lomidrevo
- 433
- 250
alantheastronomer said:The pop. II stars, including halo, bulge, and globular clusters, were all formed in one fell swoop, roughly all at the same time and so are considered one population. Their metallicities don't change. The thin disk on the other hand is comprised of a significant amount of gas, and so star formation is continually ongoing. As heavier elements are continuously being produced and mixed into the gas, the metallicity of the disk stars is continuously changing; as you mention.
Yes, that makes sense to me. However, below is a snapshot of a table from a textbook I am reading, Carroll&Ostlie. The metallicity is expressed here as iron-to-hydrogen ratio of the observed star compared to the Sun's value [Fe/H]:
$$
[Fe/H] = \log_{10} \left [ \frac{(N_{Fe}/N_H)_{star}}{(N_{Fe}/N_H)_{sun}} \right ]
$$
Halo: from -5.4 to -0.5
Bulge: from -2.0 to +0.5
(Thick disk: from -2.2 to -0.5)
That is what I had in my mind, when mentioned changing and overlapping of metallicities in my previous post. The declared range for Halo stars is quite wide, isn't it? Indeed, I am not sure how accurate or up-to-date are the data in the table, when browsing I found slightly different values from different sources, eg. this one.
But what is also interesting, the authors mention in the textbook, that correlation between age and [Fe/H] may not be 100% reliable. They suggest that some astronomers rather use [O/H] or [O/Fe] ratios. Probably it is not easy to define stellar populations with such a variety of parameters :)
If you talk about Population II stars, do you mean stars with [Fe/H] very close to -5?