How accurate are the ‘‘muonic’’ quadrupole moments in Eu?

Möller, W.; Hühnermann, H.; Alkhazov, G.; Пантелеев, В. В.

doi:10.1103/physrevlett.70.541

Cited by 20 publications

(15 citation statements)

References 17 publications

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“…The agreement between our values of the A factors and the values obtained with a Fabry-Perot spectrometer is good considering that the hfs in [2,3] was only partially resolved (FWHM in the order of 1 GHz) and the hfs was analyzed using a parametrization procedure. Our values of the B factors agree very well with the values in [ 11 ].…”

Section: Resultssupporting

confidence: 87%

“…The A and B factors are derived from the well-known expression for the energy contributions from the magnetic dipole and electric quadrupole interactions and are corrected for the differential Doppler shift (0.071%). The results are given in Table 1 together with other results obtained with the laser-ion beam technique [11 ], and results obtained with a double Fabry-Perot spectrometer [2,3]. The values presented in this work are the weighted mean of the results achieved for the different transitions with a common upper or lower level (c.f.…”

Section: Methodsmentioning

confidence: 94%

“…The uncertainty is the statistical spread with a 70% confidence interval, giving an estimated maximum systematic uncertainty of 0.035% to the measured frequency differences in the spectra. 2.269(6) 0.392 (7) U,(151)/ttx(153 ) [16] 2.2646(12) Optical data [11 ] 0.39191(12) Muonic data [17] 0.374(6) Optical data (9S4°) [12] 2.25018 64.85t3 "corrected" optical data (9S°) [12] 2.25003 0.3770 (2) netic dipole moments are ~r(151)=3.417 (6) n.m., ~z(153)= 1.5330(8) n.m. [16], and the electric quadrupole moments are Q(151)=0.903(10) barn, Q(153)= 2.412(21) barn [17], giving a large number of well separated hfs components of which the AF=AJ are the strongest. The spectral linewidth is about 60MHz (FWHM) and arises mainly from longitudinal Doppler broadening, due to the ion source energy spread, and natural lifetime broadening.…”

Section: Methodsmentioning

confidence: 99%

“…1). M61-ler et al [11] have extended the measurements to the 4 f7 (8SO/2)6p~/2; j= 3, 4 levels but their complete results…”

Section: Introductionmentioning

confidence: 95%

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Hyperfine structure of the 4f 7 (8 S 0) 6s 7 S 03 level in151,153Eu II by fast ion beam — laser spectroscopy

Villemoes

Wang

1994

Z Phys D - Atoms, Molecules and Clusters

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Section: Resultssupporting

confidence: 87%

Section: Methodsmentioning

confidence: 94%

Section: Methodsmentioning

confidence: 99%

“…1). M61-ler et al [11] have extended the measurements to the 4 f7 (8SO/2)6p~/2; j= 3, 4 levels but their complete results…”

Section: Introductionmentioning

confidence: 95%

See 2 more Smart Citations

Hyperfine structure of the 4f 7 (8 S 0) 6s 7 S 03 level in151,153Eu II by fast ion beam — laser spectroscopy

Villemoes

Wang

1994

Z Phys D - Atoms, Molecules and Clusters

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“…In the spectral synthesis calculations, the Eu  line was substituted by its HFS components, calculated by us using Casimir's equation (Casimir 1963), and HFS laboratory data from Becker et al (1993), Broström et al (1995), Villemoes & Wang (1994), and Möller et al (1993). Isotope shift was taken into account, using data from Broström et al (1995) and the solar abundance isotopic ratio ε( 151 Eu)/ε( 153 Eu) = 1.00 ± 0.29 (Lawler et al 2001).…”

Section: Spectral Synthesismentioning

confidence: 99%

The age of the Galactic thin disk from Th/Eu nucleocosmochronology

Peloso¹,

Silva²,

Mello³

2005

A&A

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Abstract. The purpose of this work is to resume investigation of Galactic thin disk dating using nucleocosmochronology with Th/Eu stellar abundance ratios, a theme absent from the literature since 1990. A stellar sample of 20 disk dwarfs/subgiants of F5 to G8 spectral types with −0.8 ≤ [Fe/H] ≤ +0.3 was selected. In stars with such spectral types and luminosity classes, spectral synthesis techniques must be employed if we wish to achieve acceptably accurate results. An homogeneous, self-consistent set of atmospheric parameters was determined. Effective temperatures were determined from photometric calibrations and Hα profile fitting; surface gravities were obtained from T eff , stellar masses and luminosities; microturbulence velocities and metallicities were obtained from detailed, differential spectroscopic analysis, relative to the Sun, using equivalent widths of Fe  and Fe  lines. Chemical abundances of the elements that contaminate the Th and Eu spectral regions (Ti, V, Cr, Mn, Co, Ni, Ce, Nd, and Sm) were determined through spectroscopic analysis. Abundance uncertainties were thoroughly scrutinised, their average value -(0.10 ± 0.02) dex -being found to be satisfactorily low. Eu and Th abundances were determined by spectral synthesis of one Eu  line (4129.72 Å) and one Th  line (4019.13 Å), taking into account the detailed hyperfine structures of contaminating Co lines, as well as the hyperfine structure and isotope shift of the Eu line. Comparison of our abundances with literature data shows that our results exhibit a similar behaviour, but a considerably lower scatter (36% lower for Eu, and 61% lower for Th). The [Th/Eu] abundance ratios thus obtained were used, in the second paper of this series, to determine the age of the Galactic disk.

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