Erratum

Bartoe, John-David F.; Brueckner, G. E.

doi:10.1364/josa.65.000617

Cited by 17 publications

(18 citation statements)

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“…HRTS, which operated at wavelengths longer than 1150Å, was the first spectrometer to combine both high spectral resolution (50 mÅ) and good angular resolution (1 ) with extensive wavelength and spatial coverage (Bartoe & Brueckner 1975). It was launched several times on sounding rockets and was part of the 5 day Spacelab 2 mission.…”

Section: Earlier Spectral Atlasesmentioning

confidence: 99%

The SUMER spectral atlas of solar-disk features

Curdt

Brekke

Feldman

et al. 2001

A&A

294

292

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Abstract.A far-ultraviolet and extreme-ultraviolet (FUV, EUV) spectral atlas of the Sun between 670Å and 1609Å in the first order of diffraction has been derived from observations obtained with the SUMER (Solar Ultraviolet Measurements of Emitted Radiation) spectrograph on the spacecraft SOHO (Solar and Heliospheric Observatory). The atlas contains spectra of the average quiet Sun, a coronal hole and a sunspot on the disk. Different physical parameters prevalent in the bright network (BN) and in the cell interior (CI) -contributing in a distinct manner to the average quiet-Sun emission -have their imprint on the BN/CI ratio, which is also shown for almost the entire spectral range. With a few exceptions, all major lines are given with their identifications and wavelengths. Lines that appear in second order are superimposed on the first order spectra. These lines are clearly marked in the atlas. The spectra include emissions from atoms and ions in the temperature range 6 × 10 3 K to 2 × 10 6 K, i.e., continua and emission lines emitted from the lower chromosphere to the corona. This spectral atlas, with its broad wavelength coverage, provides a rich source of new diagnostic tools to study the physical parameters in the chromosphere, the transition region and the corona. In particular, the wavelength range below 1100Å as observed by SUMER represents a significant improvement over the spectra produced in the past. In view of the manifold appearance and temporal variation of the solar atmosphere, it is obvious that our atlas can only be a -hopefully typical -snapshot. Brief descriptions of the data reduction and calibration procedures are given. The spectral radiances are determined with a relative uncertainty of 0.15 to 0.30 (1σ) and the wavelength scale is accurate to typically 10 mÅ. The atlas is also available in a machine readable form.

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Section: Earlier Spectral Atlasesmentioning

confidence: 99%

The SUMER spectral atlas of solar-disk features

Curdt

Brekke

Feldman

et al. 2001

A&A

294

292

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“…VAULT consists of a 30 cm Cassegrain telescope followed by a zero-dispersion spectroheliograph (Bartoe & Brueckner 1978). It is designed to operate close to the Lya Rayleigh di †raction limit with an angular ( D 0A .1) resolution of and a bandpass of 70 The light is 0A .33…”

Section: Instrument Description and Observationsmentioning

confidence: 99%

On the Correlation between Coronal and Lower Transition Region Structures at Arcsecond Scales

Vourlidas

Klimchuk

Korendyke

et al. 2001

ApJ

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We compare the morphology of active region structures observed in the 171 (T D 9 ] 105 K) and A Lya (T D 2 ] 104 K) lines. The coronal data were obtained by the T ransition Region and Coronal Explorer (T RACE) in support of the Very High Angular Resolution Ultraviolet Telescope (VAULT) sounding rocket launch, which acquired subarcsecond resolution images of an active region in the Lya line, on 1999 May 7. Using a pair of calibrated, nearly simultaneous images, we Ðnd that : (i) a very good correlation exists between the Lya and 171 intensities in the T RACE moss regions, (ii) we can identify A several identical structures in some (but not all) moss areas, and (iii) the correlations are greatly reduced at the footpoints of the 171 large-scale loops. We derive a lower limit for the Lya emission measure, A under the assumption of e †ectively optically thin emission, and compare it to the 171 emission A measure. As in previous studies, we Ðnd an excess of Lya material compared to the amount expected for a thermal conduction-dominated corona-chromosphere transition region, even for structures that appear to be identical in the two wavelengths. This result implies that some other mechanism besides classical heat conduction from the corona must contribute to the observed Lya intensities. The observations do not support the idea of a physically distinct cool loop component within active regions.

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“…Using empirical results Spicer (1979) On the other hand Nicolas at al (1979) using high resolution data ( -I" ) from the HRTS instrument (Bartoe and Brueckner 1975) in ED mechanisms and this automatically imposes strong constraints on both the topology of B and its magnitude.…”

Section: Microsoopie Effeeta and Transport Parametersmentioning

confidence: 99%

“…The problem of studying the propagation of hydromagnetic waves without recourse to the eikonal approximation was not addressed until after Belcher and Davis (1971) observed what appeared to be A1fv4n waves propagating in the solar wind with periods of the order of hours. Holl we$ (1972,1978,1980) recognized the important implications of such observatious and was the first to develop a model of Alfve'n wave w, l,; .^_o►x 4n the solar atmosphere without the restriction of the M ml though his analysis disregards various damping mechanisms, it does indicate that long period Alfvin waves of the order of hours can propagate through the chromosphere with sufficient power ( p _ 10 4 -10 5 ergs cm-2 see-') to strongly affect the solar wind and heat at least the quiet solar corona.…”

Section: Iv12 Propagation Of Electrodynamic Energy Under Certain Cmentioning

confidence: 99%