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Accurate abundance analysis of late-type stars: advances in atomic physics

  • Review Article
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The Astronomy and Astrophysics Review Aims and scope

Abstract

The measurement of stellar properties such as chemical compositions, masses and ages, through stellar spectra, is a fundamental problem in astrophysics. Progress in the understanding, calculation and measurement of atomic properties and processes relevant to the high-accuracy analysis of F-, G-, and K-type stellar spectra is reviewed, with particular emphasis on abundance analysis. This includes fundamental atomic data such as energy levels, wavelengths, and transition probabilities, as well as processes of photoionisation, collisional broadening and inelastic collisions. A recurring theme throughout the review is the interplay between theoretical atomic physics, laboratory measurements, and astrophysical modelling, all of which contribute to our understanding of atoms and atomic processes, as well as to modelling stellar spectra.

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Notes

  1. It is important to note the distinction between accuracy and precision. Accuracy refers to the correctness of a measurement, i.e. how close the measurement is to the true value, while precision refers to the reproducibility of a measurement. Depending on the situation, absolute or relative accuracy may be most important.

  2. Note, errors on the observational side, such as issues in the reduction of echelle spectra, not least continuum placement, may be at least equally important in specific cases (e.g. Caffau et al. 2008).

  3. The webpage http://physics.nist.gov/PhysRefData/ASD/Html/verhist.shtml logs all improvements and updates.

  4. On a historical note, it is worth to comment that charge transfer was first considered in astrophysics by Chamberlain (1956) after Bates (1954) noted the process \({\mathrm {H}} + {\mathrm {O}}^+ \rightleftharpoons {\mathrm {H}}^+ + {\mathrm {O}}\), should, due to the similarity of the ionisation potentials of H and O, have large cross sections at low energies. Chamberlain, and later Field and Steigman (1971), considered this process in the ISM. Later Judge (1986) also considered this process in stellar atmospheres.

  5. Partial processes are those from one channel to a particular final channel, as distinct from total processes from one channel to all possible final channels.

  6. Note there is also a misprint, see Osorio et al. (2015).

  7. We note, however, that calculations usually lack an estimate of their uncertainty. This restricts their viability, because a number without an indication of its uncertainty has no real meaning.

Abbreviations

ABO:

Anstee, Barklem and O’Mara

ASD:

Atomic Spectra Database (at NIST)

ATLAS:

Model stellar atmosphere computer program by Kurucz

AUTOSTRUCTURE:

Atomic structure computer program by Badnell

BSR:

B-Spline R-matrix

CCC:

Convergent close coupling

CCD:

Charge-coupled device

CIV3:

Atomic structure computer program by Hibbert

DESIREE:

Double ElectroStatic Ion Ring ExpEriment

DSB:

Derouich, Sahal-Bréchot and Barklem

ESO:

European Southern Observatory

FARM:

R-matrix computer program for external region problem by Burke and Noble

HBOP:

Hydrogen Bound and bound–free OPacity code

HLINOP:

Hydrogen LINe OPacity computer code by Barklem and Piskunov

HLINPROF:

Hydrogen LINe PROFile computer code by Barklem and Piskunov

IDL:

Interactive Data Language

KAULAKYS:

Computer program for Kaulaky’s free-electron model by Barklem

LFU:

Lindholm–Foley–Unsöld

LTE:

Local thermodynamic equilibrium

MARCS:

Model stellar atmosphere computer program by Gustafsson et al.

MOOG:

Stellar spectrum synthesis computer program by Sneden

MSWAVEF:

Momentum-Space WAVEFunction computer code by Barklem

NIST:

National Institute of Standards and Technology (USA)

RMATRX I:

R-matrix computer program for internal region problem by Berrington et al.

RMPS:

R-matrix with pseudo-states

STARK-B:

Stark broadening database

STGF:

R-matrix computer program for external region problem by Berrington et al.

SUPERSTRUCTURE:

Atomic structure computer program by Eissner et al.

TOPbase:

Opacity Project on-line atomic database

VALD:

Vienna Atomic Line Database

VAMDC:

Virtual Atomic and Molecular Data Centre

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Acknowledgments

This review owes particularly large debts to two great scientists, Jim O’Mara and Andrey Belyaev. I have benefitted immeasurably from having long-term scientific collaborations with them. They have taught me not only physics and astrophysics, but been models of how to do science honestly and ethically. I have learnt from them the value of analytic understanding, often with Jim on the “back-of the-envelope”. They showed me by example how to work carefully on hard problems on long timescales. I am grateful to them both. I thank the many other collaborators who have contributed to work presented here. In particular, I wish to thank Stuart Anstee, Jenny Aspelund-Johansson, Juan Manuel Borrero, Remo Collet, Moncef Derouich, Alan Dickinson, Laine Falklund, Nicole Feautrier, Xavier Gadéa, Marie Guitou, Yeisson Osorio, Sylvie Sahal-Bréchot, and Annie Spielfiedel, for collaboration on various problems in atomic physics over the years. I thank also my many colleagues at Uppsala, past and present, for providing a stimulating and pleasant environment to work in. I thank Igor Bray for clarifications regarding the CCC method. This review and much of the work in it would not have been possible without financial support from the Royal Swedish Academy of Sciences, the Wenner-Gren Foundation, Goran Gustafssons Stiftelse and the Swedish Research Council. For much of this work I was a Royal Swedish Academy of Sciences Research Fellow supported by a grant from the Knut and Alice Wallenberg Foundation. I am presently partially supported by the project grant “The New Milky Way” from the Knut and Alice Wallenberg Foundation.

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  1. Theoretical Astrophysics, Department of Physics and Astronomy, Uppsala University, Box 516, 751 20, Uppsala, Sweden

    Paul S. Barklem

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Barklem, P.S. Accurate abundance analysis of late-type stars: advances in atomic physics. Astron Astrophys Rev 24, 9 (2016). https://doi.org/10.1007/s00159-016-0095-9

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