Energy levels of one-electron atoms

Erickson, Glen W.

doi:10.1063/1.555557

Cited by 382 publications

(189 citation statements)

References 26 publications

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“…Solar X-ray spectra from the Solar Maximum Mission (SMM) and SOLEX also show no feature at 7.22 Å ; instead, they identify a feature at 7.17 Å as Al xiii (Phillips et al 1982;McKenzie et al 1985). The energy levels of Erickson (1977) and Mohr (1985) predict wavelengths of 7.171 and 7.176 Å for the 2 S 1/2 -2 P 3/2 and 2 S 1/2 -2 P 1/2 transitions, respectively. The discrepancy is apparently the result of a typo in transcribing the energy levels of Al xiii and should be corrected in the next version of APED (N. S. Brickhouse 2002, private communication).…”

Section: -(A)mentioning

confidence: 99%

Chandra,Extreme Ultraviolet Explorer, and Very Large Array Observations of the Active Binary System σ²Coronae Borealis

Osten

Ayres

Brown

et al. 2003

ApJ

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We present the results of a coordinated observing campaign on the short-period RS CVn binary 2 Coronae Borealis (F6V þ G0V; P orb ¼ 1:14 days) with the Very Large Array, the Extreme Ultraviolet Explorer, and the Chandra X-Ray Observatory High-Energy Transmission Grating Spectrometer. The radio emission is consistent with previously determined quiescent gyrosynchrotron properties. Multiple flares were seen with Extreme Ultraviolet Explorer, five occurring within two consecutive orbital periods. The first of these flares was observed with Chandra. The Chandra observations of 2 CrB showed no systematic variations of line fluxes, widths, or Doppler shifts with orbital phase, nor any response in line width or offset due to the flare. This is consistent with both stars being equally active coronal emitters. We have developed a self-consistent method of spectral analysis to derive information from the line and continuum emissions concerning the distribution of plasma with temperature and elemental abundances. A bimodal temperature distribution is appropriate for both quiescent and flare intervals, with a stable peak at 6-8 MK and another variable enhancement at higher temperatures, with evidence for significant contribution from temperatures up to 50 MK during the flare, compared to 30 MK during quiescence. The iron abundance is subsolar during quiescence but is enriched by about a factor of 2 during a large flare seen with Chandra. The noble gas elements neon and argon show elevated abundances with respect to iron, but there is no clear evidence for any first ionization potential-based abundance pattern during quiescence or the flare. We have determined coronal electron densities from the helium-like ions O vii, Ne ix, Mg xi, and Si xiii, which imply densities !10 10 cm À3 . There is a small enhancement in the electron densities derived for the flare, but it is not statistically significant. We call attention to electron temperature constraints provided by the ratios of 1s 2 1 S 0 -1snp 1 P 1 transitions of the helium-like ions O vii, Ne ix, Mg xi, and Si xiii. The derived coronal electron pressures change by 1-2 orders of magnitude over a 25% change in temperature, implying nonisobaric coronal conditions. We find no evidence for significant departures from the effectively thin coronal assumption. The electron densities inferred from the soft X-ray spectra are inconsistent with cospatial gyrosynchrotron emission; further observations are necessary to discriminate the relative locations of the radio and soft X-ray-emitting plasma.

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Section: -(A)mentioning

confidence: 99%

Chandra,Extreme Ultraviolet Explorer, and Very Large Array Observations of the Active Binary System σ²Coronae Borealis

Osten

Ayres

Brown

et al. 2003

ApJ

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“…7 The center of gravity of the hyperfine structure of the 1 2 S 1/2 ground state of H lies 1 065 304.313 826 0͑75͒ kHz ͑=͑3 / 4͒⌬ hfs ͒ above the lowest ͑F =0͒ hyperfine level. To obtain this value, we have used the hyperfine splitting ⌬ hfs reported in Ref.…”

Section: The Dissociation Energy Of Hmentioning

confidence: 99%

“…To account for the finite mass of the proton, the electron mass m e is replaced by the reduced mass m r , resulting in the relativistic Dirac eigenvalue with the reduced mass correction 7,27 TABLE II. Energy level intervals and determination of the ionization energy of H 2 in cm −1 .…”

Section: The Dissociation Energy Of Hmentioning

confidence: 99%

Determination of the ionization and dissociation energies of the hydrogen molecule

Liu

Salumbides²,

Hollenstein³

et al. 2009

The Journal of Chemical Physics

188

193

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The transition wave number from the EF 1 ⌺ g + ͑v =0,N =1͒ energy level of ortho-H 2 to the 54p1 1 ͑0͒ Rydberg state below the X + 2 ⌺ g + ͑v + =0,N + =1͒ ground state of ortho-H 2 + has been measured to be 25 209.997 56Ϯ ͑0.000 22͒ statistical Ϯ ͑0.000 07͒ systematic cm −1 . Combining this result with previous experimental and theoretical results for other energy level intervals, the ionization and dissociation energies of the hydrogen molecule have been determined to be 124 417.491 13͑37͒ and 36 118.069 62͑37͒ cm −1 , respectively, which represents a precision improvement over previous experimental and theoretical results by more than one order of magnitude. The new value of the ionization energy can be regarded as the most precise and accurate experimental result of this quantity, whereas the dissociation energy is a hybrid experimental-theoretical determination.

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“…The main source of uncertainty in the Lamb shift is the Bethe logarithm (relative uncertainty of 3.3 × 10 −8 and 1.0×10 −7 or less for the circular and near-circular states, respectively [35]), leading to a negligible uncertainty for our measurement.…”

Section: B Other Sources Of Uncertaintymentioning

confidence: 99%

Measuring the Rydberg constant using circular Rydberg atoms in an intensity-modulated optical lattice

2017

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A method for performing a precision measurement of the Rydberg constant, R∞, using cold circular Rydberg atoms is proposed. These states have long lifetimes, as well as negligible quantumelectrodynamics (QED) and no nuclear-overlap corrections. Due to these advantages, the measurement can help solve the "proton radius puzzle" [Bernauer, Pohl, Sci. Am. 310, 32 (2014)]. The atoms are trapped using a Rydberg-atom optical lattice, and transitions are driven using a recentlydemonstrated lattice-modulation technique to perform Doppler-free spectroscopy. The circular-state transition frequency yields R∞. Laser wavelengths and beam geometries are selected such that the lattice-induced transition shift is minimized. The selected transitions have no first-order Zeeman and Stark corrections, leaving only manageable second-order Zeeman and Stark shifts. For Rb, the projected relative uncertainty of R∞ in a measurement under the presence of the Earth's gravity is 10 −11 , with the main contribution coming from the residual lattice shift. This could be reduced in a future micro-gravity implementation. The next-important systematic arises from the Rb + polarizability (relative-uncertainty contribution of ≈ 3 × 10 −12 ).

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Energy levels of one-electron atoms

Cited by 382 publications

References 26 publications

Chandra,Extreme Ultraviolet Explorer, and Very Large Array Observations of the Active Binary System σ²Coronae Borealis

Chandra,Extreme Ultraviolet Explorer, and Very Large Array Observations of the Active Binary System σ²Coronae Borealis

Determination of the ionization and dissociation energies of the hydrogen molecule

Measuring the Rydberg constant using circular Rydberg atoms in an intensity-modulated optical lattice

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Energy levels of one-electron atoms

Cited by 382 publications

References 26 publications

Chandra,Extreme Ultraviolet Explorer, and Very Large Array Observations of the Active Binary System σ2Coronae Borealis

Chandra,Extreme Ultraviolet Explorer, and Very Large Array Observations of the Active Binary System σ2Coronae Borealis

Determination of the ionization and dissociation energies of the hydrogen molecule

Measuring the Rydberg constant using circular Rydberg atoms in an intensity-modulated optical lattice

Contact Info

Product

Resources

About

Chandra,Extreme Ultraviolet Explorer, and Very Large Array Observations of the Active Binary System σ²Coronae Borealis

Chandra,Extreme Ultraviolet Explorer, and Very Large Array Observations of the Active Binary System σ²Coronae Borealis