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Abstract The existence of a secondary (in addition to compact object mergers) source of heavy element (r-process) nucleosynthesis, the core-collapse of rapidly rotating and highly magnetized massive stars, has been suggested by both simulations and indirect observational evidence. Here, we probe a predicted signature ofr-process enrichment, a late-time (≳40 days post-burst) distinct red color, in observations of gamma-ray burst supernovae (GRB-SNe), which are linked to these massive star progenitors. We present optical to near-IR color measurements of four GRB-SNe atz≲ 0.4, extending out to >500 days post-burst, obtained with the Hubble Space Telescope and large-aperture ground-based telescopes. Comparison of our observations to models indicates that GRBs 030329, 100316D, and 130427A are consistent with both no enrichment and producing 0.01–0.15M⊙ofr-process material if there is a low amount of mixing between the innerr-process ejecta and outer supernova (SN) layers. GRB 190829A is not consistent with any models withr-process enrichment ≥0.01M⊙. Taken together the sample of GRB-SNe indicates color diversity at late times. Our derived yields from GRB-SNe may be underestimated due tor-process material hidden in the SN ejecta (potentially due to low mixing fractions) or the limits of current models in measuringr-process mass. We conclude with recommendations for future search strategies to observe and probe the full distribution ofr-process produced by GRB-SNe.
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The Effects of r-Process Enrichment in Hydrogen-rich Supernovae
Abstract Core-collapse supernovae (SNe) are candidate sites for rapid neutron capture process (r-process) nucleosynthesis. We explore the effects of enrichment fromr-process nuclei on the light curves of hydrogen-rich SNe and assess the detectability of these signatures. We modify the radiation hydrodynamics code, SuperNova Explosion Code, to include the approximate effects of opacity and radioactive heating fromr-process elements in the supernova (SN) ejecta. We present models spanning a range of totalr-process massesMrand their assumed radial distribution within the ejecta, finding thatMr≳ 10−2M⊙is sufficient to induce appreciable differences in their light curves as compared to ordinary hydrogen-rich SNe (without anyr-process elements). The primary photometric signatures ofr-process enrichment include a shortening of the plateau phase, coinciding with the hydrogen-recombination photosphere retreating to ther-process-enriched layers, and a steeper post-plateau decline associated with a reddening of the SN colors. We compare ourr-process-enriched models to ordinary SNe models and observational data, showing that yields ofMr≳ 10−2M⊙are potentially detectable across several of the metrics used by transient observers, provided thatr-process-rich layers are mixed at least halfway to the ejecta surface. This detectability threshold can roughly be reproduced analytically using a two-zone (kilonova-within-an-SN) picture. Assuming that a small fraction of SNe produce a detectabler-process yield ofMr≳ 10−2M⊙, and respecting constraints on the total Galactic production rate, we estimate that ≳103–104SNe need be observed to find oner-enriched event, a feat that may become possible with the Vera Rubin Observatory.
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- Award ID(s):
- 2002577
- PAR ID:
- 10538535
- Publisher / Repository:
- IoP
- Date Published:
- Journal Name:
- The Astrophysical Journal
- Volume:
- 966
- Issue:
- 2
- ISSN:
- 0004-637X
- Page Range / eLocation ID:
- 212
- Format(s):
- Medium: X
- Sponsoring Org:
- National Science Foundation
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- Free Publicly Accessible Full Text
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Accepted Manuscript
- Journal Article:
- https://doi.org/10.3847/1538-4357/ad37fe
