Hyperfine structure measurements for lines of astrophysical interest in Mn I

Booth, Anthony J.; Shallis, M. J.; Wells, Matthew P.

doi:10.1093/mnras/205.1.191

Cited by 32 publications

(18 citation statements)

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“…This seems unlikely. Second, instead of using the Kurucz line list, we extracted from Tables 1, 5, and 6 of Vitas & Vince (2003) the HFS components of the 5420 Å and 5432 Å lines, which are based on the laboratory measurements of Booth et al (1983). We retained the uncorrected wavelength and oscillator strength values (the "λ " and "log(g f ) " ones).…”

Section: The Extremely Metal-poor (Emp) Starsmentioning

confidence: 99%

Manganese in dwarf spheroidal galaxies

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Cescutti

Jablonka

et al. 2012

A&A

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We provide manganese abundances (corrected for the effect of the hyperfine structure) for a large number of stars in the dwarf spheroidal galaxies Sculptor and Fornax, and for a smaller number in the Carina and Sextans dSph galaxies. Abundances had already been determined for a number of other elements in these galaxies, including α and iron-peak ones, which allowed us to build ] for the dSph galaxies is clearly systematically offset from that for the Milky Way, which reflects the different star formation histories of the respective galaxies. The [Mn/α] behavior can be interpreted as a result of the metal-dependent Mn yields of Type II and Type Ia supernovae. We also computed chemical evolution models for star formation histories matching those determined empirically for Sculptor, Fornax, and Carina, and for the Mn yields of SNe Ia, which were assumed to be either constant or variable with metallicity. The observed [Mn/Fe] versus [Fe/H] relation in Sculptor, Fornax, and Carina can be reproduced only by the chemical evolution models that include a metallicitydependent Mn yield from the SNe Ia.

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Section: The Extremely Metal-poor (Emp) Starsmentioning

confidence: 99%

Manganese in dwarf spheroidal galaxies

North

Cescutti

Jablonka

et al. 2012

A&A

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“…The Al abundance has been corrected to account for non-LTE effects by using values interpolated from Table 1 of Baumü ller & Gehren (1997). Hyperfine structure was taken into account for Mn (data from Booth, Shallis, & Wells 1983) and Ba, for which we used data from Steffen (1985).…”

Section: Abundancesmentioning

confidence: 99%

Stellar Archaeology: A Keck Pilot Program on Extremely Metal-Poor Stars From the Hamburg/ESO Survey. III. The Lead (P[CLC]b[/CLC]) Star HE 0024−2523

Lucatello

Gratton

Cohen

et al. 2003

The Astronomical Journal

128

147

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We present a detailed abundance analysis, including spectral syntheses, of a very metal-poor ([Fe/H] ' À2.7) peculiar main-sequence star (HE 0024À2523) detected during the course of the Keck Pilot Program. Radial velocities of this star were obtained during four different observing runs over a time span of 1.1 yr and demonstrate that it is clearly a short-period spectroscopic binary. An orbital solution was obtained, and orbital parameters were determined with high precision. The rotational velocity was also measured (v rot sin i = 9.7 AE 1.5 km s À1 ); rotation appears likely to be synchronous with the orbit. The abundance analysis and spectral syntheses indicate that the object is a CH star characterized by extreme s-process enrichment, likely due to mass accretion from an evolved companion that has now probably become a white dwarf. The lead (Pb) abundance of (HE 0024À2523) is very high, the same as that of the recently discovered lead-rich, metal-poor star CS 29526-110, [Pb/Fe] = +3.3. The abundance ratio of the heavy to light s-elements, as characterized by Pb and Ba, [Pb/Ba] = +1.9, is the highest yet found for any metal-poor star and is about 0.7 dex higher than that of CS 29526-110. On the basis of the measured isotopic ratio of carbon (C 12 /C 13 $ 6) we argue that the mass donor must have had an original mass of at least $3 M . The unusually short period of this CH star suggests that it underwent a past common-envelope phase with its evolved companion. Our results are compared with the latest available models for asymptotic giant branch yields and s-process nucleosynthesis. We also discuss the possible connection between HE 0024À2523, the lithium depletion of halo stars, and halo blue straggler formation.

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“…It is also important to take the hyperfine interactions in the observational profiles into account for analyzing the strengths of the stellar absorption lines (Booth et al 1983). Transition lines from the hyperfine levels in the highly charged ions can facilitate observations of the hot rarefied astrophysical plasma (Sunyaev & Docenko 2007).…”

Section: Introductionmentioning

confidence: 99%

Spectral properties of a few F-like ions

Nandy

Sahoo

2014

A&A

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Aims. We intend to provide accurate data for the oscillator strengths, transition probabilities, lifetimes, and hyperfine shifts of the atomic energy levels in the fluorine (F)-like Ti, V, Cr, Mn, Co, Ni, Cu, Zn, and Mo ions for the diagnostic of the astrophysical plasma. Furthermore, we propose these ions for probing possible variation in the fine structure constant (α e ) by observing their transition lines from the distant astronomical objects. Methods. We have employed an all-order perturbative method in the relativistic coupled-cluster framework using the Dirac-Coulomb Hamiltonian for calculating the atomic wave functions in the considered F-like ions. We adopted the Fock-space formalism to account for the correlation effects among the occupied electrons by allowing all possible singly and doubly excited configurations in two steps: first considering the correlations between the electrons in a closed-shell configuration, and second constructing the openshell configurations of the first three low-lying states in the considered atomic systems by removing the respective electron from the core orbitals. This procedure enormously simplifies the computational complexity and overcomes the need to select important configuration state functions in determining the atomic state functions in contrast to a truncated configuration interaction method. Moreover, corrections from the frequency-independent Breit interaction and the lowest order quantum electrodynamic effects are incorporated self-consistently. Results. We present the calculated ionization potential energies of the electrons that are detached to form the above considered F-like ions. The correctness of our estimated results are ensured by comparing them with the available experimental values and other calculations. From these calculations, we evaluate the relativistic sensitivity coefficients that we propose here to be used for probing possible temporal variation of the fine structure constant (α e ) through the precise astrophysical observation of the spectral lines of the transitions involving the above low-lying states. The accuracies of these sensitivity coefficients are appraised from the comparison of our calculated energies with the experimental values. We also present the line strengths by calculating the reduced matrix elements of the allowed transitions and of the M1 and E2 forbidden transitions. By combining our calculated line strengths with the observed wavelengths, we determine the oscillator strengths, transition probabilities, and lifetimes of the first two excited states of the above ions and compare them with the other theoretical calculations. The hyperfine splittings of the states are also presented by calculating their magnetic dipole and electric quadrupole hyperfine structure constants.

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Hyperfine structure measurements for lines of astrophysical interest in Mn I

Cited by 32 publications

References 0 publications

Manganese in dwarf spheroidal galaxies

Manganese in dwarf spheroidal galaxies

Stellar Archaeology: A Keck Pilot Program on Extremely Metal-Poor Stars From the Hamburg/ESO Survey. III. The Lead (P[CLC]b[/CLC]) Star HE 0024−2523

Spectral properties of a few F-like ions

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