Studies in Various Damages on the Testicle

Saito, Sumiko

doi:10.5980/jpnjurol1928.49.10_849

Cited by 7 publications

(9 citation statements)

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“…Coronal plumes, extending as bright narrow structures from the solar chromosphere into the high corona are mostly rooted in Coronal Holes (CH) or their neighbourhood (van de Hulst 1950;Saito 1958Saito , 1965DeForest et al 2001). They are plasma density enhancements in the low and extended corona aligned along the magnetic field (Wilhelm et al 2011;Velli et al 2011).…”

Section: Introductionmentioning

confidence: 99%

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Dynamics of on-Disk Plumes as Observed With the Interface Region Imaging Spectrograph, the Atmospheric Imaging Assembly, and the Helioseismic and Magnetic Imager

Pant

Dolla

Mazumder

et al. 2015

ApJ

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We examine the role of small-scale transients in the formation and evolution of solar coronal plumes. We study the dynamics of plume footpoints seen in the vicinity of a coronal hole using the Atmospheric Imaging Assembly (AIA) images, the Helioseismic and Magnetic Imager (HMI) magnetogram on board the Solar Dynamics Observatory (SDO) and spectroscopic data from the Interface Region Imaging Spectrograph (IRIS). Quasi-periodic brightenings are observed in the base of the plumes and are associated with magnetic flux changes. With the high spectral and spatial resolution of IRIS, we identify the sources of these oscillations and try to understand what role the transients at the foot points can play in sustaining the coronal plumes.IRIS sit and stare observation provide a unique opportunity to study the evolution of foot points of the plumes. We notice enhanced line width, intensity and large deviation from the average Doppler shift in the line profiles at specific instances which indicate the presence of flows at the foot points of plumes. We propose that outflows (jet-like features) as a result of small scale reconnections affect the line profiles. These jet-like features may be also responsible for the generation of propagating disturbances within the plumes which are observed to be propagating to larger distances as recorded from multiple AIA channels. These propagating disturbances can be explained in terms of slow magnetoacoustic waves.

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Section: Introductionmentioning

confidence: 99%

“…1950; Saito 1958Saito , 1965DeForest et al 2001). They are plasma density enhancements in the low and extended corona aligned along the magnetic field (Wilhelm et al 2011;Velli et al 2011).…”

mentioning

confidence: 99%

Dynamics of on-Disk Plumes as Observed With the Interface Region Imaging Spectrograph, the Atmospheric Imaging Assembly, and the Helioseismic and Magnetic Imager

Pant

Dolla

Mazumder

et al. 2015

ApJ

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“…Above the solar limb, polar plumes appear brighter than the surrounding media, suggesting that they are denser than the background corona or inter-plume regions (e.g. van de Hulst 1950;Saito 1958Saito & 1965etc). The coronal-background electron density is about ∼ 10 8 cm −3 and falls sharply with height (see different density models in .…”

Section: Introductionmentioning

confidence: 99%

“…This paper is a forward modeling investigation of the plasma dynamics of polar plumes. These socalled "polar rays" or polar plumes (e.g., van de Hulst 1950;Saito 1958;Harvey 1965;Koutchmy, 1977;DeForest et al 1997) trace open magnetic field lines to different heights depending on observation type. In Extreme UltraViolet (EUV) emission line spectroheliograms, plumes appear as short spikes near the polar limb (Bohlin et al 1975a;Ahmad & Withbroe 1977;Widing & Feldman 1992;Walker et al 1993) with unchanged shape and sudden brightness changes over typical lifetimes ranging from several hours to days (see DeForest et al 1997;Del Zanna et al 1997).…”

Section: Introductionmentioning

confidence: 99%

Properties of Solar Polar Coronal Plumes Constrained by Ultraviolet Coronagraph Spectrometer Data

Raouafi

Harvey

Solanki

2007

ApJ

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We investigate the plasma dynamics (outflow speed and turbulence) inside polar plumes. We compare line profiles (mainly of O VI) observed by the UVCS instrument on SOHO at the minimum of solar cycle 22-23 with model calculations. We consider Maxwellian velocity distributions with different widths in plume and inter-plume regions. Electron densities are assumed to be enhanced in plumes and to approach inter-plume values with increasing height. Different combinations of the outflow and turbulence velocity in the plume regions are considered. We compute line profiles and total intensities of the H I Lyα and the O VI doublets. The observed profile shapes and intensities are reproduced best by a small solar wind speed at low altitudes in plumes that increases with height to reach ambient inter-plume values above roughly 3-4 R ⊙ combined with a similar variation of the width of the velocity distribution of the scattering atoms/ions. We also find that plumes very close to the pole give narrow profiles at heights above 2.5 R ⊙ , which are not observed. This suggests a tendency for plumes to be located away from the pole. We find that the inclusion of plumes in the model computations provides an improved correspondence with the observations and confirms previous results showing that published UVCS observations in polar coronal holes can be roughly reproduced without the need for large temperature anisotropy. The latitude distributions of plumes and magnetic flux distributions are studied by analyzing data from different instruments on SOHO and with SOLIS.

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“…Coronal plumes, extending as bright narrow structures from the solar chromosphere into the high corona are mostly rooted in coronal holes (CHs) or their neighborhood (van de Hulst 1950;Saito 1958Saito , 1965DeForest et al 2001). They are plasma density enhancements in the low and extended corona aligned along the magnetic field (Velli et al 2011;Wilhelm et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Fiber-optic spectrum analyzer

Vaskes¹,

Cheremiskin²,

Чехлова³

1992

Sov. J. Quantum Electron.

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We examine the role of small-scale transients in the formation and evolution of solar coronal plumes. We study the dynamics of plume footpoints seen in the vicinity of a coronal hole using the Atmospheric Imaging Assembly (AIA) images, the Helioseismic and Magnetic Imager magnetogram on board the Solar Dynamics Observatory and spectroscopic data from the Interface Region Imaging Spectrograph (IRIS). Quasi-periodic brightenings are observed in the base of the plumes and are associated with magnetic flux changes. With the high spectral and spatial resolution of IRIS, we identify the sources of these oscillations and try to understand what role the transients at the footpoints can play in sustaining the coronal plumes. IRIS "sit-and-stare" observations provide a unique opportunity to study the evolution of footpoints of the plumes. We notice enhanced line width and intensity, and large deviation from the average Doppler shift in the line profiles at specific instances, which indicate the presence of flows at the footpoints of plumes. We propose that outflows (jet-like features) as a result of small-scale reconnections affect the line profiles. These jet-like features may also be responsible for the generation of propagating disturbances (PDs) within the plumes, which are observed to be propagating to larger distances as recorded from multiple AIA channels. These PDs can be explained in terms of slow magnetoacoustic waves.

show abstract

Studies in Various Damages on the Testicle

Cited by 7 publications

References 0 publications

Dynamics of on-Disk Plumes as Observed With the Interface Region Imaging Spectrograph, the Atmospheric Imaging Assembly, and the Helioseismic and Magnetic Imager

Dynamics of on-Disk Plumes as Observed With the Interface Region Imaging Spectrograph, the Atmospheric Imaging Assembly, and the Helioseismic and Magnetic Imager

Properties of Solar Polar Coronal Plumes Constrained by Ultraviolet Coronagraph Spectrometer Data

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