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Baris 1: ~~{{terjemah\|Inggris}}~~ {{Cluster \| name = Messier 34 Baris 67 ⟶ 66: \| bibcode=2006MNRAS.370..954I \|arxiv = astro-ph/0605617 }}</ref> ~~<!--~~ The average proportion of elements with higher atomic numbers than helium is termed the [[metallicity]] by astronomers. This is expressed by the logarithm of the ratio of iron to hydrogen, compared to the same proportion in the Sun. For M34, the metallicity has a value of [Fe/H] = +0.07 ± 0.04. This is equivalent to a 17% higher proportion of iron compared to the Sun. Other elements show a similar abundance, with the exception of nickel which is underabundant.<ref> ~~{{cite journal~~ ~~\| author=Schuler, Simon C. ''et al''~~ ~~\| year=2003~~ ~~\| title=Spectroscopic Abundances of Solar-Type Dwarfs in the Open Cluster M34 (NGC 1039)~~ ~~\| journal=[[Astronomical Journal]]~~ ~~\| volume=125 \| issue=4 \| pages=2085–2097~~ ~~\| doi=10.1086/373927~~ ~~\| bibcode=2003AJ....125.2085S~~ ~~}}</ref>~~ At least 19 members of this cluster are [[white dwarf]]s. These are [[stellar remnant]]s of progenitor stars of up to eight [[solar mass]]es that have evolved through the [[main sequence]] and are no longer engaged in [[thermonuclear fusion]] to generate energy. 17 of the white dwarfs are of spectral type DA or DAZ, while one is a type DB and the last is a type DC.<ref>{{cite journal ~~\| author=Rubin, Kate H. R.; Williams, Kurtis A.; Bolte, M.; Koester, Detlev~~ ~~\| year=2008~~ ~~\| title=The White Dwarf Population in NGC 1039 (M34) and the White Dwarf Initial-Final Mass Relation~~ ~~\| journal=[[Astronomical Journal]]~~ ~~\| volume=135 \| issue=6 \| pages=2163–2176~~ ~~\| doi=10.1088/0004-6256/135/6/2163~~ ~~\| bibcode=2008AJ....135.2163R~~ ~~}}</ref>~~ ~~-->~~ ==Referensi== {{reflist\|2}}

Messier 34: Perbedaan antara revisi