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Line formation in solar granulation - I. Fe line shapes, shifts and asymmetries
Uppsala University, Teknisk-naturvetenskapliga vetenskapsområdet, Physics, Department of Astronomy and Space Physics.
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2000 (English)In: ASTRONOMY AND ASTROPHYSICS, ISSN 0004-6361, Vol. 359, no 2, 729-742 p.Article in journal (Refereed) Published
Abstract [en]

Realistic ab-initio 3D, radiative-hydrodynamical convection simulations of the solar granulation have been applied to Fe I and Fe II line formation. In contrast to classical analyses based on hydrostatic ID model atmospheres the procedure contains no adju

Place, publisher, year, edition, pages
SPRINGER-VERLAG , 2000. Vol. 359, no 2, 729-742 p.
Keyword [en]
convection; hydrodynamics; line : formation; radiative transfer; Sun : granulation; Sun : photosphere; METAL-POOR STARS; STELLAR GRANULATION; MODEL ATMOSPHERES; IRON ABUNDANCE; WAVELENGTH SHIFTS; OPTICAL-SPECTRUM; CONVECTION; SIMULATIONS; SUN
URN: urn:nbn:se:uu:diva-36618OAI: oai:DiVA.org:uu-36618DiVA: diva2:64517
Addresses: Asplund M, Univ Uppsala, Astron Observ, Box 515, S-75120 Uppsala, Sweden. NORDITA, DK-2100 Copenhagen O, Denmark. NBIFAFG, Astron Observ, DK-2100 Copenhagen, Denmark. Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48823 USA. Univ Texas,Available from: 2008-10-17 Created: 2008-10-17 Last updated: 2011-01-14

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