Experimental isotope shifts of the 5 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow /><mml:mn>2</mml:mn></mml:msup><mml:mspace width="-0.16em" /><mml:msub><mml:mi>S</mml:mi><mml:mrow><mml:mn>1</mml:mn><mml:mo>/</mml:mo><mml:mn>2</mml:mn></mml:mrow></mml:msub></mml:mrow></mml:math>state and low-lying excited states of Rb

Aldridge, Leland; Gould, P. L.; Eyler, E. E.

doi:10.1103/physreva.84.034501

Cited by 9 publications

(5 citation statements)

References 24 publications

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“…III a comparison between the literature values and the newly determined values is shown. The total isotope shifts were found to be 41.935(60) MHz for the 6P 3/2 isotopes and 41.237(62) MHz for the 6P 1/2 isotopes, which agree well with the literature values [26,27]. With the determined hyperfine splitting values, the magnetic dipole constant A and the electric quadrupole constant B can be calculated for the 5S → 6P transitions.…”

Section: Discussionsupporting

confidence: 86%

Absolute frequency measurement of rubidium 5S-6P transitions

Glaser,

Karlewski,

Grimmel

et al. 2019

Preprint

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We report on measurements on the 5S-6P rubidium transition frequencies for rubidium isotopes with an absolute uncertainty of better than 450 kHz for the 5S → 6P 1/2 transition and 20 kHz for the 5S → 6P 3/2 transition, achieved by saturation absorption spectroscopy. From the results we derive the hyperfine splitting with an accuracy of 460 kHz and 30 kHz, respectively. We also verify the literature values for the isotope shifts as well as magnetic dipole constant and the electric quadrupole constant.

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Section: Discussionsupporting

confidence: 86%

Absolute frequency measurement of rubidium 5S-6P transitions

Glaser,

Karlewski,

Grimmel

et al. 2019

Preprint

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“…The data of the hyperfine splittings and isotope shifts for Rb [14,19,20], In [13,15], K [14,21,22], and Ga [13,15,23] are combined with our measurements to calculate the center-of-mass frequencies.…”

Section: Absolute Frequenciesmentioning

confidence: 99%

Comparison of resonance frequencies of major atomic lines in 398–423 nm

et al. 2016

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It has been highly developed along with the progress of next-generation atomic clocks in the visible frequency range, which require Hz-level stabilization of the laser [1]. Such an etalon is not expensive and can also be a convenient tool to determine absolute frequencies of lasers. For example, the absolute frequencies of water molecule lines near 790 nm have been accurately determined by using an ultralow-expansion etalon calibrated to the D 1 and D 2 lines of rubidium atoms [2,3]. To investigate many resonance lines spread in a span of a few tens of nanometer using such an etalon, the change of the free spectral range of the etalon due to the dispersion of the mirrors has to be taken into account.In this paper, we report high-resolution spectroscopy for transitions from the ground states of Ca, Rb, In, K, Ga, and Yb atoms in the 398-423 nm spectral range, using this kind of etalon for which small group-delay-dispersion (GDD) mirrors are attached. In this wavelength range the use of the etalon is especially efficient, since it is very difficult to directly measure laser frequencies with optical frequency combs for this range without using a frequency doubling system. The etalon resonance frequencies are calibrated to the absolute frequencies of Ca at 423 nm and Rb at 422 nm, whose uncertainties are less than 0.4 MHz [4,5]. Except these two atomic lines, the absolute frequencies of the atomic lines observed in this paper have not been determined precisely so far. Recent development of violet and blue laser diodes has promoted the spectroscopy of this spectral range, and thus, these atomic line data are of increasing importance. For example, these lines have been utilized for laser cooling, which essentially requires the stabilization of the laser frequency. Bose-Einstein condensates of Ca and Yb have been realized [6,7], and these lines observed in this study are the main cooling transitions. The cooling of In and Ga atomic Abstract We have demonstrated spectroscopy of Ca, Rb, In, K, Ga, and Yb atomic lines in 398-423 nm. Using an etalon of an ultralow-expansion coefficient, we have determined ratios of the resonance frequencies of these atoms. The etalon has small group-delay-dispersion mirrors to be an accurate frequency reference over a wavelength span of a few tens of nanometer. The etalon resonance frequencies are calibrated with accurately known transition frequencies of Ca at 423 nm and Rb at 422 nm. Based on this calibration, the absolute frequencies are also determined for some atomic lines with smaller uncertainties than earlier reports.

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“…The line at λ7800 Å of interest here is a hyperfine multiplet produced by the transition 2 S 1/2 − 2 P 3/2 . The isotopic shifts δ = E 85 − E 87 , that is, the energy difference for a given level between the level for 85 Rb and 87 Rb are: δ( 2 S 1/2 ) = 164.35 MHz, and δ( 2 P 3/2 ) = 86.31 MHz, respectively (Aldridge et al 2011). The hyperfine effective Hamiltonian was parametrised in terms of the magnetic-dipole and electricquadrupole hyperfine structure constants.…”

Section: Zeeman Broadeningmentioning

confidence: 99%

Rubidium abundances in solar metallicity stars

Abia

Laverny

Коротин

et al. 2021

A&A

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Context. Rubidium is one of the few elements produced by the neutron capture s- and r-processes in almost equal proportions. Recently, a Rb deficiency ([Rb/Fe] < 0.0), amounting to a factor of about two with respect to the Sun, has been found in M dwarfs of near-solar metallicity. This stands in contrast to the close-to-solar [Sr, Zr/Fe] ratios derived in the same stars. This deficiency is difficult to understand from the point of view of observations and of nucleosynthesis. Aims. To test the reliability of this Rb deficiency, we study the Rb and Zr abundances in a sample of KM-type giant stars across a similar metallicity range, extracted from the AMBRE Project. Methods. We used high-resolution and high signal-to-noise spectra to derive Rb and Zr abundances in a sample of 54 bright giant stars with metallicities in the range of −0.6 ≲ [Fe/H] ≲ +0.4 dex, via spectral synthesis in both local and non-local thermodynamic equilibrium (LTE and NLTE, respectively). We also studied the impact of the Zeeman broadening in the profile of the Rb I at λ7800 Å line. Results. The LTE analysis also results in a Rb deficiency in giant stars, however, it is considerably lower than that obtained in M dwarfs. However, once NLTE corrections are performed, the [Rb/Fe] ratios are very close to solar (average −0.01 ± 0.09 dex) in the full metallicity range studied here. This stands in contrast to the value found for M dwarfs. The [Zr/Fe] ratios derived are in excellent agreement with those obtained in previous studies in FGK dwarf stars with a similar metallicity. We investigate the effect of gravitational settling and magnetic activity as possible causes of the Rb deficiency found in M dwarfs. Although the former phenomenon has a negligible impact on the surface Rb abundance, the presence of an average magnetic field with an intensity that is typical of that observed in M dwarfs may result in systematic Rb abundance underestimations if the Zeeman broadening is not considered in the spectral synthesis. This may explain the Rb deficiency in M dwarfs, but not fully. On the other hand, the new [Rb/Fe] and [Rb/Zr] versus [Fe/H] relationships can be explained when the Rb production by rotating massive stars and low-to-intermediate mass stars (these latter also producing Zr) are considered, without the need to deviate from the standard s-process nucleosynthesis in asymptotic giant branch stars, as suggested previously.

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Experimental isotope shifts of the 5 2S1/2state and low-lying excited states of Rb

Cited by 9 publications

References 24 publications

Absolute frequency measurement of rubidium 5S-6P transitions

Absolute frequency measurement of rubidium 5S-6P transitions

Comparison of resonance frequencies of major atomic lines in 398–423 nm

Rubidium abundances in solar metallicity stars

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