Actinide-rich and Actinide-poor r -process-enhanced Metal-poor Stars Do Not Require Separate r -process Progenitors
Abstract
The astrophysical production site of the heaviest elements in the universe remains a mystery. Incorporating heavy-element signatures of metal-poor, $r$-process-enhanced stars into theoretical studies of $r$-process production can offer crucial constraints on the origin of heavy elements. In this study, we introduce and apply the "actinide-dilution with matching" model to a variety of stellar groups, ranging from actinide-deficient to actinide-enhanced, to empirically characterize r-process ejecta mass as a function of electron fraction. We find that actinide-boost stars do not indicate the need for a unique and separate $r$-process progenitor. Rather, small variations of neutron richness within the same type of $r$-process event can account for all observed levels of actinide enhancements. The very low-$$Y_e$$ , fission-cycling ejecta of an $r$-process event need only constitute 10%–30% of the total ejecta mass to accommodate most actinide abundances of metal-poor stars. We find that our empirical $$Y_e$$ distributions of ejecta are similar to those inferred from studies of GW170817 mass ejecta ratios, which is consistent with neutron-star mergers being a source of the heavy elements in metal-poor, $r$-process-enhanced stars.
- Authors:
-
[1];
[2];
[3];
[4];
[5];
[1]
- Univ. of Notre Dame, IN (United States). Dept. of Physics; Joint Inst. for Nuclear Astrophysics (JINA), East Lansing, MI (United States)
- Joint Inst. for Nuclear Astrophysics (JINA), East Lansing, MI (United States); Massachusetts Inst. of Technology (MIT), Cambridge, MA (United States). Dept. of Physics
- Joint Inst. for Nuclear Astrophysics (JINA), East Lansing, MI (United States); North Carolina State Univ., Raleigh, NC (United States) Dept. of Physics
- Joint Inst. for Nuclear Astrophysics (JINA), East Lansing, MI (United States); Los Alamos National Lab. (LANL), Los Alamos, NM (United States). Theoretical Division
- Univ. of Notre Dame, IN (United States). Dept. of Physics
- Publication Date:
- Research Org.:
- Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC). Nuclear Physics (NP) (SC-26)
- OSTI Identifier:
- 1565905
- Report Number(s):
- LA-UR-19-23313
Journal ID: ISSN 1538-4357; TRN: US2000941
- Grant/Contract Number:
- 89233218CNA000001
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal (Online)
- Additional Journal Information:
- Journal Name: The Astrophysical Journal (Online); Journal Volume: 881; Journal Issue: 1; Journal ID: ISSN 1538-4357
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; Atomic, Nuclear and Particle Physics; Astronomy and Astrophysics
Citation Formats
Holmbeck, Erika M., Frebel, Anna, McLaughlin, G. C., Mumpower, Matthew R., Sprouse, Trevor M., and Surman, Rebecca. Actinide-rich and Actinide-poor r -process-enhanced Metal-poor Stars Do Not Require Separate r -process Progenitors. United States: N. p., 2019.
Web. doi:10.3847/1538-4357/ab2a01.
Holmbeck, Erika M., Frebel, Anna, McLaughlin, G. C., Mumpower, Matthew R., Sprouse, Trevor M., & Surman, Rebecca. Actinide-rich and Actinide-poor r -process-enhanced Metal-poor Stars Do Not Require Separate r -process Progenitors. United States. https://doi.org/10.3847/1538-4357/ab2a01
Holmbeck, Erika M., Frebel, Anna, McLaughlin, G. C., Mumpower, Matthew R., Sprouse, Trevor M., and Surman, Rebecca. Tue .
"Actinide-rich and Actinide-poor r -process-enhanced Metal-poor Stars Do Not Require Separate r -process Progenitors". United States. https://doi.org/10.3847/1538-4357/ab2a01. https://www.osti.gov/servlets/purl/1565905.
@article{osti_1565905,
title = {Actinide-rich and Actinide-poor r -process-enhanced Metal-poor Stars Do Not Require Separate r -process Progenitors},
author = {Holmbeck, Erika M. and Frebel, Anna and McLaughlin, G. C. and Mumpower, Matthew R. and Sprouse, Trevor M. and Surman, Rebecca},
abstractNote = {The astrophysical production site of the heaviest elements in the universe remains a mystery. Incorporating heavy-element signatures of metal-poor, $r$-process-enhanced stars into theoretical studies of $r$-process production can offer crucial constraints on the origin of heavy elements. In this study, we introduce and apply the "actinide-dilution with matching" model to a variety of stellar groups, ranging from actinide-deficient to actinide-enhanced, to empirically characterize r-process ejecta mass as a function of electron fraction. We find that actinide-boost stars do not indicate the need for a unique and separate $r$-process progenitor. Rather, small variations of neutron richness within the same type of $r$-process event can account for all observed levels of actinide enhancements. The very low-$Y_e$ , fission-cycling ejecta of an $r$-process event need only constitute 10%–30% of the total ejecta mass to accommodate most actinide abundances of metal-poor stars. We find that our empirical $Y_e$ distributions of ejecta are similar to those inferred from studies of GW170817 mass ejecta ratios, which is consistent with neutron-star mergers being a source of the heavy elements in metal-poor, $r$-process-enhanced stars.},
doi = {10.3847/1538-4357/ab2a01},
journal = {The Astrophysical Journal (Online)},
number = 1,
volume = 881,
place = {United States},
year = {2019},
month = {8}
}
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Figures / Tables:
Figure 1: Top: Dy versus Zr abundances for metal-poor Milky Way stars with an r -process signature (circles), a measurement of Th (filled circles), an actinide-boost signature (red outlines), or other enrichment (e.g., s-process, i-process, and/or carbon enhancement; crosses). The dashed lines are constant values of log ϵ (Zr/Dy) ofmore »
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Works referencing / citing this record:
r -process Enrichment in the Galactic Halo Characterized by Nucleosynthesis Variation in the Ejecta of Coalescing Neutron Star Binaries
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