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Chemical Composition of Open Clusters II C H and C Fe in

search for multiple populations in Magellanic Cloud

1 INTRODUCTION.In the last few decades,our understanding of globular clusters (GCs) as simple stellar populations (SSPs) has been overturned by the presence of star-to-star abundance spreads in light elements (e.g.C,N,O,Na) and by the broadening/splitting of features in clusters colourmagnitude diagrams (CMDs).search for multiple populations in Magellanic Cloud 1 INTRODUCTION.In the last few decades,our understanding of globular clusters (GCs) as simple stellar populations (SSPs) has been overturned by the presence of star-to-star abundance spreads in light elements (e.g.C,N,O,Na) and by the broadening/splitting of features in clusters colourmagnitude diagrams (CMDs).chemical composition of ultracompact dwarf galaxies in the Abstract.We present spectroscopic observations of ultracompact dwarf (UCD) galaxies in the Fornax and Virgo clusters made to measure and compare their stellar

chemical composition of ultracompact dwarf galaxies in the

Abstract.We present spectroscopic observations of ultracompact dwarf (UCD) galaxies in the Fornax and Virgo clusters made to measure and compare their stellarchemical composition of ultracompact dwarf galaxies in the Abstract.We present spectroscopic observations of ultracompact dwarf (UCD) galaxies in the Fornax and Virgo clusters made to measure and compare their stellar[2001.03179v1] The Gaia-ESO Survey a new approach to Jan 09,2020 Chemical Composition of Open Clusters II C H and C Fe in#0183;Open clusters (OCs) are recognised as excellent tracers of Galactic thin-disc properties.At variance with intermediate-age and old OCs,for which a significant number of studies is now available,clusters younger than 150 Myr have been mostly overlooked in terms of their chemical composition,with few exceptions.On the other hand,previous investigations seem to indicate an anomalous

[2001.03179v1] The Gaia-ESO Survey a new approach to

Jan 09,2020 Chemical Composition of Open Clusters II C H and C Fe in#0183;Open clusters (OCs) are recognised as excellent tracers of Galactic thin-disc properties.At variance with intermediate-age and old OCs,for which a significant number of studies is now available,clusters younger than 150 Myr have been mostly overlooked in terms of their chemical composition,with few exceptions.On the other hand,previous investigations seem to indicate an anomalous The chemical composition of the stellar cluster Gaia1The chemical composition of Gaia1 does not support an extra-galactic origin for this stellar cluster,that can be considered as a standard Galactic open cluster.Key words.Stars abundances techniques spectroscopic open clusters and associations individual (Gaia1) 1.Introduction Gaia1 is a stellar cluster that has been recently Some results are removed in response to a notice of local law requirement.For more information,please see here.Previous123456NextOCCASO - II.Physical parameters and Fe abundances of red Open clusters have long been used to study the chemodynamical evolution of the Galactic disc.This requires a homogeneously analysed sample covering a wide range of ages and distances.In this paper,we present the Open Clusters Chemical Abundances from Spanish Observatories (OCCASO) second data release.This comprises a sample of high-resolution (R gt; 65 000) and high signal-to-noise

Some results are removed in response to a notice of local law requirement.For more information,please see here.12345NextMetallicities and Stellar Populations

and we define these quantities such that X+Y+Z=1.A different way of measuring a star's chemical composition is by the Iron(Fe)-to-Hydrogen(H) ratio:.for the sun,so that for every Iron atom there are 20,000 Hydrogen atoms.We measure this value for other stars relative to the sun using a quantity called [Fe/HSome results are removed in response to a notice of local law requirement.For more information,please see here.Prussian blue analogue Cu3[Fe(CN)6]2 derived N-doped Cu The fabrication procedure of high content of nitrogen-doped Cu/Fe 3 C clusters ORR electrocatalyst was displayed in Schematic 1.Cu 3 [Fe(CN) 6] 2 can be easily and extensively fabricated by mixing the aqueous solution of Cu(NO 3) 2 3H 2 O and K 3 Fe(CN) 6 under vigorous stirring.Then,the Cu/Fe/N-C catalysts were successfully prepared via pyrolysis of the mixture of Cu 3 [Fe(CN) 6] 2 and

Oxidation Behavior of FeAl,FeSi and FeAlSi Intermetallics

The description of the synergic effect of aluminum and silicon on the oxidation behavior of FeAlSi alloys at 800 Chemical Composition of Open Clusters II C H and C Fe in#176;C in air is presented.The oxidation rate,microstructure,phase,and chemical composition of these ternary alloys are compared with the binary FeAl and FeSi alloys.Oxidation Behavior of FeAl,FeSi and FeAlSi IntermetallicsThe description of the synergic effect of aluminum and silicon on the oxidation behavior of FeAlSi alloys at 800 Chemical Composition of Open Clusters II C H and C Fe in#176;C in air is presented.The oxidation rate,microstructure,phase,and chemical composition of these ternary alloys are compared with the binary FeAl and FeSi alloys.Open clusters as key tracers of Galactic chemical of 6 stars,derived an average [Fe/H] value of 0.61 Chemical Composition of Open Clusters II C H and C Fe in#177;0.14dex.Yong et al.(2005) derived [Fe/H]=0.45 and 0.53 for two stars near the RGB tip observed at high resolution.Cr 261 This is one of the oldest open clusters in the Galaxy,with an age in the range 610 Gyr (but the upper value is

Open Star Clusters - SEDS Messier Database

Aug 27,2007 Chemical Composition of Open Clusters II C H and C Fe in#0183;Also,as all the stars in a cluster formed from the same diffuse nebula,they are all of similar initial chemical composition.Open clusters are of great interest for astrophysicists because of these properties the stars in a cluster are all at about theOCCASO - II.Physical parameters and Fe abundances of red Open clusters have long been used to study the chemodynamical evolution of the Galactic disc.This requires a homogeneously analysed sample covering a wide range of ages and distances.In this paper,we present the Open Clusters Chemical Abundances from Spanish Observatories (OCCASO) second data release.This comprises a sample of high-resolution (R gt; 65 000) and high signal-to-noise News from the Galactic suburbia the chemicalCa II triplet,suggesting an intrinsic star-to-star scatter in its Fe or Ca content.From our analysis,we assess that all the investigated stars share the same [Fe/H],[Ca/Fe] and [Ti/Fe] abundance ratios,while a large spread in Mg and K abundances is detected.The distribution of

Nano-sized Superlattice Clusters Created by Oxygen

Jul 02,2015 Chemical Composition of Open Clusters II C H and C Fe in#0183;In the present work,we report the discovery of a new,oxygen-enriched,nano-sized superlattice (NSS) clusters (25 nm) in ball-milled Fe and FeMetallicity in Open Clusters Request PDFA study of chemical composition for 23 A-type stars in four nearby open clusters (Pleiades,Coma,Hyades and Praesepe) has derived detailed abundances for Mg,Ca,Sc,Cr,Fe,and Ni from high Metallicities and Stellar Populationsand we define these quantities such that X+Y+Z=1.A different way of measuring a star's chemical composition is by the Iron(Fe)-to-Hydrogen(H) ratio:.for the sun,so that for every Iron atom there are 20,000 Hydrogen atoms.We measure this value for other stars relative to the sun using a quantity called [Fe/H

Metal substitution reaction in the cluster [(H)2Fe3(3

Apr 01,1996 Chemical Composition of Open Clusters II C H and C Fe in#0183;The cluster [(H) 2 Fe 3 ( 3 Se)(CO) 9] has been found to react with [CPW(CO) 3] 2 [Cp = ( 5 C 5 H 5)] when refluxed in m-xylene.Two major products of this reaction have been isolated,one of which is the heteronuclear cluster [(H)Fe 2 W( 3 Se)(CO) 8 Cp].Its structure has been determined by X-ray analysis.Magnetic properties of iron clusters in Sc75Fe25 nanoglass Jan 15,2020 Chemical Composition of Open Clusters II C H and C Fe in#0183;The virtual STEM-HAADF images displayed in Fig.1(a) and (b) show the nanoscale morphology of the nanoglass and the corresponding metallic glass ribbon.Their contrast is sensitive to sample mass (i.e.density Chemical Composition of Open Clusters II C H and C Fe in#215; thickness) with the bright contrast indicating an Fe-rich cluster.Fig.1(c) and (d) are STEM-EELS elemental maps of the nanoglass sample and the metallic glass ribbon sampleEarly corrosion behaviour of irradiated FeCrAl alloy in a Sep 01,2020 Chemical Composition of Open Clusters II C H and C Fe in#0183;In order to investigate the early corrosion behaviour of irradiated nuclear-grade FeCrAl alloys in the normal-service PWRs,an FeCrAl alloy was irradiated by 400-keV Fe + with different ion fluences at 400 Chemical Composition of Open Clusters II C H and C Fe in#176;C,and then was corroded in a simulated PWR environment at 340 Chemical Composition of Open Clusters II C H and C Fe in#176;C and 15.16 MPa.The microstructure,chemical composition,and corrosion

DFT Studies of Pt/Au Bimetallic Clusters and Their

Density functional theory (DFT) calculations were performed to study Pt/Au clusters of different size,structure,and composition as well as their interactions with a CO molecule.Among the Pt/Au isomers studied here,the planar structure is the most stable structure in many Pt compositions,although three-dimensional structures become more stable with increasing Pt composition.Cited by 55Publish Year 1990Author Eileen D.Friel,Ann Merchant BoesgaardChemical Composition of Open Clusters.III.Iron and Mar 01,1992 Chemical Composition of Open Clusters II C H and C Fe in#0183;Iron and carbon abundances are determined for F dwarfs in several open clusters and the field in order to investigate the homogeneity of chemical mixing in the Galactic disk.Abundances are based on measurements of eight Fe I lines and six high-excitation C I lines in the spectral region 7065-7155 A analyzed with model atmospheres.Cluster mean values of Fe/H and C/H show cluster-to-cluster Cited by 143Publish Year 1992Author Eileen D.Friel,Ann M.BoesgaardOxygen in the Blanco 1 open cluster Request PDFChemical composition of open clusters.I - Fe/H from high-resolution spectroscopy.II - C/H and C/Fe in F dwarfs from high-resolution spectroscopy the same pattern as the Fe/H cluster

Chemical composition of giant stars in the open cluster

The mean metallicity of this cluster,as determined from nine denite member stars,is very close to solar [Fe/H] = 0:02 0:01.Abundances of carbon,nitrogen,and sodium exhibit alterations caused by extra-mixing the mean 12 C= 13 C ratio is lowered to 19Chemical composition of giant stars in the open clusterThe mean metallicity of this cluster,as determined from nine denite member stars,is very close to solar [Fe/H] = 0:02 0:01.Abundances of carbon,nitrogen,and sodium exhibit alterations caused by extra-mixing the mean 12 C= 13 C ratio is lowered to 19Chemical composition of giant stars in the open cluster IC Aims The main aim of this study is a comprehensive chemical analysis of red giant stars in the open cluster IC 4756,including determinations of 12C/13C and C/N abundance ratios,and comparisons

Chemical composition of A and F dwarfs members of

metallicity of Chemical Composition of Open Clusters II C H and C Fe inlt;[Fe/H] Chemical Composition of Open Clusters II C H and C Fe ingt;=+0.140.05 dex.Abundances derived from calibration of Geneva photometry by Grenon (2000) ( Chemical Composition of Open Clusters II C H and C Fe inlt;[Fe/H] Chemical Composition of Open Clusters II C H and C Fe ingt;=+0.140.01) also yield a slightly enhanced metal-licity.Several papers have addressed the chemical composi-tion of A and F dwarfs in the Hyades open cluster.Carbon and iron abundances have been derived for 14 F stars byChemical composition of A and F dwarfs members of the metallicity of Chemical Composition of Open Clusters II C H and C Fe inlt;[Fe/H] Chemical Composition of Open Clusters II C H and C Fe ingt;=+0.140.05 dex.Abundances derived from calibration of Geneva photometry by Grenon (2000) ( Chemical Composition of Open Clusters II C H and C Fe inlt;[Fe/H] Chemical Composition of Open Clusters II C H and C Fe ingt;=+0.140.01) also yield a slightly enhanced metal-licity.Several papers have addressed the chemical composi-tion of A and F dwarfs in the Hyades open cluster.Carbon and iron abundances have been derived for 14 F stars byChemical Composition of Open Clusters.II.C/H and C/Fe in Mar 01,1990 Chemical Composition of Open Clusters II C H and C Fe in#0183;We have determined carbon abundances for F dwarfs in open clusters and moving groups of a variety of ages and [Fe/H] abundances to investigate the homogeneity of chemical mixing within the Galactic disk.The stars studied range in age from 5 Chemical Composition of Open Clusters II C H and C Fe in#215; 10 7 to 2 Chemical Composition of Open Clusters II C H and C Fe in#215; 10 9 years,and in metallicity from [Fe/H] = -0.2 to +0.15; our sample of F dwarfs comes from the Per,Pleiades,and Hyades clusters

CHEMICAL COMPOSITION OF INTERMEDIATE-MASS

mean cluster metallicity of [Fe/H] = 0.07 Chemical Composition of Open Clusters II C H and C Fe in#177; 0.03 dex from the iron abundances of the F-type stars.We nd that for most chemical elements,the normal late B- and A-type stars exhibit larger star-to-star abundance variations than the F-type stars probably because of the faster rotation of the B and A stars.The abundances of C,O,Mg,Si,CHEMICAL COMPOSITION OF INTERMEDIATE-MASSmean cluster metallicity of [Fe/H] = 0.07 Chemical Composition of Open Clusters II C H and C Fe in#177; 0.03 dex from the iron abundances of the F-type stars.We nd that for most chemical elements,the normal late B- and A-type stars exhibit larger star-to-star abundance variations than the F-type stars probably because of the faster rotation of the B and A stars.The abundances of C,O,Mg,Si,CHEMICAL ABUNDANCES OF MEMBER STARS IN THE OPEN CLUSTER We have taken high signal-to-noise (S/N),high-resolution spectra of 11 solar-type stars in the Praesepe open cluster to determine the chemical abundances of 16 elements Li,C,O,Na,Mg,Al,Si,Ca,Sc,Ti,V,Cr,Fe,Ni,Y,and Ba.We have determined Fe from Fe I and Fe II lines and find [Fe/H] = +0.12 Chemical Composition of Open Clusters II C H and C Fe in#177;0.04.

Astrochemistry of transition metals? The selected cases of

By considering the simplest organic substrate CH 4,the parental reaction schemes (gas phase,T = 30 K) (I) [FeN] + + CH 4 + H [Fe] + + H 3 CNH 2; (II) [FeNH] + + CH 4 [Fe] + + H 3 CNH 2 and (III) [(CO) 2 FeN] + + H [FeCO] + + HNCO are analyzed by theoretical methods (B2PLYP double hybrid functional/TZVPPP basis set).All Astrochemistry of transition metals? The selected cases of By considering the simplest organic substrate CH 4,the parental reaction schemes (gas phase,T = 30 K) (I) [FeN] + + CH 4 + H [Fe] + + H 3 CNH 2; (II) [FeNH] + + CH 4 [Fe] + + H 3 CNH 2 and (III) [(CO) 2 FeN] + + H [FeCO] + + HNCO are analyzed by theoretical methods (B2PLYP double hybrid functional/TZVPPP basis set).All (PDF) The Galactic system of old open clusters age Chemical Composition of Open Clusters.II.C/H and C/Fe in F Dwarfs from High-Resolution Spectroscopy. Cluster mean values of Fe/H and C/H show cluster-to-cluster variations well in

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