Ionization balance of Ti in the photospheres of the Sun and four late-type stars

In this paper we investigate statistical equilibrium of Ti in the atmospheres of late-type stars. The Ti i/Ti ii level populations are computed with available experimental atomic data, except for photoionization and collision-induced transition rates, for which we have to rely on theoretical approxi...

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Published in:	Monthly notices of the Royal Astronomical Society Vol. 413; no. 3; pp. 2184 - 2198
Main Author:	Bergemann, Maria
Format:	Journal Article
Language:	English
Published:	Oxford, UK Blackwell Publishing Ltd 01-05-2011 Wiley-Blackwell Oxford University Press
Subjects:	Astronomy Atmosphere Earth, ocean, space Exact sciences and technology line: formation line: profiles radiative transfer Star & galaxy formation Stars & galaxies stars: abundances Sun Sun: abundances Titanium line: formation Sun: abundances stars: abundances line: profiles radiative transfer Late type stars Line shape Atmosphere model Radiative transfer Chemical evolution Metal-poor stars Galactic evolution Population II Line formation Stellar abundance Thermodynamic non equilibrium Milky Way Sun Statistical equilibrium Meteorites Inelastic collision Photoionization Ionization Metallicity Surface gravity LTE
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Abstract	In this paper we investigate statistical equilibrium of Ti in the atmospheres of late-type stars. The Ti i/Ti ii level populations are computed with available experimental atomic data, except for photoionization and collision-induced transition rates, for which we have to rely on theoretical approximations. For the Sun, the non-local thermodynamic equilibrium (NLTE) line formation with adjusted H i inelastic collision rates and mafags-os model atmosphere solve the long-standing discrepancy between Ti i and Ti ii lines. The NLTE abundances determined from both ionization stages agree within 0.01 dex with each other and with the Ti abundance in C i meteorites. The Ti NLTE model does not perform similarly well for the metal-poor stars, overestimating NLTE effects in the atmospheres of dwarfs, but underestimating overionization for giants. Investigating different sources of errors, we find that only [Ti/Fe] ratios based on Ti ii and Fe ii lines can be safely used in studies of Galactic chemical evolution. To avoid spurious abundance trends with metallicity and dwarf/giant discrepancies, it is strongly recommended to disregard Ti i lines in abundance analyses, as well as in determination of surface gravities.
AbstractList	In this paper we investigate statistical equilibrium of Ti in the atmospheres of late-type stars. The Tii/Tiii level populations are computed with available experimental atomic data, except for photoionization and collision-induced transition rates, for which we have to rely on theoretical approximations. For the Sun, the non-local thermodynamic equilibrium (NLTE) line formation with adjusted Hi inelastic collision rates and mafags-os model atmosphere solve the long-standing discrepancy between Tii and Tiii lines. The NLTE abundances determined from both ionization stages agree within 0.01dex with each other and with the Ti abundance in Ci meteorites. The Ti NLTE model does not perform similarly well for the metal-poor stars, overestimating NLTE effects in the atmospheres of dwarfs, but underestimating overionization for giants. Investigating different sources of errors, we find that only [Ti/Fe] ratios based on Tiii and Feii lines can be safely used in studies of Galactic chemical evolution. To avoid spurious abundance trends with metallicity and dwarf/giant discrepancies, it is strongly recommended to disregard Tii lines in abundance analyses, as well as in determination of surface gravities. [PUBLICATION ABSTRACT] In this paper we investigate statistical equilibrium of Ti in the atmospheres of late-type stars. The Tii/Tiii level populations are computed with available experimental atomic data, except for photoionization and collision-induced transition rates, for which we have to rely on theoretical approximations. For the Sun, the non-local thermodynamic equilibrium (NLTE) line formation with adjusted Hi inelastic collision rates and mafags-os model atmosphere solve the long-standing discrepancy between Tii and Tiii lines. The NLTE abundances determined from both ionization stages agree within 0.01dex with each other and with the Ti abundance in Ci meteorites. The Ti NLTE model does not perform similarly well for the metal-poor stars, overestimating NLTE effects in the atmospheres of dwarfs, but underestimating overionization for giants. Investigating different sources of errors, we find that only [Ti/Fe] ratios based on Tiii and Feii lines can be safely used in studies of Galactic chemical evolution. To avoid spurious abundance trends with metallicity and dwarf/giant discrepancies, it is strongly recommended to disregard Tii lines in abundance analyses, as well as in determination of surface gravities. ABSTRACT In this paper we investigate statistical equilibrium of Ti in the atmospheres of late‐type stars. The Ti i/Ti ii level populations are computed with available experimental atomic data, except for photoionization and collision‐induced transition rates, for which we have to rely on theoretical approximations. For the Sun, the non‐local thermodynamic equilibrium (NLTE) line formation with adjusted H i inelastic collision rates and mafags‐os model atmosphere solve the long‐standing discrepancy between Ti i and Ti ii lines. The NLTE abundances determined from both ionization stages agree within 0.01 dex with each other and with the Ti abundance in C i meteorites. The Ti NLTE model does not perform similarly well for the metal‐poor stars, overestimating NLTE effects in the atmospheres of dwarfs, but underestimating overionization for giants. Investigating different sources of errors, we find that only [Ti/Fe] ratios based on Ti ii and Fe ii lines can be safely used in studies of Galactic chemical evolution. To avoid spurious abundance trends with metallicity and dwarf/giant discrepancies, it is strongly recommended to disregard Ti i lines in abundance analyses, as well as in determination of surface gravities. In this paper we investigate statistical equilibrium of Ti in the atmospheres of late-type stars. The Ti i/Ti ii level populations are computed with available experimental atomic data, except for photoionization and collision-induced transition rates, for which we have to rely on theoretical approximations. For the Sun, the non-local thermodynamic equilibrium (NLTE) line formation with adjusted H i inelastic collision rates and mafags-os model atmosphere solve the long-standing discrepancy between Ti i and Ti ii lines. The NLTE abundances determined from both ionization stages agree within 0.01 dex with each other and with the Ti abundance in C i meteorites. The Ti NLTE model does not perform similarly well for the metal-poor stars, overestimating NLTE effects in the atmospheres of dwarfs, but underestimating overionization for giants. Investigating different sources of errors, we find that only [Ti/Fe] ratios based on Ti ii and Fe ii lines can be safely used in studies of Galactic chemical evolution. To avoid spurious abundance trends with metallicity and dwarf/giant discrepancies, it is strongly recommended to disregard Ti i lines in abundance analyses, as well as in determination of surface gravities.
Author	Bergemann, Maria
Author_xml	– sequence: 1 givenname: Maria surname: Bergemann fullname: Bergemann, Maria email: mbergema@mpa-garching.mpg.de organization: Max-Planck Institute for Astrophysics, Karl-Schwarzschild Str. 1, 85741 Garching, Germany
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Snippet	In this paper we investigate statistical equilibrium of Ti in the atmospheres of late-type stars. The Ti i/Ti ii level populations are computed with available... ABSTRACT In this paper we investigate statistical equilibrium of Ti in the atmospheres of late‐type stars. The Ti i/Ti ii level populations are computed with... In this paper we investigate statistical equilibrium of Ti in the atmospheres of late-type stars. The Tii/Tiii level populations are computed with available...
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SubjectTerms	Astronomy Atmosphere Earth, ocean, space Exact sciences and technology line: formation line: profiles radiative transfer Star & galaxy formation Stars & galaxies stars: abundances Sun Sun: abundances Titanium
Title	Ionization balance of Ti in the photospheres of the Sun and four late-type stars
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