Interferometric investigation of the line of sight velocities in ?5303 during the eclipse of 11 September, 1968

Delone, A. B.; Макарова, Е. А.

doi:10.1007/bf00152228

Cited by 12 publications

(2 citation statements)

References 9 publications

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“…For 148 measured line profiles V ls the range from 5 to 148 km s −1 was found and besides for 89% of the cases V ls less than 80 km s −1 and for 11% V ls greater than 80 km s −1 were observed. From an interferogram in the green line 5303Å obtained during the eclipse of 1968, Delone and Makarova [1975] constructed line profiles that could be frequently decomposed into components: from their shifts the velocities up to 135 km s −1 were deter-mined. For 510 measured line profiles V ls the range from 15 to 135 km s −1 was found and besides in 74% of the cases V ls less than 80 km s −1 and approximately in 26% of the cases V ls greater than 80 km s −1 were observed.…”

Section: Directed Motions: Methods For Velocity Determinationmentioning

confidence: 99%

Turbulent and directed mass motions in various structures of the low corona

Delone¹,

Yakunina²,

Porfir'eva³

et al. 2007

Int. J. Geomagn. Aeron.

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A brief review on turbulent and ordered plasma motions in the solar corona is presented. Velocities in quiet coronal regions, coronal loops, coronal holes, and cavities around quiescent prominences are analyzed. Data based on interferometric observations of several total solar eclipses obtained earlier by the authors and in addition the values of turbulent velocities resulting from revising the 5303 line profiles were used. Published data based both on ground and space observations in visual and far ultraviolet (UV) spectral region are collected. The turbulent velocities in quiet loop structures and diffuse quiet corona seem to be similar, and the coronal plasma in the vicinity of the quiet protuberances is less turbulent than in the quiet corona or in the coronal holes. Velocities of directed motions for different structures in the corona are examined. It seems that the turbulent velocities are comparable by their magnitudes with the direct plasma velocities; however, at the same time they are slightly less.

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Section: Directed Motions: Methods For Velocity Determinationmentioning

confidence: 99%

Turbulent and directed mass motions in various structures of the low corona

Delone¹,

Yakunina²,

Porfir'eva³

et al. 2007

Int. J. Geomagn. Aeron.

Self Cite

View full text Add to dashboard Cite

show abstract

“…Further, the coronal lines are known to have nonthermal line widths along with the expected thermal line widths (Delone & Makarova 1969, 1975Chae et al 1998). Excess line widths of the order of 15-20 km s −1 were reported by Skylab and Solar Maximum Mission in the coronal forbidden lines.…”

Section: Introductionmentioning

confidence: 96%

Line Profile Studies of Coronal Active Regions in Fe xii λ195.12 Using Hinode/EIS

Prabhakar

Raju

2022

ApJ

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Coronal active regions are studied using Hinode/EIS observations in the EUV line Fe xii λ195.12 by analyzing their line profiles from 2006 December to 2019 December. The period covers the last 2 yr of solar cycle 23 and solar cycle 24 fully. Active regions are the main source of magnetic field in the solar atmosphere, important in its heating and dynamics. Line profiles were obtained from various active regions spread across the Sun on a monthly basis from which we obtained the intensity, line width, Doppler velocity, and centroid and examined their variation during the solar cycle. The histograms of the Doppler velocity and centroid show that they behave in six different ways with respect to the position of rest wavelength. In addition, the shifts in the centroid were found to be more compared to the Doppler velocity. The variation of the line width with respect to the Doppler velocity or the centroid mostly follows a second-degree polynomial. A multicomponent line profile is simulated to explain the difference in the behavior of the Doppler velocity and the centroid with respect to the line width. We also find that the intensity and the line width of the different data sets show a global dependence on the solar cycle with a good correlation. The implications of the results for the coronal heating and dynamics are pointed out.

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Clues to the mode of excitation of Fe x ions in the solar corona from the 1980 eclipse observations

Singh

1985

Sol Phys

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The line and continuum intensities deduced from the multislit spectra of the (Fex) coronal emission line taken at the 1980 eclipse are used to discuss the relative roles of radiative and collisional excitation mechanisms. It is shown that for R/R o < 1.2, collisional excitation is the predominant mode. Collisional as well as radiative excitation is equally important for 1.2 < R/R o < 1.4, whereas beyond 1.4 R e radiative excitation becomes dominant. The line width measurements indicate that a large number of locations have half-widths around 1.3 A. The maximum half-width is reached at ~ 1.4 R o with an average value of 1.6 A.

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Interferometric investigation of the line of sight velocities in ?5303 during the eclipse of 11 September, 1968

Cited by 12 publications

References 9 publications

Turbulent and directed mass motions in various structures of the low corona

Turbulent and directed mass motions in various structures of the low corona

Line Profile Studies of Coronal Active Regions in Fe xii λ195.12 Using Hinode/EIS

Clues to the mode of excitation of Fe x ions in the solar corona from the 1980 eclipse observations

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