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Sökning: WFRF:(Dearborn David S.)

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1.
  • Angelou, George C., et al. (författare)
  • Thermohaline mixing and the variation of [C/Fe] with magnitude in M3
  • 2010
  • Ingår i: 11th Symposium on Nuclei in the Cosmos, NIC 2010; Heidelberg; Germany; 19 July 2010 through 23 July 2010.
  • Konferensbidrag (refereegranskat)abstract
    • We use observations of M3 to constrain thermohaline mixing. This is done by matching [C/Fe] and [N/Fe] along the RGB of M3. We find our models can explain observations if it is assumed there is a spread of ∼ 0.3 - 0.4 dex in [C/Fe] in the stars in M3 from their birth. We reproduce the full spread in [C/Fe] at the tip of the RGB. Thermohaline mixing can produce a significant change in [N/Fe] as a function of absolute magnitude on the RGB for initially CN-weak stars, but not for initially CN-strong stars, which have so much nitrogen to begin with that any deep mixing does not significantly affect the surface nitrogen composition.
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2.
  • Dolan, Michelle M., et al. (författare)
  • Evolutionary Tracks For Betelgeuse
  • 2016
  • Ingår i: Astrophysical Journal. - 0004-637X .- 1538-4357. ; 819:1
  • Tidskriftsartikel (refereegranskat)abstract
    • We have constructed a series of nonrotating quasi-hydrostatic evolutionary models for the M2 Iab supergiant Betelgeuse (alpha Orionis). Our models are constrained by multiple observed values for the temperature, luminosity, surface composition, and mass loss for this star, along with the parallax distance and high-resolution imagery that determines its radius. We have then applied our best-fit models to analyze the observed variations in surface luminosity and the size of detected surface bright spots as the result of up-flowing convective material from regions of high temperature in the surface convective zone. We also attempt to explain the intermittently observed periodic variability in a simple radial linear adiabatic pulsation model. Based on the best fit to all observed data, we suggest a best progenitor mass estimate of 20(-3)(+5) M-circle dot and a current age from the start of the zero-age main sequence of 8.0-8.5 Myr based on the observed ejected mass while on the giant branch.
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