The Ultraviolet Emission Spectrum of the Solar Chromosphere and Corona

Burton, W. M.; Ridgeley, A.; Wilson, R. G.

doi:10.1093/mnras/135.2.207

Cited by 65 publications

(29 citation statements)

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“…At shorter wavelengths, however, the spectral and spatial resolution were moderate and only strong lines could be observed and/or identified. Spectral catalogues and line lists covering the FUV and EUV portions of the spectrum have previously been published by Burton et al (1967) 1 , Burton & Ridgeley (1970) 1 , Dupree & Reeves (1971), Gabriel et al (1971) 1 , Huber et al (1973) 1 , Malinovsky & Heroux (1973), Kjeldseth-Moe et al (1976), Doschek et al (1976) 1 , Feldman et al (1976aFeldman et al ( , 1976b 1 , Vernazza & Reeves (1978), Dere (1978) 1 , , Cohen et al (1978) 1 , Cohen (1981), Sandlin et al (1986) 1 , Brekke et al (1991), Feldman & Doschek (1991) 1 , Brekke (1993), Thomas & Neupert (1994), Brooks et al (1999).…”

Section: Earlier Spectral Atlasesmentioning

confidence: 99%

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The SUMER spectral atlas of solar-disk features

Curdt

Brekke

Feldman

et al. 2001

A&A

289

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%

“…Spectra covering the 300Å to 2950Å wavelength range with a spectral resolution of about 0.4Å were obtained during a series of rocket flights in the late 1960s and early 1970s by Burton et al (1967), Burton & Ridgeley (1970), and Gabriel et al (1971). Due to low spectral resolution, line shapes could not be obtained.…”

Section: Earlier Spectral Atlasesmentioning

confidence: 99%

The SUMER spectral atlas of solar-disk features

Curdt

Brekke

Feldman

et al. 2001

A&A

289

292

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“…It has now become clear that there is an error in the Z scaling of Griem's transition probabilities, and the theory has been recalculated with semi-empirical values for the forbidden line transition probability (Freeman et al, 1970;Gabriel and Jordan, 1970). Recently, more precise values have been calculated by Drake (1971), and these are in satisfactory agreement with the semi-empirical values used by Freeman et al…”

Section: Helium-like Forbidden Linesmentioning

confidence: 70%

“…The solar limb spectra of Burton et al (1967) enabled Fexi and xn lines to be identified in the region 1200 A-1500 A. This work can be greatly extended by measurements carried out recently during the total eclipse of 7 March, 1970.…”

Section: Transitions Within the Ground Configurationmentioning

confidence: 76%

Some Problems Relating to Solar Line Identification

Gabriel¹

1971

Highlights astron.

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“…A significant achievement resulted from the development of this system when Dr. Wilson's group obtained the chromospheric spectrum in April 1965 by setting the spectrograph slit about 10 sec of arc outside the visible limb with a slit width of 4 sec of arc. The experiment used Kodak Pathe SC-5 and SC-7 Schumann film and recovery techniques (Burton and Wilson, 1965;Burton et al, 1967). …”

Section: Pointing Controls For Rocketsmentioning

confidence: 99%

Recent Techniques in Solar Optical Astronomy from Space

Reeves¹

1968

Highlights astron.

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The article summarizes some of the recent advances in the techniques of solar space research, particularly over the last 4 years, in an attempt to review the current state of instrument technology. The present state of development in rocket and satellite vehicles for solar observations, far ultraviolet detectors, optical materials, ultraviolet reflection coatings, filters, and photographic film fogging, are among the topics described.

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The Ultraviolet Emission Spectrum of the Solar Chromosphere and Corona

Cited by 65 publications

References 0 publications

The SUMER spectral atlas of solar-disk features

The SUMER spectral atlas of solar-disk features

Some Problems Relating to Solar Line Identification

Recent Techniques in Solar Optical Astronomy from Space

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