VFTS meeting: animation of main-sequence model evolution
| Main Author: | Chen Wang |
|---|---|
| Other Authors: | Langer, Norbert, Xu, Xiao-Tian, Schootemeijer, Abel, Hastings, Ben, Marchant, Pablo |
| Format: | info Video eJournal |
| Terbitan: |
, 2020
|
| Subjects: | |
| Online Access: |
https://zenodo.org/record/4067165 |
Daftar Isi:
- This animation shows the evolution of our binary and single stellar models from 2Myr to 100Myr. We populate 3763 binaries, whose primary mass is in the range of 3Msun to 100Msun, following a Salpeter IMF with an exponent of -2.37. The mass ratio is uniformly distributed from 0.1 to 1. The orbital period logP is uniformly distributed from the minimum value at which the two stars would contact initially to 3.5. Both components rotate at half of their critical velocities initially. Considering a binary fraction of 70%, we populate 1612 single stars with vi=0.5. In addition, we also populate 537 slowly-rotating single stars with vi=0.2 to reproduce the observed blue MS in young star clusters. The number is chosen such that the ratio between the slow and fast rotators is 1/3, which is the same as the ratio of observed blue and red MS stars. Gravity darkening and observational errors are included. Filled circles correspond to single stellar models, while open symbols correspond to binaries with different companions. Single stellar tracks with vi=0.5 are plotted with solid grey lines. The black dotted line represents the ZAMS line of vi=0.2 single stellar models. In the legend, the number in each group outside the parenthesis corresponds to the number of stars whose color and magnitude are in the figure range. While the number in the parenthesis corresponds to the number of stars above the orange dashed line, which is 1.75 mag below the turn-off magnitude.