Open AccessThird dredge‐up in low‐mass stars: solving the Large Magellanic Cloud carbon star mystery
Author(s) -
Stancliffe Richard J.,
Izzard Robert G.,
Tout Christopher A.
Publication year - 2005
Publication title -
monthly notices of the royal astronomical society: letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.067
H-Index - 122
eISSN - 1745-3933
pISSN - 1745-3925
DOI - 10.1111/j.1745-3933.2005.08491.x
Subject(s) - physics , astrophysics , carbon star , asymptotic giant branch , metallicity , stars , small magellanic cloud , large magellanic cloud , luminosity , luminosity function , star formation , astronomy , galaxy
A long standing problem with asymptotic giant branch (AGB) star models has been their inability to produce the low‐luminosity carbon stars in the Large and Small Magellanic Clouds (LMC and SMC, respectively). Dredge‐up must begin earlier and extend deeper. We find this for the first time in our models of LMC metallicity. Such features are not found in our models of SMC metallicity. The fully implicit and simultaneous stellar evolution code stars has been used to calculate the evolution of AGB stars with metallicities of Z = 0.008 and Z = 0.004 , corresponding to the observed metallicities of the LMC and SMC, respectively. Third dredge‐up occurs in stars of 1 M ⊙ and above and carbon stars were found for models between 1 M ⊙ and 3 M ⊙ . We use the detailed models as input physics for a population synthesis code and generate carbon star luminosity functions. We now find that we are able to reproduce the carbon star luminosity function of the LMC without any manipulation of our models. The SMC carbon star luminosity function still cannot be produced from our detailed models unless the minimum core mass for third dredge‐up is reduced by 0.06 M ⊙ .