loops often present in quiet sun. We have also detected compact bright loops, likely transition region loops, mostly in quiet sun. These small loop-like regions are generally devoid of network jets. In spite of different magnetic structures in the coronal hole and quiet sun in the transition region, there appears to be no substantial difference for the increase in foot-point brightness of the jets, which suggests that the generation mechanism of these network jets is likely the same in both regions.

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Section: Resultsmentioning

confidence: 99%

Statistical Study of Network Jets Observed in the Solar Transition Region: a Comparison Between Coronal Holes and Quiet-Sun Regions

et al. 2016

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“…Thus, we infer that the intermittent coronal outflow might be caused by the chromospheric jet. In previous studies, chromospheric spicule-like jets were often reported near the solar limb, e.g., chromospheric anemone jets (Shibata et al 2007) and the type-II spicule with jet signature (De Pontieu et al 2007). Here, we find that chromospheric jets occur on the solar disk in the possible solar wind source region.…”

Section: Chromospheric Activities In the Source Regionmentioning

confidence: 99%

“…Here, we find that chromospheric jets occur on the solar disk in the possible solar wind source region. The driver of the chromospheric jet might be attributed to magnetic reconnection in the chromosphere (Shibata et al 2007;De Pontieu et al 2007) or a shock wave leaking from the photosphere along the inclined magnetic field lines (Hansteen et al 2006). …”

Section: Chromospheric Activities In the Source Regionmentioning

confidence: 99%

“…Upflows of heated chromospheric plasmas, probably caused by magnetic reconnection, were suggested to supply the observed overdense material to coronal loops in ARs (Aschwanden 2001). Small-scale magnetic reconnection, which may excite transverse waves ), was inferred to be ubiquitous in the chromosphere from observations of chromospheric anemone jets (Shibata et al 2007). The chromospheric jets were sometimes found to be associated with coronal EUV/X-ray jets (Shibata et al 1992;Chae et al 1999;Zhang et al 2000), which have been modeled by magnetic reconnection between newly emerging closed loop and pre-existing open field lines at the chromosphere (Yokoyama & Shibata 1995).…”

Section: Introductionmentioning

confidence: 99%

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Intermittent outflows at the edge of an active region – a possible source of the solar wind?

He¹,

Marsch²,

Tu³

et al. 2010

A&A

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Context. It has already been established that the solar wind may originate at the edges of active regions (ARs), but the key questions of how frequently these outflows occur, and at which height the nascent solar wind originates have not yet been addressed. Aims. We study the occurrence rate of these intermittent outflows, the related plasma activities beneath in the low solar atmosphere, and the interplanetary counterparts of the nascent solar wind outflow. Methods. We use the observations from XRT/Hinode and TRACE to study the outflow patterns. The occurrence frequency of the intermittent outflow is estimated by counting the occurrences of propagating intensity enhancements in height-time diagrams. We adopt observations of SOT/Hinode and EIS/Hinode to investigate the phenomena in the chromosphere associated with the coronal outflows. The ACE plasma and field in-situ measurements near Earth are used to study the interplanetary manifestations. Results. We find that in one elongated coronal emission structure, referred to as strand, the plasma flows outward intermittently, about every 20 min. The flow speed sometimes exceeds 200 km s −1 , which is indicative of rapid acceleration, and thus exceeds the coronal sound speed at low altitudes. The inferred flow speed of the soft-X-ray-emitting plasma component seems a little higher than that of the Fe ix/x-emitting plasma component. Chromospheric jets are found to occur at the root of the strand. Upflows in the chromosphere are also confirmed by blue-shifts of the He ii line. The heliospheric plasma counterpart close to the Earth is found to be an intermediate-speed solar wind stream. The AR edge may also deliver some plasmas to a fraction of the fast solar wind stream, most of which emanate from the neighboring CH. Conclusions. The possible origin of the nascent solar wind in the chromosphere, the observed excessive outflow speed of over 200 km s −1 in the lower corona, and the corresponding intermediate-speed solar wind stream in interplanetary space are all linked in our case study. These phenomena from the low solar atmosphere to the heliosphere near Earth in combination shed new light on the solar wind formation process. These observational results will constrain future modeling of the solar winds originating close to an AR.

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“…The role of magnetic reconnection for heating and dynamics of the solar corona was revisited by Shibata et al (2007), this time observationally with Ca ii H data from Hinode/SOT. So-called "anemone jets" were found both in the corona and in the chromosphere.…”

Section: Jetsmentioning

confidence: 99%

The magnetic field in the solar atmosphere

Wiegelmann

Thalmann

Solanki

2014

Astron Astrophys Rev

176

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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Chromospheric Anemone Jets as Evidence of Ubiquitous Reconnection

Cited by 392 publications

References 24 publications

Statistical Study of Network Jets Observed in the Solar Transition Region: a Comparison Between Coronal Holes and Quiet-Sun Regions

Statistical Study of Network Jets Observed in the Solar Transition Region: a Comparison Between Coronal Holes and Quiet-Sun Regions

Intermittent outflows at the edge of an active region – a possible source of the solar wind?

The magnetic field in the solar atmosphere

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