Forbidden lines of the solar corona and transition zone - 975-3000 A

Sandlin, G. D.; Brueckner, G. E.; Tousey, R.

doi:10.1086/155320

Cited by 140 publications

(119 citation statements)

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“…Figure 4 shows the emissivity ratio of the 1467.06 Å line from the Sandlin et al (1977) observation 40 above an active region, together with those of new forbidden lines identified here, as described below.…”

Section: Ground Configuration 3s 2 3p 4 and Forbidden Transitionsmentioning

confidence: 95%

“…Sandlin et al (1977) provided an extensive and accurate list of calibrated line intensities and wavelengths in the 970−2650 Å range. They estimated the relative intensities to be accurate within 30% in the 1210−1930 Å range and 50% above 1930 Å, given the large scattered continuum.…”

Section: Coronal Forbidden Linesmentioning

confidence: 99%

“…The energy of level 3 is obtained from the wavelengths of the 3−44 and 2−44 lines observed at 181.131 and 180.595 Å, and the energy of level 2. The energy of level 4, 37 743, is from the strong 1−4 transition observed by Sandlin et al (1977) at 2648.71 Å (air). The wavelength of the 2−4 line observed by Jefferies et al (1971) at 3986.8 Å (air) provides an energy of 37 743.6, in good agreement.…”

Section: Ground Configuration 3s 2 3p 4 and Forbidden Transitionsmentioning

confidence: 99%

“…The energy of level 5 is from the bright 2−5 line observed by Sandlin et al (1977) at 1467.06 Å. Jordan (1971) used the 1970 eclipse observations described by Gabriel et al (1971) to …”

Section: Ground Configuration 3s 2 3p 4 and Forbidden Transitionsmentioning

confidence: 99%

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Benchmarking atomic data for astrophysics: Fe xi

Zanna¹

2010

A&A

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High-resolution spectroscopic observations of the solar corona and laboratory measurements are used to review all the line identifications for Fe xi, from the EUV to the visible. The results of the atomic structure and scattering calculations are presented elsewhere, while detailed comparisons between observed and predicted wavelengths and intensities are discussed here. All the brightest EUV lines in the solar corona are now finally firmly identified. Several new identifications are proposed, in particular, coronal forbidden lines. The previously-known density-diagnostics are confirmed. New and important temperature diagnostics are presented, and the presence of blends highlighted.

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Section: Ground Configuration 3s 2 3p 4 and Forbidden Transitionsmentioning

confidence: 95%

Section: Coronal Forbidden Linesmentioning

confidence: 99%

Section: Ground Configuration 3s 2 3p 4 and Forbidden Transitionsmentioning

confidence: 99%

“…The energy of level 5 is from the bright 2−5 line observed by Sandlin et al (1977) at 1467.06 Å. Jordan (1971) used the 1970 eclipse observations described by Gabriel et al (1971) to …”

Section: Ground Configuration 3s 2 3p 4 and Forbidden Transitionsmentioning

confidence: 99%

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Benchmarking atomic data for astrophysics: Fe xi

Zanna¹

2010

A&A

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“…Sandlin et al (1977) found a net blueshift of 6 km −1 in Fe xii spectra. Peter & Judge (1999) reported a temperature dependence of net Doppler shifts and showed that redshift at 10 5 K could be as large as 10 km s −1 .…”

Section: Gaussian Fittingmentioning

confidence: 93%

Distribution of jets and magnetic fields in a coronal hole

Kamio

Hara

Watanabe

et al. 2009

A&A

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Context. Recent observations of ubiquitous jets in coronal holes suggest that they play an important role in coronal heating and solar wind acceleration. Aims. The aim of our study is to understand the magnetic connectivity and the formation of jets in coronal holes. The study of jets also helps to understand the magnetic field configuration in the coronal hole. Methods. A coordinated observation between EIS and SUMER was carried out in a polar coronal hole to investigate both the transition region and the corona. Spectropolarimeter (SP) data allowed us to examine the relationship between the distribution of jets and magnetic fields in the photosphere. Results. Coronal jets as well as explosive events and cool upflows were identified from EIS and SUMER data. The location of these events are correlated with network fields in the photosphere. Conclusions. Footpoints of coronal jets are connected to patches of vertical kG fields in the photosphere, which are thought to anchor open fields in the upper corona. Explosive events and cool upflows occur in network regions which harbor low-lying fields in the transition region.

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ATOMIC DATA AND SPECTRAL LINE INTENSITIES FOR Mg VI

Bhatia

Young

1998

Atomic Data and Nuclear Data Tables

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Electron collision strengths for Mg VI, calculated in the distorted-wave approximation, are presented for all transitions between the 23 levels of the 2s 2 2p 3 , 2s2p 4 , 2p 5 , and 2s 2 2p 2 3s configurations. Radiative data have been calculated utilizing the same four-configuration model of the ion. Proton rates for the transitions between the ground states are also presented. The level balance equations for Mg VI have been solved using these data and comparisons are made with previous results-excellent agreement is found. Theoretical line intensities for the important transitions are presented and compared with lines found in the extreme ultraviolet in a spectrum from the

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Forbidden lines of the solar corona and transition zone - 975-3000 A

Cited by 140 publications

References 0 publications

Benchmarking atomic data for astrophysics: Fe xi

Benchmarking atomic data for astrophysics: Fe xi

Distribution of jets and magnetic fields in a coronal hole

ATOMIC DATA AND SPECTRAL LINE INTENSITIES FOR Mg VI

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