Tracks
hr001.d25
Isochrones iso0125.tot Y=0.26, Z=0.01 Xd=2e-5
This Web version consists of a ReadMe file with explanations, and 10 tables
Tracks
hr001.d25
Isochrones iso0125.tot Y=0.26, Z=0.01 Xd=2e-5
Tracks hr001.d45 .
Isochrones iso0145.tot Y=0.26, Z=0.01 Xd=4e-5
Tracks hr002.d15 .
Isochrones iso0215.tot Y=0.28, Z=0.02 Xd=1e-5
Tracks hr002.d25 .
Isochrones iso0225.tot Y=0.28, Z=0.02 Xd=2e-5
Tracks hr002.d45 .
Isochrones iso0245.tot Y=0.28, Z=0.02 Xd=4e-5
In the following files, the imprecise treatment of D-burning is corrected. Further, a smaller central temperature is chosen for the first model, so the scale of times is slightly different from the scale of the 1997 models. Both corrections affect the very low mass tracks. Please make comparisons yourself and report to me any "strange" behaviours.
Tracks 1998
hr00215.1998 , from 0.017 to 0.35Msun
Tracks 1998
hr00225.1998 , from 0.017 to 0.9Msun
Tracks 1998
hr00245.1998 , from 0.017 to 0.3Msun
Isochrones 1998 iso0215.1998 Y=0.28, Z=0.02
Xd=1e-5
Isochrones 1998 iso0225.1998 Y=0.28, Z=0.02
Xd=2e-5
Isochrones 1998 iso0245.1998 Y=0.28, Z=0.02
Xd=4e-5
Additional information on the models can be found in the reference papers:
Presentation of the isochrones:
F.D'Antona and I. Mazzitelli, 1997 , `Evolution of low mass stars' in ``Cool stars in Clusters and Associations'', eds. G. Micela and R. Pallavicini, Mem. S.A.It., 68, 807
Problems concerning the treatment of convection in low mass stars:
F. D'Antona, I. Mazzitelli 1998 , `A role for superadiabatic convection in low mass structures?', in ``Brown Dwarfs and Extrasolar Planets", ASP Conference Series, eds. R. Rebolo, E. Martin, M.R. Zapatero Osorio, p. 442
Reasons why we adopt several initial Deuterium abundances:
Censori, C. & D'Antona, F. 1998 , ``Brown Dwarfs and the luminosity function of young stellar populations", in ``Brown Dwarfs and Extrasolar Planets" ASP Conference Series, eds. R. Rebolo, E. Martin, M.R. Zapatero Osorio, p. 518
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