Revisiting the Perseus Cluster III: Role of Aspherical Explosions on its Chemical Composition and Extension to Metal-Poor Stars and Galaxies

Abstract

The Perseus Cluster has been precisely measured by the legacy Hitomi telescope on the Si-group (Si, S, Ar, Ca) and Fe-group elements (Cr, Mn, Ni). These element abundance ratios provide insight into the typical behaviour of supernovae. In Paper II, we presented new massive star explosion models at various metallicity, assuming spherical explosions. We show that while the fitting is improved, some features (e.g., Ni/Fe) remain to be improved. In this article, we extend our calculation to an aspherical explosion using the jet-induced explosion mechanism. The detailed pre- and post-explosion chemical profiles are calculated with a large post-processing network to capture the production of odd-number elements (V, Mn, Cu) and iron-group elements. We further explore how the jet-driven explosions create the diversity of models which could be compatible with the observed diversity in terms of $^{56}$Ni-mass vs ejecta mass, Ti-V relation, and stellar abundances. Finally, we apply the new collapsar models in the Galactic Chemical Evolution context. We study how the galactic stars, including the Zn-enriched star HE 1327-2326, can put constraints on the relative rates of collapsar and some of its model parameters. We show that collapsar could lead to significant changes in some elements, e.g., Zn. Our study shows that the collapsar is a necessary component to explain multiple elemental trends observed in the Milky Way Galaxy.

Figures (16)

• Figure 1: (top panel) The pre-explosion density (blue lines) and temperature (orange lines) profiles for the M40-series. The solid lines correspond to the initial profile used in this work, and the dashed lines correspond to that from Nomoto2013ARAA used in Leung2023Jet1. (bottom panel) The pre-explosion chemical composition profile used for the M40 series (solid lines) and that from Nomoto2013ARAA. The $^{28}$Si (green lines), $^{16}$ (orange lines) and $^{4}$He (blue lines) profiles are presented.
• Figure 2: (top panel) The energy evolution of the characteristic model M40-100-100 for the kinetic energy (blue solid line), internal energy (orange dashed line), absolute value of the potential energy (green dot-dashed line) and the total energy (red dotted line). (bottom panel) The statistics of the thermodynamics history of the tracers, showing the tracer maximum temperature and their corresponding density. Each point corresponds to the average $T_{\rm max}$ for each density bin and the error bar represents the standard deviation. The M40-100-100 (blue circles) and N40-1000-1000 Leung2023Jet1.
• Figure 3: The chemical composition [X$_i$/$^{56}$Fe] for M40-100-100 after all short-lived radioactive isotopes have decayed. The two horizontal lines correspond to two times (upper line) and half (lower line) of the solar value.
• Figure 4: The elemental mass fraction [X/Fe] for M40-100-100.
• Figure 5: The initial tracer distribution for both bound by gravity (blue circles) and ejected (pink triangles). The annotations and circles correspond to the element shell from the pre-explosion models for M20-100-100 (top panel), M30-100-100 (middle panel) and M40-100-100 (bottom panel).