Fundamental Speed Limits to the Generation of Quantumness

Jing, Jun; Wu, Lian-Ao; Campo, Adolfo del

doi:10.1038/srep38149

Cited by 51 publications

(48 citation statements)

References 50 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Foukal 1978) and in flare loops at cool temperatures such as Hα (e.g. Jing et al 2016), He II 304Å (Scullion et al 2016), and IRIS slit-jaw images (Lacatus et al 2017). Jing et al (2016) showed, importantly, that the impact of the rain in the chromosphere followed exactly the same path as the flare ribbon and had the same size scale as the ribbon, demonstrating a tight cause and ef-fect between the energy release and formation of rain.…”

Section: Introductionmentioning

confidence: 97%

“…The work of Mikić et al (2013) showed that TNE and the formation of coronal condensations also depends strongly on the geometry of the loop, both in terms of crosssectional area expansion and a general loop asymmetry. The requirement that the heating be steady over a long period of time, however, suggests an issue: rain is observed in flares (Jing et al 2016) and perhaps in non-flaring impulsive events as well (Kohutova et al 2019).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Electron Beams Cannot Directly Produce Coronal Rain

Reep

Antolin

Bradshaw

2020

ApJ

View full text Add to dashboard Cite

Coronal rain is ubiquitous in flare loops, forming shortly after the onset of the solar flare. Rain is thought to be caused by a thermal instability, a localized runaway cooling of material in the corona. The models that demonstrate this require extremely long duration heating on the order of the radiative cooling time, localized near the footpoints of the loops. In flares, electron beams are thought to be the primary energy transport mechanism, driving strong footpoint heating during the impulsive phase that causes evaporation, filling and heating flare loops. Electron beams, however, do not act for a long period of time, and even supposing that they did, their heating would not remain localized at the footpoints. With a series of numerical experiments, we show directly that these two issues mean that electron beams are incapable of causing the formation of rain in flare loops. This result suggests that either there is another mechanism acting in flare loops responsible for rain, or that the modeling of the cooling of flare loops is somehow deficient. To adequately describe flares, the standard model must address this issue to account for the presence of coronal rain.

show abstract

Section: Introductionmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

Electron Beams Cannot Directly Produce Coronal Rain

Reep

Antolin

Bradshaw

2020

ApJ

View full text Add to dashboard Cite

show abstract

“…5). Similar phenomena linked to coronal rain have been observed in Kleint et al (2014) and Jing et al (2016). They are typically explained as a result of collision of the individual rain blobs with the dense transition region plasma or as a result of compression and the resulting heating of the plasma confined under the rain blobs (Müller et al 2003).…”

Section: Thermal Instability and Formation Of Condensationsmentioning

confidence: 69%

“…They are typically explained as a result of collision of the individual rain blobs with the dense transition region plasma or as a result of compression and the resulting heating of the plasma confined under the rain blobs (Müller et al 2003). A shock front caused by instabilityinduced siphon flows transitioning from supersonic to subsonic speeds has also been suggested as a possible explanation (Jing et al 2016).…”

Section: Thermal Instability and Formation Of Condensationsmentioning

confidence: 99%

Formation of coronal rain triggered by impulsive heating associated with magnetic reconnection

Kohutova

Verwichte

Froment

2019

A&A

View full text Add to dashboard Cite

Context. Coronal rain consists of cool plasma condensations formed in coronal loops as a result of thermal instability. The standard models of coronal rain formation assume that the heating is quasi-steady and localised at the coronal loop footpoints. Aims. We present an observation of magnetic reconnection in the corona and the associated impulsive heating triggering formation of coronal rain condensations. Methods. We analyse combined SDO/AIA and IRIS observations of a coronal rain event following a reconnection between threads of a low-lying prominence flux rope and surrounding coronal field lines.Results. The reconnection of the twisted flux rope and open field lines leads to a release of magnetic twist. Evolution of the emission of one of the coronal loops involved in the reconnection process in different AIA bandpasses suggests that the loop becomes thermally unstable and is subject to the formation of coronal rain condensations following the reconnection and that the associated heating is localised in the upper part of the loop leg.Conclusions. In addition to the standard models of thermally unstable coronal loops with heating localised exclusively in the footpoints, thermal instability and subsequent formation of condensations can be triggered by the impulsive heating associated with magnetic reconnection occurring anywhere along a magnetic field line.

show abstract

“…Other forms of QSL in open system were also reported, such as the QSL in different environments [23][24][25][26][27][28][29], the initialstate dependence [30], the geometric form for Wigner phase space [31], the experimentally realizable metric [32]. In addition, many other aspects of QSL were also widely studied such as using the fidelity [33,34] and function of relative purity [35,36], the mechanism for quantum speedup [37], the connection with generation of quantumness [38], generalization of geometric QSL form [39], via gauge invariant distance [40], even the QSL for almost all states [41], and so on.…”

Section: Introductionmentioning

confidence: 99%

Quantum speed limit based on the bound of Bures angle

2020

Sci Rep

View full text Add to dashboard Cite

In this paper, we investigate the unified bound of quantum speed limit time in open systems based on the modified Bures angle. This bound is applied to the damped Jaynes-Cummings model and the dephasing model, and the analytical quantum speed limit time is obtained for both models. As an example, the maximum coherent qubit state with white noise is chosen as the initial states for the damped Jaynes-Cummings model. It is found that the quantum speed limit time in both the non-Markovian and the Markovian regimes can be decreased by the white noise compared with the pure state. In addition, for the dephasing model, we find that the quantum speed limit time is not only related to the coherence of initial state and non-Markovianity, but also dependent on the population of initial excited state.

show abstract

Fundamental Speed Limits to the Generation of Quantumness

Cited by 51 publications

References 50 publications

Electron Beams Cannot Directly Produce Coronal Rain

Electron Beams Cannot Directly Produce Coronal Rain

Formation of coronal rain triggered by impulsive heating associated with magnetic reconnection

Quantum speed limit based on the bound of Bures angle

Contact Info

Product

Resources

About