Measurement of relative oscillator strengths for Mn I. Transitions from levels in the range 0 eV &lt;   &lt;   3 eV

Booth, Anthony J.; Blackwell, D. E.; Petford, A. D.; Shallis, M. J.

doi:10.1093/mnras/208.1.147

Cited by 50 publications

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“…It can be seen that our oscillator strengths for the transitions from the z 6 P • J levels agree, to within the uncertainty, with the previous UV and visible measurements by Booth et al (1984). There is also a good agreement with our laboratory log(g f ) values for the transitions from the z 6 P • J levels and the semiempirical calculated log(g f ) values of Kurucz & Bell (1995).…”

Section: Introductionsupporting

confidence: 89%

“…There is also a good agreement with our laboratory log(g f ) values for the transitions from the z 6 P • J levels and the semiempirical calculated log(g f ) values of Kurucz & Bell (1995). The measured log(g f ) values for UV transitions from the z 4 P • J levels agree with both Booth et al (1984) and Kurucz & Bell (1995) to within the uncertainties. However, the semi-empirical log(g f ) values of Kurucz & Bell (1995) for IR transitions from the z 4 P • J levels are approximately 30% (0.12 dex where the unit dex is log 10 of the ratio of the two values) stronger than our values.…”

Section: Introductionsupporting

confidence: 86%

“…To assist in the correct interpretation of the oscillator strengths in Table 1 we provide wavenumbers, wavelengths and oscillator strengths in Table 2 for the HFS component lines in the IR transitions 3d 6 ( 5 D)4s a 6 D J −3d 5 ( 6 S)4s4p z 6 P • J and 3d 6 ( 5 D)4s a 4 D J −3d 5 ( 6 S)4s4p z 4 P • J . The wavenumber of each transition from the upper hyperfine structure level to the lower hyperfine structure level, σ HFS trans , The previous laboratory log(g f )s from Booth et al (1984), the uncertainties in the log(g f )s of Booth et al (1984) are those assigned by NIST, Fuhr & Wiese (2003). ( f ) Semi-empirical log(g f ) calculations of Kurucz & Bell (1995).…”

Section: Introductionmentioning

confidence: 99%

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Infrared Mn i laboratory oscillator strengths for the study of late type stars and ultracool dwarfs

Blackwell-Whitehead

Pavlenko

Nave

et al. 2010

A&A

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Aims. The aim of our new laboratory measurements is to measure accurate absolute oscillator strengths for neutral manganese transitions in the infrared needed for the study of late-type stars and ultracool dwarfs. Methods. Branching fractions have been measured by high resolution Fourier transform spectroscopy and combined with radiative level lifetimes in the literature to yield oscillator strengths.Results. We present experimental oscillator strengths for 20 Mn i transitions in the wavelength range 3216 to 13 997 Å, 15 of which are in the infrared. The transitions at 12 899 Å and 12 975 Å are observed as strong features in the spectra of late-type stars and ultracool dwarfs. We have fitted our calculated spectra to the observed Mn i lines in spectra of late-type stars. Using the new experimentally measured Mn i log(g f ) values together with existing data for Mn i hyperfine structure splitting factors we determined the manganese abundance to be log N(Mn) = −6.65 ± 0.05 in the atmosphere of the Sun, log N(Mn) = 6.95 ± 0.20 in the atmosphere of Arcturus, and log N(Mn) = −6.70 ± 0.20 in the atmosphere of M 9.5 dwarf 2MASSW 0140026+270150.

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Section: Introductionsupporting

confidence: 89%

Section: Introductionsupporting

confidence: 86%

Section: Introductionmentioning

confidence: 99%

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Infrared Mn i laboratory oscillator strengths for the study of late type stars and ultracool dwarfs

Blackwell-Whitehead

Pavlenko

Nave

et al. 2010

A&A

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“…The large photospheric -meteoritic difference may be due to unaccounted uncertainties in the photospheric calculations introduced by the different techniques used to determine oscillator strengths in previous laboratory measurements. Blackwell & Collins (1972) and Booth et al (1984a) both used absorption techniques to determine oscillator strengths. In particular, Booth et al (1984a) quotes uncertainties as low as 3 per cent, but Booth's uncertainties have been been independently moderated in the NIST (National Institute of Standards and Technology, USA) atomic spectra database to be of the order of 10 to 20 per cent, see Fuhr & Wiese (2003).…”

Section: Laboratory Oscillator Strengthsmentioning

confidence: 99%

“…Blackwell & Collins (1972) and Booth et al (1984a) both used absorption techniques to determine oscillator strengths. In particular, Booth et al (1984a) quotes uncertainties as low as 3 per cent, but Booth's uncertainties have been been independently moderated in the NIST (National Institute of Standards and Technology, USA) atomic spectra database to be of the order of 10 to 20 per cent, see Fuhr & Wiese (2003). Greenlee & Whaling (1979) used emission spectroscopy to determine oscillator strengths, and their measurements include many of the transitions relevant to our current study of the solar photosphere, but the uncertainty in their oscillator strengths is of the order 25 per cent.…”

Section: Laboratory Oscillator Strengthsmentioning

confidence: 99%

A revision of the solar manganese abundance using new and remeasured laboratory oscillator strengths

Blackwell-Whitehead¹,

Bergemann²

2007

A&A

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Context. The solar photospheric element abundances are generally in good agreement with the meteoritic CI chondrite abundances, with the exception of a small number of elements including manganese. The solar photospheric abundances, determined using model atmospheres, include laboratory oscillator strengths where available. However, the current laboratory database for Mn i oscillator strengths is derived from several different laboratory observations determined from several different laboratory techniques. The uncertainty in the solar photospheric manganese abundance and the difference between it and the meteoritic CI chondrite abundance may just be an artefact of inaccurate laboratory data. Aims. The aim of our new laboratory measurements is to measure a self consistent set of accurate absolute oscillator strengths and use the new laboratory data to re-evaluate the solar manganese abundance. Methods. New and more accurate oscillator strengths have been determined by combining branching fractions with previously measured energy level lifetimes. Using the new laboratory data, the solar photospheric abundance of manganese has been determined with theoretical and semi-empirical model atmospheres, MAFAGS-ODF and Holweger & Müller, respectively.Results. We present experimental oscillator strengths for 94 Mn i transitions covering the wavelength range 2384 to 17 744 Å. Using 22 relatively un-blended solar Mn i transitions, we determine the photospheric abundance of manganese to be log ε = 5.37±0.05 dex. Conclusions.The new value is in good agreement with previous photospheric abundance determinations. The implications for the solar photospheric and meteoritic CI chondrite abundance is discussed.

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Stellar Evolution in Globular Clusters

Carney

Saas-Fee Advanced Courses

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Measurement of relative oscillator strengths for Mn I. Transitions from levels in the range 0 eV < < 3 eV

Cited by 50 publications

References 0 publications

Infrared Mn i laboratory oscillator strengths for the study of late type stars and ultracool dwarfs

Infrared Mn i laboratory oscillator strengths for the study of late type stars and ultracool dwarfs

A revision of the solar manganese abundance using new and remeasured laboratory oscillator strengths

Stellar Evolution in Globular Clusters

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