Advanced

Chemical Abundances of Main-sequence, Turnoff, Subgiant, and Red Giant Stars from APOGEE Spectra. II. Atomic Diffusion in M67 Stars

Souto, Diogo; Prieto, C. Allende; Cunha, Katia; Pinsonneault, Marc; Smith, Verne V.; Garcia-Dias, R.; Bovy, Jo; Garcia-Hernández, D. A.; Holtzman, Jon LU and Johnson, J. A., et al. (2019) In Astrophysical Journal 874(1).
Abstract


Chemical abundances for 15 elements (C, N, O, Na, Mg, Al, Si, K, Ca, Ti, V, Cr, Mn, Fe, and Ni) are presented for 83 stellar members of the 4 Gyr old solar-metallicity open cluster M67. The sample contains stars spanning a wide range of evolutionary phases, from G dwarfs to red clump stars. The abundances were derived from near-IR (λ1.5-1.7 μm) high-resolution spectra (R ,F= ,F22,500) from the SDSS-IV/Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey. A 1D local thermodynamic equilibrium abundance analysis was carried out using the APOGEE synthetic spectral libraries, via χ
2
... (More)


Chemical abundances for 15 elements (C, N, O, Na, Mg, Al, Si, K, Ca, Ti, V, Cr, Mn, Fe, and Ni) are presented for 83 stellar members of the 4 Gyr old solar-metallicity open cluster M67. The sample contains stars spanning a wide range of evolutionary phases, from G dwarfs to red clump stars. The abundances were derived from near-IR (λ1.5-1.7 μm) high-resolution spectra (R ,F= ,F22,500) from the SDSS-IV/Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey. A 1D local thermodynamic equilibrium abundance analysis was carried out using the APOGEE synthetic spectral libraries, via χ
2
minimization of the synthetic and observed spectra with the qASPCAP code. We found significant abundance differences (∼0.05-0.30 dex) between the M67 member stars as a function of the stellar mass (or position on the Hertzsprung-Russell diagram), where the abundance patterns exhibit a general depletion (in [X/H]) in stars at the main-sequence turnoff. The amount of the depletion is different for different elements. We find that atomic diffusion models provide, in general, good agreement with the abundance trends for most chemical species, supporting recent studies indicating that measurable atomic diffusion operates in M67 stars.

(Less)
Please use this url to cite or link to this publication:
author
, et al. (More)
(Less)
organization
publishing date
type
Contribution to journal
publication status
published
subject
keywords
diffusion, infrared: stars, open clusters and associations: general, stars: abundances
in
Astrophysical Journal
volume
874
issue
1
publisher
American Astronomical Society
external identifiers
  • scopus:85064427709
ISSN
0004-637X
DOI
10.3847/1538-4357/ab0b43
language
English
LU publication?
yes
id
94c0c770-b2db-4823-994a-ef461c67c30b
date added to LUP
2019-05-06 09:53:47
date last changed
2019-05-21 04:22:23
@article{94c0c770-b2db-4823-994a-ef461c67c30b,
  abstract     = {<p><br>
                                                         Chemical abundances for 15 elements (C, N, O, Na, Mg, Al, Si, K, Ca, Ti, V, Cr, Mn, Fe, and Ni) are presented for 83 stellar members of the 4 Gyr old solar-metallicity open cluster M67. The sample contains stars spanning a wide range of evolutionary phases, from G dwarfs to red clump stars. The abundances were derived from near-IR (λ1.5-1.7 μm) high-resolution spectra (R ,F= ,F22,500) from the SDSS-IV/Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey. A 1D local thermodynamic equilibrium abundance analysis was carried out using the APOGEE synthetic spectral libraries, via χ                             <br>
                            <sup>2</sup><br>
                                                          minimization of the synthetic and observed spectra with the qASPCAP code. We found significant abundance differences (∼0.05-0.30 dex) between the M67 member stars as a function of the stellar mass (or position on the Hertzsprung-Russell diagram), where the abundance patterns exhibit a general depletion (in [X/H]) in stars at the main-sequence turnoff. The amount of the depletion is different for different elements. We find that atomic diffusion models provide, in general, good agreement with the abundance trends for most chemical species, supporting recent studies indicating that measurable atomic diffusion operates in M67 stars.                         <br>
                        </p>},
  articleno    = {97},
  author       = {Souto, Diogo and Prieto, C. Allende and Cunha, Katia and Pinsonneault, Marc and Smith, Verne V. and Garcia-Dias, R. and Bovy, Jo and Garcia-Hernández, D. A. and Holtzman, Jon and Johnson, J. A. and Jönsson, Henrik and Majewski, Steve R. and Shetrone, Matthew and Sobeck, Jennifer and Zamora, Olga and Pan, Kaike and Nitschelm, Christian},
  issn         = {0004-637X},
  keyword      = {diffusion,infrared: stars,open clusters and associations: general,stars: abundances},
  language     = {eng},
  month        = {03},
  number       = {1},
  publisher    = {American Astronomical Society},
  series       = {Astrophysical Journal},
  title        = {Chemical Abundances of Main-sequence, Turnoff, Subgiant, and Red Giant Stars from APOGEE Spectra. II. Atomic Diffusion in M67 Stars},
  url          = {http://dx.doi.org/10.3847/1538-4357/ab0b43},
  volume       = {874},
  year         = {2019},
}