Probing the strength of radial migration via churning by using metal-rich red giant stars from APOGEE
(2024) In Monthly Notices of the Royal Astronomical Society 533(1). p.538-550- Abstract
Making use of the APOGEE DR17 catalogue with high quality data for 143 509 red giant branch stars we explore the strength of different mechanisms that causes a star to radially migrate in the Milky Way stellar disc. At any position in the disc we find stars that are more metal-rich than the local interstellar medium. This is surprising and normally attributed to the migration of these stars after their formation inside their current Galactocentric radius. Such stars are prime candidates for studying the strength of different migratory processes. We specifically select two types of metal-rich stars: (i) super metal-rich stars ([Fe/H] > 0.2) and (ii) stars that are more metal-rich than their local environment. For both, we explore the... (More)
Making use of the APOGEE DR17 catalogue with high quality data for 143 509 red giant branch stars we explore the strength of different mechanisms that causes a star to radially migrate in the Milky Way stellar disc. At any position in the disc we find stars that are more metal-rich than the local interstellar medium. This is surprising and normally attributed to the migration of these stars after their formation inside their current Galactocentric radius. Such stars are prime candidates for studying the strength of different migratory processes. We specifically select two types of metal-rich stars: (i) super metal-rich stars ([Fe/H] > 0.2) and (ii) stars that are more metal-rich than their local environment. For both, we explore the distribution of orbital parameters and ages as evidence of their migration history. We find that most super metal-rich stars have experienced some amount of churning as they have orbits with Rg ≥ 5 kpc. Furthermore, about half of the super metal-rich stars are on non-circular orbits (ecc > 0.15) and therefore also have experienced blurring. The metallicity of young stars in our sample is generally the same as the metallicity of the interstellar medium, suggesting they have not radially migrated yet. Stars with lower metallicity than the local environment have intermediate to old ages. We further find that super metal-rich stars have approximately the same age distribution at all Galactocentric radii, which suggests that radial migration is a key mechanism responsible for the chemical compositions of stellar populations in the Milky Way.
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- author
- Lehmann, Christian LU ; Feltzing, Sofia LU ; Feuillet, Diane LU and Kordopatis, Georges LU
- organization
- publishing date
- 2024-09
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- Galaxy: disc, Galaxy: evolution, Galaxy: kinematics and dynamics, Galaxy: stellar content, stars: kinematics and dynamics
- in
- Monthly Notices of the Royal Astronomical Society
- volume
- 533
- issue
- 1
- pages
- 13 pages
- publisher
- Oxford University Press
- external identifiers
-
- scopus:85201062009
- ISSN
- 0035-8711
- DOI
- 10.1093/mnras/stae1736
- language
- English
- LU publication?
- yes
- id
- 3db14279-c8db-4575-9c69-6ab02a8a0bf0
- date added to LUP
- 2024-09-02 15:53:41
- date last changed
- 2024-09-02 15:55:01
@article{3db14279-c8db-4575-9c69-6ab02a8a0bf0, abstract = {{<p>Making use of the APOGEE DR17 catalogue with high quality data for 143 509 red giant branch stars we explore the strength of different mechanisms that causes a star to radially migrate in the Milky Way stellar disc. At any position in the disc we find stars that are more metal-rich than the local interstellar medium. This is surprising and normally attributed to the migration of these stars after their formation inside their current Galactocentric radius. Such stars are prime candidates for studying the strength of different migratory processes. We specifically select two types of metal-rich stars: (i) super metal-rich stars ([Fe/H] > 0.2) and (ii) stars that are more metal-rich than their local environment. For both, we explore the distribution of orbital parameters and ages as evidence of their migration history. We find that most super metal-rich stars have experienced some amount of churning as they have orbits with R<sub>g</sub> ≥ 5 kpc. Furthermore, about half of the super metal-rich stars are on non-circular orbits (ecc > 0.15) and therefore also have experienced blurring. The metallicity of young stars in our sample is generally the same as the metallicity of the interstellar medium, suggesting they have not radially migrated yet. Stars with lower metallicity than the local environment have intermediate to old ages. We further find that super metal-rich stars have approximately the same age distribution at all Galactocentric radii, which suggests that radial migration is a key mechanism responsible for the chemical compositions of stellar populations in the Milky Way.</p>}}, author = {{Lehmann, Christian and Feltzing, Sofia and Feuillet, Diane and Kordopatis, Georges}}, issn = {{0035-8711}}, keywords = {{Galaxy: disc; Galaxy: evolution; Galaxy: kinematics and dynamics; Galaxy: stellar content; stars: kinematics and dynamics}}, language = {{eng}}, number = {{1}}, pages = {{538--550}}, publisher = {{Oxford University Press}}, series = {{Monthly Notices of the Royal Astronomical Society}}, title = {{Probing the strength of radial migration via churning by using metal-rich red giant stars from APOGEE}}, url = {{http://dx.doi.org/10.1093/mnras/stae1736}}, doi = {{10.1093/mnras/stae1736}}, volume = {{533}}, year = {{2024}}, }