Accelerating and Supersonic Density Fluctuations in Coronal Hole Plumes: Signature of Nascent Solar Winds

Cho, Il-Hyun; Nakariakov, V. M.; Moon, Yong‐Jae; Lee, Jinyi; Yu, Dae Jung; Cho, Kyung-Suk; Yurchyshyn, Vasyl; Lee, Harim

doi:10.3847/2041-8213/abb020

Cited by 9 publications

(4 citation statements)

References 49 publications

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“…The estimated mass flux is ≈1.2 × 10 12 g s −1 , which is lower than the mass flux from network jets derived from IRIS observations (Tian et al 2014), but higher than the rough estimates of mass flux from a polar plume and open structures at the periphery of an active region (Sakao et al 2007;Cho et al 2020). Therefore, the jetlet mass flux is roughly comparable to the mass-loss rate in the wind at solar minimum, but a smaller fraction (≈60%) of the solar-maximum wind (Wang 1998(Wang , 2020.…”

Section: Mass-loss Rate From Jetletscontrasting

confidence: 54%

Quasi-periodic Energy Release and Jets at the Base of Solar Coronal Plumes

Kumar

Karpen

Uritsky

et al. 2022

ApJ

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Coronal plumes are long, ray-like, open structures that have been considered as possible sources of the solar wind. Their origin in the largely unipolar coronal holes has long been a mystery. Earlier spectroscopic and imaging observations revealed blueshifted plasma and propagating disturbances (PDs) in plumes that are widely interpreted in terms of flows and/or propagating slow-mode waves, but these interpretations (flows versus waves) remain under debate. Recently we discovered an important clue about plume internal structure: dynamic filamentary features called plumelets, which account for most of the plume emission. Here we present high-resolution observations from the Solar Dynamics Observatory/Atmospheric Imaging Assembly and the Interface Region Imaging Spectrograph that revealed numerous, quasi-periodic, tiny jets (so-called jetlets) associated with transient brightening, flows, and plasma heating at the chromospheric footpoints of the plumelets. By analogy to larger coronal jets, these jetlets are most likely produced within the plume base by magnetic reconnection between closed and open flux at stressed 3D null points. The jetlet-associated brightenings are in phase with plumelet-associated PDs, and vary with a period of ∼3–5 minutes, which is remarkably consistent with the photospheric/chromospheric p-mode oscillation. This reconnection at the open-closed boundary in the chromosphere/transition region is likely modulated or driven by local manifestations of the global p-mode waves. The jetlets extend upward to become plumelets, contribute mass to the solar wind, and may be sources of the switchbacks recently detected by the Parker Solar Probe.

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Section: Mass-loss Rate From Jetletscontrasting

confidence: 54%

Quasi-periodic Energy Release and Jets at the Base of Solar Coronal Plumes

Kumar

Karpen

Uritsky

et al. 2022

ApJ

View full text Add to dashboard Cite

show abstract

“…The estimated mass flux is ≈1.2×10 12 g s −1 , which is lower than the mass flux from network jets derived from IRIS observations (Tian et al 2014), but higher than the rough estimates of mass flux from a polar plume and open structures at the periphery of an active region (Sakao et al 2007;Cho et al 2020). Therefore the jetlet mass flux is roughly comparable to the mass-loss rate in the wind at solar minimum, but a smaller fraction (≈ 60%) of the solarmaximum wind (Wang 1998(Wang , 2020.…”

Section: Mass Loss Rate From Jetletscontrasting

confidence: 54%

Quasiperiodic Energy Release and Jets at the Base of Solar Coronal Plumes

Kumar,

Karpen,

Uritsky

et al. 2022

Preprint

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Coronal plumes are long, ray-like, open structures, which have been considered as possible sources for the solar wind. Their origin in the largely unipolar coronal holes has long been a mystery. Earlier spectroscopic and imaging observations revealed blue-shifted plasma and propagating disturbances (PDs) in plumes that are widely interpreted in terms of flows and/or propagating slow-mode waves, but these interpretations (flows vs waves) remain under debate. Recently we discovered an important clue about plume internal structure: dynamic filamentary features called "plumelets", which account for most of the plume emission. Here we present highresolution observations from the Solar Dynamics Observatory's Atmospheric Imaging Assembly (SDO/AIA) and the Interface Region Imaging Spectrograph (IRIS) that revealed numerous, quasiperiodic, tiny jets (socalled "jetlets") associated with transient brightening, flows, and plasma heating at the chromospheric footpoints of the plumelets. By analogy to larger coronal jets, these jetlets are most likely produced within the plume base by magnetic reconnection between closed and open flux at stressed 3D null points. The jetlet-associated brightenings are in phase with plumelet-associated PDs, and vary with a period of ∼3 to 5 minutes, which is remarkably consistent with the photospheric/chromospheric p-mode oscillation. This reconnection at the openclosed boundary in the chromosphere/transition region is likely modulated or driven by local manifestations of the global p-mode waves. The jetlets extend upward to become plumelets, contribute mass to the solar wind, and may be sources of the switchbacks recently detected by the Parker Solar Probe.

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“…A similar technique has recently been successfully applied to the analysis of the mechanisms responsible for the excitation of kink oscillations of coronal loops, which is based on a special catalog of corresponding events [Zimovets et al, 2015]. A separate task is to determine inclination angles of jet axes with respect to the solar surface and their evolution during a solar cycle, which will significantly improve the reconstruction of the global geometry of the coronal magnetic field by the method proposed in [Fleishman et al, 2017].…”

Section: Discussionmentioning

confidence: 99%

Diagnostics of plasma jets in the solar corona

Anfinogentov

Kaltman

Stupishin

et al. 2021

Solar-Terrestrial Physics

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The paper discusses the diagnostics of plasma jets in the solar corona with the use of data from modern space- and ground-based telescopes observing the Sun in the extreme ultraviolet (EUV) and micro- wave bands. We examine observational parameters of EUV and radio emission in events associated with plasma jets, depending on the mechanism of formation, initiation conditions, and evolution of the jets. The opportunities provided by the study of plasma jets, which relies on simultaneous observations in different bands, are highlighted. For a number of jets, we have measured their primary parameters; and in this paper we present preliminary results of statistical processing of the data obtained. Microwave observations of several specific events, made by ground-based instruments RATAN-600, SRH, and Nobeyama Radioheliograph, are considered in detail. The diagnostic capabilities of these instruments for studying coronal jets are shown. To analyze the three-dimensional structure of the coronal magnetic field, we have used SDO/HMI data, which allowed for the reconstruction of the field in the lower corona. The information gained is compared with the results of diagnostics of the magnetic field at the base of the corona according to RATAN-600 data. The purpose of the methods developed is to determine the physical mechanisms responsible for the generation, collimation, and dynamics of plasma jets in the solar atmosphere.

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Accelerating and Supersonic Density Fluctuations in Coronal Hole Plumes: Signature of Nascent Solar Winds

Cited by 9 publications

References 49 publications

Quasi-periodic Energy Release and Jets at the Base of Solar Coronal Plumes

Quasi-periodic Energy Release and Jets at the Base of Solar Coronal Plumes

Quasiperiodic Energy Release and Jets at the Base of Solar Coronal Plumes

Diagnostics of plasma jets in the solar corona

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