Anna Frebel - The iron-deficient star HE 1327 −2326 Conclusions • Metal-poor stars provide important constraints on e.g. the properties of the first generation of stars and SNe, nucleosynthesis processes, stellar evolution at low [Fe/H] • HE1327 −2326 and HE 01017-5240 have by far the lowest iron abundances known, and is possibly are members of a new population of the most extreme. We present a new abundance analysis of HE 1327-2326, which is currently the most iron-poor star, based on observational data obtained with the VLT Ultraviolet and Visual Echelle Spectrograph (UVES). We correct the one-dimensional (1D) LTE abundances for three-dimensional (3D) effects to provide an abundance pattern that supersedes previous works and should be used to observationally test current models of the chemical yields of the first-generation supernovae (SNe). Apart from confirming the. So ist der Eisenanteil von HE 1327-2326 beispielsweise rund 400.0000 Mal geringer als bei der Sonne. Das spricht dafür, dass auch seine Sternenwiege ähnlich metallarm war. Deshalb wissen wir. Look at other dictionaries: HE1327-2326 — HE 1327 2326 HE 1327 2326 est une étoile de magnitude 13,5 située dans la constellation de l Hydre Femelle. Découverte en 2005, elle présente la plus faible métallicité connue, [Fe/H] = 5,6, soit plus de 200 000 fois moins que le Soleil
HE 1327-2326 und Anna Frebel · Mehr sehen » Durchmusterung. Lage der von der Bonner Durchmusterung (oben) und der Córdoba-Durchmusterung (unten) beschriebenen Objekte im Vergleich zum gesamten Firmament. Farblegende siehe Beschreibungsseite. Bei dieser äquatorialen Projektion ist der von beiden Beobachtungsorten (Bonn und Córdoba. HE 1327-2326, An Unevolved Star with [Fe/H] < -5.0. III. Does its Atmosphere Reflect its Natal Composition? By A J Korn, O. Richard, L Mashonkina, Michael Bessell, Anna Frebel and Wako Aoki. Cite . BibTex; Full citation Abstract. Based on spectroscopic constraints derived from nonlocal thermodynamic equilibrium line formation, we explore the likely range of stellar parameters (Teff and log g.
HE 1327-2326 is either in its main-sequence or subgiant phase of evolution. Its non-LTE-corrected iron abundance is [Fe/H] = -5.45, 0.2 dex lower than that of HE 0107-5240, the previously most iron-poor object known, and more than 1 dex lower than those of all other metal-poor stars. Both HE 1327-2326 and HE 0107-5240 exhibit extremely large overabundances of carbon ([C/Fe] ~ +4). The. Autor: Frebel, Anna et al.; Genre: Zeitschriftenartikel; Im Druck veröffentlicht: 2008-09-01; Titel: HE 1327−2326, an unevolved star with [Fe/H]<−5.0. - II. New 3D−1D corrected abundances from a Very Large Telescope UVES spectru So ist der Eisenanteil von HE 1327-2326 beispielsweise rund 400.0000 Mal geringer als bei der Sonne. Das spricht dafür, dass auch seine Sternenwiege ähnlich metallarm war. Deshalb wissen wir. HE 1327 - 2326. Animiere den Titel (Der Urknall) mit einem beliebigen Effekt! Schreib als Untertitel deinen Namen! Quellen. Wikipedia. Spektrum der Wissenschaft. Der Stoff aus dem der Kosmos ist - Brian Greene. Verschiebe diese Folie hinter die letzte Folie! Woher kommt die Idee des Urknalls? Alle Galaxien bewegen sich von uns weg . Je weiter sie weg sind, desto schneller. Kosmische. Archivierte Blogs. 3vor10 Alles was fliegt Amerikanische Begegnungen Andererseits Arte-Fakten Beauty full Science Chemisch gesehen Columbus Gastblog Darwinjahr Das Labortagebuch Deutsches Museum Diax's Rake Die andere Bildung Durchschaut E-Mobility Echolot Ein bisschen dunkel Epi goes Gender Flug und Zeit For Women in Science Geo? Logisch! Heureka Hinterm Mond gleich links Historikertag Iconic.
of HE 1327 2326 appeared to be similar to that of CS 22876 032, which was the most metal-poor dwarf known at that time (½Fe/H¼ 3:71;: Norris et al. 2000). This suggested that the effective temperatures of the two stars were very similar; further comparison indicated that the metallicity of HE 1327 2326 might indeed be lower than that of CS 22876 032. We have been conducting an observing. HE 1327-2326 is either in its main-sequence or subgiant phase of evolution. Its non-LTE-corrected iron abundance is [Fe/H]=-5.45, 0.2 dex lower than that of HE 0107-5240, the previously most iron-poor object known, and more than 1 dex lower than those of all other metal-poor stars. Both HE 1327-2326 and HE 0107-5240 exhibit extremely large overabundances of carbon ([C/Fe]~+4). The combination. We present a new abundance analysis of HE 1327-2326, which is currently the most iron-poor star, based on observational data obtained with the VLT Ultraviolet and Visual Echelle Spectrograph (UVES). We correct the one-dimensional (1D) LTE abundances for three-dimensional (3D) effects to provide an abundance pattern that supersedes previous works and should be used to observationally test. We present a new abundance analysis of HE 1327-2326, the currently most iron-poor star, based on observational data obtained with VLT/UVES. We correct the 1D LTE abundances for 3D effects to provide an abundance pattern that supersedes previous works, and should be used to observationally test current models of the chemical yields of the first-generation SNe. Apart from confirming the 1D LTE.
