Sökning: onr:"swepub:oai:DiVA.org:su-201329" > The GALAH Survey :
Fältnamn | Indikatorer | Metadata |
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000 | 04256naa a2200685 4500 | |
001 | oai:DiVA.org:su-201329 | |
003 | SwePub | |
008 | 220127s2022 | |||||||||||000 ||eng| | |
024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-2013292 URI |
024 | 7 | a https://doi.org/10.1093/mnras/stab33412 DOI |
040 | a (SwePub)su | |
041 | a engb eng | |
042 | 9 SwePub | |
072 | 7 | a ref2 swepub-contenttype |
072 | 7 | a art2 swepub-publicationtype |
100 | 1 | a Sharma, Sanjib4 aut |
245 | 1 0 | a The GALAH Survey :b dependence of elemental abundances on age and metallicity for stars in the Galactic disc |
264 | c 2021-11-25 | |
264 | 1 | b Oxford University Press (OUP),c 2022 |
338 | a print2 rdacarrier | |
520 | a Using data from the GALAH survey, we explore the dependence of elemental abundances on stellar age and metallicity among Galactic disc stars. We find that the abundance of most elements can be predicted from age and [Fe/H] with an intrinsic scatter of about 0.03 dex. We discuss the possible causes for the existence of the abundance–age–metallicity relations. Using a stochastic chemical enrichment scheme that takes the volume of supernovae remnants into account, we show the intrinsic scatter is expected to be small, about 0.05 dex or even smaller if there is additional mixing in the ISM. Elemental abundances show trends with both age and metallicity and the relationship is well described by a simple model in which the dependence of abundance ([X/Fe]) on age and [Fe/H] are additively separable. Elements can be grouped based on the direction of their abundance gradient in the (age,[Fe/H]) plane and different groups can be roughly associated with three distinct nucleosynthetic production sites, the exploding massive stars, the exploding white dwarfs, and the AGB stars. However, the abundances of some elements, like Co, La, and Li, show large scatter for a given age and metallicity, suggesting processes other than simple Galactic chemical evolution are at play. We also compare the abundance trends of main-sequence turn-off (MSTO) stars against that of giants, whose ages were estimated using asteroseismic information from the K2 mission. For most elements, the trends of MSTO stars are similar to that of giants. The existence of abundance relations implies that we can estimate the age and birth radius of disc stars, which is important for studying the dynamic and chemical evolution of the Galaxy. | |
650 | 7 | a NATURVETENSKAPx Fysik0 (SwePub)1032 hsv//swe |
650 | 7 | a NATURAL SCIENCESx Physical Sciences0 (SwePub)1032 hsv//eng |
653 | a Galaxy: disc | |
653 | a Galaxy: evolution | |
653 | a Galaxy: formation | |
653 | a Galaxy:abundances | |
653 | a Galaxy: kinematics and dynamics | |
700 | 1 | a Hayden, Michael R.4 aut |
700 | 1 | a Bland-Hawthorn, Joss4 aut |
700 | 1 | a Stello, Dennis4 aut |
700 | 1 | a Buder, Sven4 aut |
700 | 1 | a Zinn, Joel C.4 aut |
700 | 1 | a Spina, Lorenzo4 aut |
700 | 1 | a Kallinger, Thomas4 aut |
700 | 1 | a Asplund, Martin4 aut |
700 | 1 | a De Silva, Gayandhi M.4 aut |
700 | 1 | a D'Orazi, Valentina4 aut |
700 | 1 | a Freeman, Ken C.4 aut |
700 | 1 | a Kos, Janez4 aut |
700 | 1 | a Lewis, Geraint F.4 aut |
700 | 1 | a Lin, Jane4 aut |
700 | 1 | a Lind, Karinu Stockholms universitet,Institutionen för astronomi4 aut0 (Swepub:su)kali3212 |
700 | 1 | a Martell, Sarah L.4 aut |
700 | 1 | a Schlesinger, Katharine J.4 aut |
700 | 1 | a Simpson, Jeffrey D.4 aut |
700 | 1 | a Zucker, Daniel B.4 aut |
700 | 1 | a Zwitter, Tomaž4 aut |
700 | 1 | a Chen, Boquan4 aut |
700 | 1 | a Cotar, Klemen4 aut |
700 | 1 | a Kafle, Prajwal R.4 aut |
700 | 1 | a Khanna, Shourya4 aut |
700 | 1 | a Tepper-Garcia, Thor4 aut |
700 | 1 | a Wang, Purmortal4 aut |
700 | 1 | a Wittenmyer, Rob A.4 aut |
710 | 2 | a Stockholms universitetb Institutionen för astronomi4 org |
773 | 0 | t Monthly notices of the Royal Astronomical Societyd : Oxford University Press (OUP)g 510:1, s. 734-752q 510:1<734-752x 0035-8711x 1365-2966 |
856 | 4 | u http://arxiv.org/pdf/2011.13818 |
856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-201329 |
856 | 4 8 | u https://doi.org/10.1093/mnras/stab3341 |
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