Main-sequence lifetimes versus initial mass and initial metallicity

The below link is to a TAR file containing text files that contain the main-sequence lifetimes of the BPASSv2.2 single star models. The age given is when a helium core is formed, this occurs once the central hydrogen mass fraction drops below 0.1, so it is a lower limit on the age. The filenames are "He_times_zXXX", where the initial metallicity mass fraction is, Z=0.XXX. Except for zem4 and zem5 which have metallicities of Z=1e-4 and 1e-5 respectively. In each file the first column is the initial mass in solar masses and the second column is the lifetime in years.

Helium and Wolf-Rayet Stellar Models

Stellar models calculated with Cambridge STARS evolution code

Code is available from http://www.ast.cam.ac.uk/~stars/

Stellar models are described in McClelland & Eldridge (2016).

Contact lmcc054@aucklanduni.ac.nz for further details.

There are several files for download at 4 metallicities, Z=0.008, 0.014, 0.020 and 0.040. These are approximately LMC, "new" solar, "old" star and twice solar.

The files are grouped as follows: plotfiles_METALLICITY_CLUMPING_MASSLOSS

MASSLOSS is the scaling factor (beta) applied to the mass-loss rate. Mass-loss scheme is taken from Nugis and Lamers (2000).

CLUMPING is the clumping factor for the inflated envelope. See Graefener et al. (2011) for details.

Each model grid is compressed using XZ Utils. To decompress, use the -J flag with tar. For example, tar -vxJf filename.tar.xz

Evolutionary tracks:

Z=0.008:

Z=0.014:

Z=0.020:

Z=0.040: