Contribution of Spicules to Solar Coronal Emission

Mondal, Shanwlee Sow; Klimchuk, J. A.; Sarkar, Aveek

doi:10.3847/1538-4357/ac879b

Cited by 5 publications

(5 citation statements)

References 40 publications

(72 reference statements)

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“…Whether spicules contribute to the solar wind and how much is not well known. A recent study by Sow Mondal et al (2022) suggests that significantly more spicules than observed were needed to drive the solar wind.…”

Section: Introductionmentioning

confidence: 99%

Magnetic Reconnection as the Driver of the Solar Wind

Raouafi

Stenborg

Seaton

et al. 2023

ApJ

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We present EUV solar observations showing evidence for omnipresent jetting activity driven by small-scale magnetic reconnection at the base of the solar corona. We argue that the physical mechanism that heats and drives the solar wind at its source is ubiquitous magnetic reconnection in the form of small-scale jetting activity (a.k.a. jetlets). This jetting activity, like the solar wind and the heating of the coronal plasma, is ubiquitous regardless of the solar cycle phase. Each event arises from small-scale reconnection of opposite-polarity magnetic fields producing a short-lived jet of hot plasma and Alfvén waves into the corona. The discrete nature of these jetlet events leads to intermittent outflows from the corona, which homogenize as they propagate away from the Sun and form the solar wind. This discovery establishes the importance of small-scale magnetic reconnection in solar and stellar atmospheres in understanding ubiquitous phenomena such as coronal heating and solar wind acceleration. Based on previous analyses linking the switchbacks to the magnetic network, we also argue that these new observations might provide the link between the magnetic activity at the base of the corona and the switchback solar wind phenomenon. These new observations need to be put in the bigger picture of the role of magnetic reconnection and the diverse form of jetting in the solar atmosphere.

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Section: Introductionmentioning

confidence: 99%

Magnetic Reconnection as the Driver of the Solar Wind

Raouafi

Stenborg

Seaton

et al. 2023

ApJ

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“…It is unclear to us how the plugs of plasma expelled in the jetting events could make it into the solar wind and maintain the hot temperature of solar wind material, as adiabatic cooling would be expected as the material disperses (Klimchuk 2012;Sow Mondal et al 2022). One concept deserving of consideration is the consequences of the twists put onto the open flux tubes by the erupting minifilaments.…”

Section: Discussionmentioning

confidence: 99%

How Small-scale Jetlike Solar Events from Miniature Flux Rope Eruptions Might Produce the Solar Wind

Sterling,

Panesar,

Moore

2024

ApJ

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We consider small-scale jetlike events that might make the solar wind, as has been suggested in recent studies. We show that the events referred to as “coronal jets” and as “jetlets” both fall on a power-law distribution that also includes large-scale eruptions and spicule-sized features; all of the jetlike events could contribute to the solar wind. Based on imaging and magnetic field data, it is plausible that many or most of these events might form by the same mechanism: Magnetic flux cancelation produces small-scale flux ropes, often containing a cool-material minifilament. This minifilament/flux rope erupts and reconnects with adjacent open coronal field, along which “plasma jets” flow and contribute to the solar wind. The erupting flux ropes can contain twist that is transferred to the open field, and these become Alfvénic pulses that form magnetic switchbacks, providing an intrinsic connection between switchbacks and the production of the solar wind.

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“…The steady uniform heating is maintained as the impulsive heating events are later imposed. We also include an additional temperature and density-dependent heating in the chromosphere to maintain the desired chromospheric temperature in the presence of expansion cooling (see the discussion in Sow Mondal et al 2022).…”

Section: Loop Heatingmentioning

confidence: 99%

Modeling of Condensations in Coronal Loops Produced by Impulsive Heating with Variable Frequencies and Locations

Kucera,

Klimchuk,

Luna

2024

ApJ

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We present the results of models of impulsively heated coronal loops using the 1D hydrodynamic Adaptively Refined Godunov Solver code. The impulsive heating events (which we refer to as nanoflares) are modeled by discrete pulses of energy along the loop. We explore the occurrence of cold condensations due to the effective equivalent of thermal nonequilibrium in loops with steady heating, and examine its dependence on nanoflare timing and intensity and also nanoflare location along the loop, including randomized distributions of nanoflares. We find that randomizing the distribution of nanoflares, both in time/intensity and location, diminishes the likelihood of condensation occurring as compared to distributions with regularly occurring nanoflares with the same average properties. The usual criteria that condensation is favored for heating near loop footpoints and with high cadences are more strict for randomized (as opposed to regular) nanoflare distributions, and for randomized distributions the condensations stay in the loop for a shorter amount of time. That said, condensation can sometimes occur in cases where the average values of parameters (frequency or location) are beyond the critical limits above which condensation does not occur for corresponding steady, non-randomized values of those parameters. These properties of condensation occurring due to randomized heating can be used in the future to investigate the diagnostics of coronal heating mechanisms.

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Contribution of Spicules to Solar Coronal Emission

Cited by 5 publications

References 40 publications

Magnetic Reconnection as the Driver of the Solar Wind

Magnetic Reconnection as the Driver of the Solar Wind

How Small-scale Jetlike Solar Events from Miniature Flux Rope Eruptions Might Produce the Solar Wind

Modeling of Condensations in Coronal Loops Produced by Impulsive Heating with Variable Frequencies and Locations

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