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  • Lind, KarinUppsala universitet,Observationell astrofysik,Max Planck Inst Astron, Germany. (author)

Non-LTE line formation of Fe in late-type stars - IV. Modelling of the solar centre-to-limb variation in 3D

  • Article/chapterEnglish2017

Publisher, publication year, extent ...

  • 2017-03-25
  • OXFORD UNIV PRESS,2017
  • electronicrdacarrier

Numbers

  • LIBRIS-ID:oai:DiVA.org:uu-327363
  • https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-327363URI
  • https://doi.org/10.1093/mnras/stx673DOI
  • https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-144759URI

Supplementary language notes

  • Language:English
  • Summary in:English

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  • Subject category:ref swepub-contenttype
  • Subject category:art swepub-publicationtype

Notes

  • Our ability to model the shapes and strengths of iron lines in the solar spectrum is a critical test of the accuracy of the solar iron abundance, which sets the absolute zero-point of all stellar metallicities. We use an extensive 463-level Fe atom with new photoionization cross-sections for Fe I and quantum mechanical calculations of collisional excitation and charge transfer with neutral hydrogen; the latter effectively remove a free parameter that has hampered all previous line formation studies of Fe in non-local thermodynamic equilibrium (NLTE). For the first time, we use realistic 3D NLTE calculations of Fe for a quantitative comparison to solar observations. We confront our theoretical line profiles with observations taken at different viewing angles across the solar disc with the Swedish 1-m Solar Telescope. We find that 3D modelling well reproduces the observed centre-to-limb behaviour of spectral lines overall, but highlight aspects that may require further work, especially cross-sections for inelastic collisions with electrons. Our inferred solar iron abundance is log(epsilon(Fe)) = 7.48 +/- 0.04 dex.

Subject headings and genre

Added entries (persons, corporate bodies, meetings, titles ...)

  • Amarsi, A. M.Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.;Australian Natl Univ, Res Sch Astron & Astrophys, Cotter Rd, Canberra, ACT 2611, Australia. (author)
  • Asplund, M.Australian Natl Univ, Res Sch Astron & Astrophys, Cotter Rd, Canberra, ACT 2611, Australia. (author)
  • Barklem, Paul S.Uppsala universitet,Observationell astrofysik(Swepub:uu)pba11670 (author)
  • Bautista, M.Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. (author)
  • Bergemann, M.Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. (author)
  • Collet, R.Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. (author)
  • Kiselman, DanStockholms universitet,Institutionen för astronomi(Swepub:su)dan (author)
  • Leenaarts, JorritStockholms universitet,Institutionen för astronomi(Swepub:su)jleen (author)
  • Pereira, T. M. D.Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway. (author)
  • Uppsala universitetObservationell astrofysik (creator_code:org_t)

Related titles

  • In:Monthly notices of the Royal Astronomical Society: OXFORD UNIV PRESS468:4, s. 4311-43220035-87111365-2966

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