1979
DOI: 10.1086/157356
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Extreme-ultraviolet limb spectra of a prominence observed from SKYLAB

Abstract: Line profiles of extreme ultraviolet emission lines observed in a solar prominence at positions above the white-light limb with the NRL slit spectrograph on Skylab are discussed. Absolute line intensities and full widths at half-maximum are presented for lines formed over the temperature range ~1 x 10 4 to 2.2 x 10 5 K. The volume emission measures calculated using resonance line intensities are greater than quiet-Sun emission measures at the same height above the limb and indicate a somewhat different distrib… Show more

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Cited by 30 publications
(21 citation statements)
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“…To account for the observed emission intensity, therefore, the effective prominence width (i.e., column depth) would be smaller if the heating were steady rather than impulsive. Skylab slitspectrograph observations of a limb prominence yielded a column depth of around 1200 km at transition-region temperatures (Mariska et al 1979), which is comparable to our lower estimate. The observed prominence width typically is much larger, indicating small filling factors, which is consistent with their wispy appearance in high-resolution images.…”
Section: Differential Emission Measuresupporting
confidence: 86%
“…To account for the observed emission intensity, therefore, the effective prominence width (i.e., column depth) would be smaller if the heating were steady rather than impulsive. Skylab slitspectrograph observations of a limb prominence yielded a column depth of around 1200 km at transition-region temperatures (Mariska et al 1979), which is comparable to our lower estimate. The observed prominence width typically is much larger, indicating small filling factors, which is consistent with their wispy appearance in high-resolution images.…”
Section: Differential Emission Measuresupporting
confidence: 86%
“…Preliminary results indicate that, contrary to the expectations, the prominence appears to contain hotter material at lower rather than at greater heights and, in addition, confirm earlier results (Feldman and Doschek 1977b;Mariska et al 1979;) that the line widths in a prominence are narrower than in quiet-Sun areas.…”
Section: Prominencessupporting
confidence: 78%
“…Their widths smoothly increase with T f orm . We consider this increase to be real, since Mariska, Doschek, and Feldman (1979) found comparable widths ∆λ e /λ = 8 · 10 −5 and a similar increase with T f orm , which they interpreted as a discontinuity of the non-thermal velocities between cool and hot emitting material. This increase of line widths is particularly pronounced in prominence E/70N (Fig.…”
Section: The Broader 'Hot' Linesmentioning
confidence: 78%
“…If we apply the revised correction with broader instrumental profiles by Chae, Schühle, and Lemaire (1998), the resulting widths 5 · 10 −5 < ∆λ e /λ < 9 · 10 −5 are still significantly broader than those obtained by Mariska, Doschek, and Feldman (1979) from observations with the NRL slit spectrograph on Skylab (at a spectral resolution of 60 mÅ). Interestingly, their reduced widths of lines from neutral and singly charged atoms of typically ∆λ e /λ ≈ 3 · 10 −5 are very near to those of our Ca IR line (entered in Figs.…”
Section: Correction Of Narrow Lines For the Sumer Profilementioning
confidence: 88%