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An investigation of non-canonical mixing in red giant stars using APOGEE 12C/13C ratios observed in open cluster stars

Journal Article · · Monthly Notices of the Royal Astronomical Society
 [1];  [1];  [2];  [3];  [4];  [5];  [6];  [7];  [1];  [8];  [9];  [10]
  1. University of Virginia, Charlottesville, VA (United States)
  2. NSF’s National Optical-Infrared Astronomy Research Laboratory, Tucson, AZ (United States); Sorbonne Université, Paris (France)
  3. Herzberg Astronomy and Astrophysics Research Centre, Victoria, BC (Canada)
  4. Sorbonne Université, Paris (France); Observatório Nacional, Rio de Janeiro (Brazil); University of Arizona, Tucson, AZ (United States)
  5. Instituto de Astrofísica de Canarias, Tenerife (Spain); Universidad de La Laguna, Tenerife (Spain)
  6. Max-Planck-Institut für Astrophysik, Garching (Germany)
  7. University of California, Santa Cruz, CA (United States)
  8. Texas Christian University, Fort Worth, TX (United States)
  9. Instituto de Astrofísica de Canarias, Tenerife (Spain)
  10. Universidad de Antofagasta (Chile)

Standard stellar evolution theory poorly predicts the surface abundances of chemical species in low-mass, red giant branch (RGB) stars. Observations show an enhancement of p–p chain and CNO cycle products in red giant envelopes, which suggests the existence of non-canonical mixing that brings interior burning products to the surface of these stars. The 12C/13C ratio is a highly sensitive abundance metric used to probe this mixing. We investigate extra RGB mixing by examining: (1) how 12C/13C is altered along the RGB, and (2) how 12C/13C changes for stars of varying age and mass. Our sample consists of 43 red giants, spread over 15 open clusters from the Sloan Digital Sky Survey’s APOGEE DR17, that have reliable 12C/13C ratios derived from their APOGEE spectra. We vetted these 12C/13C ratios and compared them as a function of evolution and age/mass to the standard mixing model of stellar evolution, and to a model that includes prescriptions for RGB thermohaline mixing and stellar rotation. We find that the observations deviate from standard mixing models, implying the need for extra mixing. Additionally, some of the abundance patterns depart from the thermohaline model, and it is unclear whether these differences are due to incomplete observations, issues inherent to the model, our assumption of the cause of extra mixing, or any combination of these factors. Nevertheless, the surface abundances across our age/mass range clearly deviate from the standard model, agreeing with the notion of a universal mechanism for RGB extra mixing in low-mass stars.

Research Organization:
US Department of Energy (USDOE), Washington, DC (United States). Office of Science, Sloan Digital Sky Survey (SDSS)
Sponsoring Organization:
USDOE
OSTI ID:
2425100
Journal Information:
Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Journal Issue: 3 Vol. 524; ISSN 0035-8711
Publisher:
Oxford University PressCopyright Statement
Country of Publication:
United States
Language:
English

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