Title: New s-process Site in Rapidly-Rotating Massive Pop II Stars
Authors: Projjwal Banerjee, Alexander Heger, Yong-Zhong Qian
First Author’s Institutions: Department of Physics, Indian Institute of Technology Palakkad, India; Department of Astronomy, Shanghai Jiao Tong University, Shanghai, China.
Status: Open access on ArXiv
One of the main goals of nuclear astrophysics is to understand and explain the composition of the universe. Starting out with Hydrogen, Helium and a teeny bit of Lithium, the universe evolved to have an entire periodic table worth of chemical elements. How did this happen? We know that stars and supernovae played a key role in this chemical enrichment. However, exactly how and where different elements are produced, and in what quantities, remains a topic of vigorous ongoing research. Heavy element nucleosynthesis is a key piece of this puzzle and has received a lot of attention recently in the context of neutron star mergers.
Heavy elements, i.e. elements heavier than iron, are mainly formed through the s-process and the r-process. The s-process involves slow neutron capture and the r-process involves rapid neutron capture with respect to the decay time of the isotopes involved. Typical s- and r-process paths in the chart of nuclides are shown in Figure 1. The main thing to note here is that the s-process stays fairly close to the black dots indicating stable nuclei whereas the r-process proceeds far away from stability.
Although both these processes make roughly equal overall contribution to the total abundance of heavy elements, the s-process does not get the same hype as it’s cool twin, the r-process. This is partly due to the fact that the site of the r-process was a huge mystery until very recently, when neutron star mergers were identified as one of the sites where the process occurs. It still remains to be seen whether they are the only site of the r-process.
The s-process, on the other hand, is known to occur inside asymptotic giant branch (AGB) stars. This is the final stage of evolution for long-lived, low-mass stars between 1-3 solar masses. The AGB stars can produce elements up to 209Bi, forming what’s called the “main” component of the s-process. However, a weaker version of the s-process also happens in massive stars (>10 solar masses), producing elements up to atomic mass number (A) ~ 90. Today’s paper shakes things up by introducing a new site for the main s-process – in rotating metal-poor massive stars!
The authors find that above a critical rotation speed, massive metal-poor stars evolve in a quasi-chemically-homogeneous (QCH) manner. This means the stars are spinning so fast that the rotationally induced mixing is very efficient. At the end of core hydrogen-burning, which produces Helium, these stars look like Helium stars. We can see this in panel (a) of Figure 2. Now starts the story of the s-process, which goes like this:
1) The star in the QCH state starts burning Helium in the center, producing 12C. Its core becomes convective.
2) The convective core grows in size. Some of the 12C is mixed outward into the radiative region of the star. In this region, there are still some protons present, along with the right thermodynamic conditions to allow 12C to react with protons. This produces 13C.
3) Some 13C is mixed back into the convective He-burning core. In regions that are hot enough, 13C reacts efficiently with the 4He, producing oxygen, as well as neutrons. This leads to high neutron densities that allow the s-process to happen!
We can see this play out in panels (b) through (d) of Figure 2.
In Figure 3, we can see the amount of heavy elements present during different stages of the star’s evolution. There is a clear and strong s-process pattern leading all the way up to lead!
Apart from being interesting in its own right, this new site may also be important for explaining the abundance patterns seen in very metal-poor (VMP) stars. These are old stars thought to reflect the composition of the interstellar medium at ~1 Gyr after the Big Bang. This is much too early for low-mass stars to contribute any s-process elements (they evolve slowly), implying that the heavy element abundances seen in VMP stars must come from the r-process. However, if a strong s-process is possible in massive stars as well, we cannot be so sure! Massive stars live fast and die young, which would allow for an earlier onset of s-process enrichment. Figure 4 shows s-process yield patterns from the authors’ calculations, compared to abundances observed in two VMP stars. The fits are quite good, presenting a potential explanation for VMP observations.
Of course, we should remember that this is an initial exploration of a new idea, though it seems promising. Stay tuned to see where the research leads!