Chromospheric magnetic reconnection caused by photospheric flux emergence: implications for jet-like events formation

Ding, J. Y.; Madjarska, M. S.; Doyle, J. G.; Lu, Quanming

doi:10.1051/0004-6361/200913101

Cited by 14 publications

(27 citation statements)

References 31 publications

(40 reference statements)

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“…For example, the numerical results in the paper by Chen et al (2001), Archontis & Hood (2009) and Xu et al (2011) show that the temperature enhancement for EBs is around several thousands Kelvin and the lifetime is around several minutes, which are similar as the observation results of EBs. By setting suitable initial magnetic fields and plasma density, the numerical simulations can lead to the formation of chromosphere jets which have similar topology structures as from the observations, the up-flow speeds from the simulations can be in the range around 10 − 130 km −1 (Ding et al 2010Yang et al 2013), which are the same as the speeds of the observed chromosphere jets. On the other hand, some numerical simulations focus more on the physical mechanisms of magnetic reconnection in solar chromosphere, the partially ionized effects including ambipolar diffusion and recombination have been studied detailedly (e.g., Leake et al 2012;Murphy & Lukin 2015;Singh et al 2015).…”

Section: Introductionmentioning

confidence: 67%

“…Most of the previous numerical simulations which focus on the formations of EBs (e.g., Chen et al 2001;Isobe et al 2007;Archontis & Hood 2009), chromosphere jets (e.g., Ding et al 2010Ding et al , 2011Yang et al 2013) and micro-flares (e.g., Jiang et al 2012;Archontis & Hansteen 2014) are studied based on the single fluid MHD equations with an assumed anomalous resistivity. The topology structures and many characteristics in these numerical simulations can match well with the observation results.…”

Section: Introductionmentioning

confidence: 99%

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Heating Mechanisms in the Low Solar Atmosphere Through Magnetic Reconnection in Current Sheets

Lin

Roussev

et al. 2016

ApJ

111

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Section: Introductionmentioning

confidence: 67%

Section: Introductionmentioning

confidence: 99%

Heating Mechanisms in the Low Solar Atmosphere Through Magnetic Reconnection in Current Sheets

Lin

Roussev

et al. 2016

ApJ

111

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“…Recently, Ding et al (2010) used a 2.5-dimensional resistive MHD model in Cartesian coordinates to investigate magnetic reconnection in the low atmosphere, e.g. chromosphere, discussing the implications for jet features at transition-region temperatures.…”

Section: Introductionmentioning

confidence: 99%

“…They showed that faster and hotter outflows could be obtained if a physical environment with lower mass density was considered, however, the highest temperature of the plasma heated by magnetic reconnection is only 5 × 10 5 K in their study. Here, we expand the work of Ding et al (2010) varying the electron density and field strength as applied to a larger range of jet features, including fibrils, spicules, chromospheric jets and transition region jets. This work uses a larger grid model (see later) than the previous study.…”

Section: Introductionmentioning

confidence: 99%

Magnetic reconnection resulting from flux emergence: implications for jet formation in the lower solar atmosphere?

Ding¹,

Madjarska²,

Doyle³

et al. 2011

A&A

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Aims. We aim at investigating the formation of jet-like features in the lower solar atmosphere, e.g. chromosphere and transition region, as a result of magnetic reconnection. Methods. Magnetic reconnection as occurring at chromospheric and transition regions densities and triggered by magnetic flux emergence is studied using a 2.5D MHD code. The initial atmosphere is static and isothermal, with a temperature of 2 × 10 4 K. The initial magnetic field is uniform and vertical. Two physical environments with different magnetic field strength (25 G and 50 G) are presented. In each case, two sub-cases are discussed, where the environments have different initial mass density.Results. In the case where we have a weaker magnetic field (25 G) and higher plasma density (N e = 2 × 10 11 cm −3 ), valid for the typical quiet Sun chromosphere, a plasma jet would be observed with a temperature of 2-3 × 10 4 K and a velocity as high as 40 km s −1 . The opposite case of a medium with a lower electron density (N e = 2 × 10 10 cm −3 ), i.e. more typical for the transition region, and a stronger magnetic field of 50 G, up-flows with line-of-sight velocities as high as ∼90 km s −1 and temperatures of 6 × 10 5 K, i.e. upper transition region -low coronal temperatures, are produced. Only in the latter case, the low corona Fe ix 171 Å shows a response in the jet which is comparable to the O v increase. Conclusions. The results show that magnetic reconnection can be an efficient mechanism to drive plasma outflows in the chromosphere and transition region. The model can reproduce characteristics, such as temperature and velocity for a range of jet features like a fibril, a spicule, a hot X-ray jet or a transition region jet by changing either the magnetic field strength or the electron density, i.e. where in the atmosphere the reconnection occurs.

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“…Recent examples of numerical simulations of explosive events in this scenario can be found in Ding et al (2010), Heggland et al (2009), Litvinenko & Chae (2009), and Chen & Priest (2006).…”

Section: Introductionmentioning

confidence: 99%

Statistical techniques for the detection and analysis of solar explosive events

Sarro

2011

A&A

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Context. Solar explosive events are commonly explained as small-scale magnetic reconnection events, although an unambiguous confirmation of this scenario remains elusive owing to the lack of spatial resolution and the statistical analysis of sufficiently large samples of this type of events. Aims. We propose a sound statistical treatment of data cubes consisting of a temporal sequence of long-slit spectra of the solar atmosphere. The analysis comprises all stages from the explosive event detection to its characterization and the subsequent sample study. Methods. We designed two complementary approaches based on the combination of standard statistical techniques (the robust principal component analysis in one approach and wavelet decomposition and independent component analysis in the second) to obtain least biased samples. These techniques are implemented in the spirit of letting the data speak for themselves. The analysis is carried out for two spectral lines: the C iv line at 1548.2 Å and the Ne viii line at 770.4 Å. Results. We find significant differences between the characteristics of the line profiles emitted in the proximities of two active regions, and in the quiet Sun, most visible in the relative importance of a separate population of red shifted profiles. We also find a higher frequency of explosive events near the active regions, and in the C iv line. The distribution of the explosive events characteristics is interpreted in the light of recent numerical simulations. Finally, we point out several regions of the parameter space where the reconnection model has to be refined in order to explain the observations.

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Chromospheric magnetic reconnection caused by photospheric flux emergence: implications for jet-like events formation

Cited by 14 publications

References 31 publications

Heating Mechanisms in the Low Solar Atmosphere Through Magnetic Reconnection in Current Sheets

Heating Mechanisms in the Low Solar Atmosphere Through Magnetic Reconnection in Current Sheets

Magnetic reconnection resulting from flux emergence: implications for jet formation in the lower solar atmosphere?

Statistical techniques for the detection and analysis of solar explosive events

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