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LIBRIS Formathandbok  (Information om MARC21)
FältnamnIndikatorerMetadata
00006192naa a2200589 4500
001oai:DiVA.org:mau-41577
003SwePub
008210406s2021 | |||||||||||000 ||eng|
009oai:lup.lub.lu.se:3808dfe5-1a6a-4976-9551-8203e5bf6161
0247 a https://urn.kb.se/resolve?urn=urn:nbn:se:mau:diva-415772 URI
0247 a https://doi.org/10.3847/1538-4357/abd6be2 DOI
0247 a https://lup.lub.lu.se/record/3808dfe5-1a6a-4976-9551-8203e5bf61612 URI
040 a (SwePub)maud (SwePub)lu
041 a engb eng
042 9 SwePub
072 7a ref2 swepub-contenttype
072 7a art2 swepub-publicationtype
1001 a Griffith, Emilyu The Department of Astronomy and Center of Cosmology and AstroParticle Physics, The Ohio State University, Columbus, OH 43210, USA4 aut
2451 0a The Similarity of Abundance Ratio Trends and Nucleosynthetic Patterns in the Milky Way Disk and Bulge
264 c 2021-03-08
264 1b Institute of Physics Publishing (IOPP),c 2021
338 a electronic2 rdacarrier
520 a We compare abundance ratio trends in a sample of similar to 11,000 Milky Way bulge stars (R-GC < 3 kpc) from the Apache Point Observatory Galactic Evolution Experiment (APOGEE) to those of APOGEE stars in the Galactic disk (5 kpc < R-GC < 11 kpc). We divide each sample into low-Ia (high-[Mg/Fe]) and high-Ia (low-[Mg/Fe]) populations, and in each population, we examine the median trends of [X/Mg] versus [Mg/H] for elements X = Fe, O, Na, Al, Si, P, S, K, Ca, V, Cr, Mn, Co, Ni, Cu, and Ce. To remove small systematic trends of APOGEE abundances with stellar log(g), we resample the disk stars to match the log(g) distributions of the bulge data. After doing so, we find nearly identical median trends for low-Ia disk and bulge stars for all elements. High-Ia trends are similar for most elements, with noticeable (0.05-0.1 dex) differences for Mn, Na, and Co. The close agreement of abundance trends (with typical differences less than or similar to 0.03 dex) implies that similar nucleosynthetic processes enriched bulge and disk stars despite the different star formation histories and physical conditions of these regions. For example, we infer that differences in the high-mass slope of the stellar initial mass function between disk and bulge must have been less than or similar to 0.30. This agreement, and the generally small scatter about the median sequences, means that one can predict all of a bulge star's APOGEE abundances with good accuracy knowing only its measured [Mg/Fe] and [Mg/H] and the observed trends of disk stars.
650 7a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng
653 a Nucleosynthesis
653 a Explosive nucleosynthesis
653 a Stellar nucleosynthesis
653 a Chemical abundances
653 a Galactic abundances
653 a Stellar abundances
653 a Galactic bulge
7001 a Weinberg, David H.u The Department of Astronomy and Center of Cosmology and AstroParticle Physics, The Ohio State University, Columbus, OH 43210, USA4 aut
7001 a Johnson, Jennifer A.u The Department of Astronomy and Center of Cosmology and AstroParticle Physics, The Ohio State University, Columbus, OH 43210, USA4 aut0 (Swepub:lu)je1014jo
7001 a Beaton, Rachaelu The Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA4 aut
7001 a Garcia-Hernandez, D. A.u Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, Tenerife, Spain; Universidad de La Laguna (ULL), Departamento de Astrofísica, E-38206 La Laguna, Tenerife, Spain,University of La Laguna (ULL)4 aut
7001 a Hasselquist, Stenu Department of Physics & Astronomy, University of Utah, Salt Lake City, UT 84112, USA4 aut
7001 a Holtzman, Jonu Department of Astronomy, New Mexico State University, Las Cruces, NM 88003, USA4 aut0 (Swepub:lu)jo6205ho
7001 a Johnson, James W.u The Department of Astronomy and Center of Cosmology and AstroParticle Physics, The Ohio State University, Columbus, OH 43210, USA4 aut
7001 a Jönsson, Henriku Malmö University,Lund University,Lunds universitet,Malmö universitet,Institutionen för materialvetenskap och tillämpad matematik (MTM),Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, SE-22100 Lund, Sweden,Astronomi - Genomgår omorganisation,Institutionen för astronomi och teoretisk fysik - Genomgår omorganisation,Naturvetenskapliga fakulteten,Lund Observatory - Undergoing reorganization,Department of Astronomy and Theoretical Physics - Undergoing reorganization,Faculty of Science4 aut0 (Swepub:lu)astr-hkj
7001 a Lane, Richard R.u Instituto de Astronomía y Ciencias Planetarias de Atacama, Universidad de Atacama, Copayapu 485, Copiapó, Chile,University of Atacama4 aut
7001 a Nataf, David M.u Center for Astrophysical Sciences and Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USA4 aut
7001 a Roman-Lopes, Alexandreu Departamento de Astronomía, Universidad de La Serena—Av. Juan Cisternas, 1200 North, La Serena, Chile4 aut
7102 a The Department of Astronomy and Center of Cosmology and AstroParticle Physics, The Ohio State University, Columbus, OH 43210, USAb The Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA4 org
7730 t Astrophysical Journald : Institute of Physics Publishing (IOPP)g 909:1q 909:1x 0004-637Xx 1538-4357
8564 u https://doi.org/10.3847/1538-4357/abd6bey Fulltext
8564 u https://mau.diva-portal.org/smash/get/diva2:1541944/FULLTEXT01.pdfx primaryx Raw objecty fulltext:postprint
8564 u https://iopscience.iop.org/article/10.3847/1538-4357/abd6be/pdf
8564 u http://dx.doi.org/10.3847/1538-4357/abd6bey FULLTEXT
8564 8u https://urn.kb.se/resolve?urn=urn:nbn:se:mau:diva-41577
8564 8u https://doi.org/10.3847/1538-4357/abd6be
8564 8u https://lup.lub.lu.se/record/3808dfe5-1a6a-4976-9551-8203e5bf6161

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