Spectral and Photometric Measurements of Solar X-Ray Emission Below 60 Å

Blake, R. L.; Chubb, T. A.; Friedman, H.; Unzicker, Alexander

doi:10.1086/148258

Cited by 79 publications

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“…In 1963, using a rocket borne crystal spectrometer, Blake et al [3] measured the first high-resolution Solar spectrum that included Fe XVII X-ray lines. The spectrometer employed no slits for these measurements, so the spectrum included emission from the entire Solar disk.…”

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confidence: 99%

A brief review of the intensity of lines 3C and 3D in neon-like Fe XVII

Brown¹

2008

Can. J. Phys.

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X-ray emission from neon-like Fe XVII has been measured with high-resolution spectrometers from laboratory or celestial sources for nearly seven decades. Two of the strongest lines regularly identified in these spectra are the 1P1 → 1S0 resonance and the 3D1 → 1S0 intercombination line, known as 3C and 3D, respectively. This paper gives a brief overview of measurements of the intensities of the lines 3C and 3D from laboratory and celestial sources and their comparison to model calculations, with an emphasis on measurements completed using an electron beam ion trap. It includes a discussion of the measured absolute cross sections compared with results from modern atomic theory calculations as well as the diagnostic utility of the relative intensity, R = I3C/I3CD, as it applies to the interpretation of spectra measured from the Sun and extra-solar sources. PACS Nos.: 32.30.Rj, 32.30.–r, 32.70.Cs, 52.72.+v, 95.85.Nv, 96.60.P–, 97.10.Ex

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confidence: 99%

A brief review of the intensity of lines 3C and 3D in neon-like Fe XVII

Brown¹

2008

Can. J. Phys.

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“…In Figures 2 and 3 a comparison is made with measurements performed by Ariel II in 1962(POUNDS, 1965 and by the Naval Research Laboratory in 1963 (BLAKE et al, 1965). The two measurements of July 6 and 23 coincide with optical flares of importance 1 and 1 -, both in their beginning phase.…”

Section: I(n)/i(o) Curves Fits To the Corresponding Curve Inmentioning

confidence: 80%

Determination of the solar X-ray spectrum by using the atmospheric extinction

Landini¹

1967

Sol Phys

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“…The corresponding potentials were computed by BELY (1967). The radial wave functions were computed using the modified quantumdefect method devised by BURGESS (1966). This method is quite similar to the method proposed by STEWART and ROTENBERG (1965).…”

Section: Theorymentioning

confidence: 99%

“…These results are in fairly good agreement. Using these oscillator strengths, POTTASCH (1966) was able to compute the excitation cross-sections for the permitted transitions by the impact parameter method of BURGESS (1962); computing then the line-intensity ratios he found a strong disagreement with the observed ones. His conclusion is that some excitation cross-sections corresponding to the forbidden transition 2p6-+2p 5 3p are certainly not negligible.…”

Section: Introductionmentioning

confidence: 99%

The excitation of Fe XVII by electron impacts

Bely

1967

Sol Phys

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The cross-sections for the excitation of Fexvu are computed using the Coulomb-Born approximation. For the excitation of the configurations 2p ~ 3s, 2p 5 3p and 2p 5 3d, the intermediate coupling scheme is used, while an extrapolation is made for the excitation of the 2s 2p 6 3s, 2s 2p 6 3p and 2s 2p 6 3d configurations from the results obtained earlier in the lithium-like ions. It is found that the excitation cross-section Q (2p 61S0--+2p5 3p 1S0) is fairly large and partly removes the disagreement between the theoretical and experimental intensity-line ratios.

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Spectral and Photometric Measurements of Solar X-Ray Emission Below 60 Å

Cited by 79 publications

References 0 publications

A brief review of the intensity of lines 3C and 3D in neon-like Fe XVII

A brief review of the intensity of lines 3C and 3D in neon-like Fe XVII

Determination of the solar X-ray spectrum by using the atmospheric extinction

The excitation of Fe XVII by electron impacts

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