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Line formation in solar granulation III. The photospheric Si and meteoritic Fe abundances
Uppsala University, Teknisk-naturvetenskapliga vetenskapsområdet, Physics, Department of Astronomy and Space Physics.
2000 (English)In: ASTRONOMY AND ASTROPHYSICS, ISSN 0004-6361, Vol. 359, no 2, 755-758 p.Article in journal (Refereed) Published
Abstract [en]

Using realistic hydrodynamical simulations of the solar surface convection as 3D, time-dependent, inhomogeneous model atmospheres, the solar photospheric Si abundance has been determined to be log epsilon(Si) = 7.51 +/- 0.04. This constitutes a difference

Place, publisher, year, edition, pages
SPRINGER-VERLAG , 2000. Vol. 359, no 2, 755-758 p.
Keyword [en]
convection; hydrodynamics; line : formation; Sun : abundances; Sun : granulation; Sun : photosphere; ABSOLUTE OSCILLATOR-STRENGTHS; NEUTRAL HYDROGEN-ATOMS; TRANSITIONS; COLLISIONS; ELEMENTS; SILICON
URN: urn:nbn:se:uu:diva-36615OAI: oai:DiVA.org:uu-36615DiVA: diva2:64514
Addresses: Asplund M, Astron Observ, Box 515, S-75120 Uppsala, Sweden. NORDITA, DK-2100 Copenhagen O, Denmark.Available from: 2008-10-17 Created: 2008-10-17 Last updated: 2011-01-14

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