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Title: Nuclear processes in other universes: Varying the strength of the weak force

Abstract

Motivated by the possibility that the laws of physics could be different in other regions of space-time, here we consider nuclear processes in universes where the weak interaction is either stronger or weaker than observed. We focus on the physics of both big bang nucleosynthesis (BBN) and stellar evolution. For sufficiently ineffective weak interactions, neutrons do not decay during BBN, and the baryon-to-photon ratio η must be smaller in order for protons to survive without becoming incorporated into larger nuclei. For stronger weak interactions, neutrons decay before the onset of BBN, and the early Universe is left with nearly a pure hydrogen composition. We then consider stellar structure and evolution for the different nuclear compositions resulting from BBN, a wide range of weak force strengths, and the full range of stellar masses for a given universe. We delineate the range of this parameter space that supports working stars, along with a determination of the dominant nuclear reactions over the different regimes. Deuterium burning dominates the energy generation in stars when the weak force is sufficiently weak, whereas proton-proton burning into helium-3 dominates for the regime where the weak force is much stronger than in our Universe. Finally, although stars inmore » these universes are somewhat different, they have comparable surface temperatures, luminosities, radii, and lifetimes so that a wide range of such universes remain potentially habitable.« less

Authors:
 [1];  [2];  [3]
  1. Univ. of Michigan, Ann Arbor, MI (United States). Dept. of Astronomy
  2. Univ. of California, Berkeley, CA (United States). Dept. of Physics; Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
  3. Univ. of Michigan, Ann Arbor, MI (United States). Dept. of Astronomy. Dept. of Physics
Publication Date:
Research Org.:
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Sponsoring Org.:
USDOE National Nuclear Security Administration (NNSA); John Templeton Foundation (United States); Univ. of Michigan (United States); National Science Foundation (NSF); Heising-Simons Foundation (United States)
OSTI Identifier:
1482006
Alternate Identifier(s):
OSTI ID: 1471759
Report Number(s):
LA-UR-18-25809
Journal ID: ISSN 2470-0010
Grant/Contract Number:  
AC52-06NA25396; ID55112; PHY-1630782; 2017-228
Resource Type:
Accepted Manuscript
Journal Name:
Physical Review D
Additional Journal Information:
Journal Volume: 98; Journal Issue: 6; Journal ID: ISSN 2470-0010
Publisher:
American Physical Society (APS)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; anthropic considerations; big bang nucleosynthesis; formation & evolution of stars & galaxies; H & He burning

Citation Formats

Howe, Alex R., Grohs, Evan, and Adams, Fred C. Nuclear processes in other universes: Varying the strength of the weak force. United States: N. p., 2018. Web. https://doi.org/10.1103/PhysRevD.98.063014.
Howe, Alex R., Grohs, Evan, & Adams, Fred C. Nuclear processes in other universes: Varying the strength of the weak force. United States. https://doi.org/10.1103/PhysRevD.98.063014
Howe, Alex R., Grohs, Evan, and Adams, Fred C. Thu . "Nuclear processes in other universes: Varying the strength of the weak force". United States. https://doi.org/10.1103/PhysRevD.98.063014. https://www.osti.gov/servlets/purl/1482006.
@article{osti_1482006,
title = {Nuclear processes in other universes: Varying the strength of the weak force},
author = {Howe, Alex R. and Grohs, Evan and Adams, Fred C.},
abstractNote = {Motivated by the possibility that the laws of physics could be different in other regions of space-time, here we consider nuclear processes in universes where the weak interaction is either stronger or weaker than observed. We focus on the physics of both big bang nucleosynthesis (BBN) and stellar evolution. For sufficiently ineffective weak interactions, neutrons do not decay during BBN, and the baryon-to-photon ratio η must be smaller in order for protons to survive without becoming incorporated into larger nuclei. For stronger weak interactions, neutrons decay before the onset of BBN, and the early Universe is left with nearly a pure hydrogen composition. We then consider stellar structure and evolution for the different nuclear compositions resulting from BBN, a wide range of weak force strengths, and the full range of stellar masses for a given universe. We delineate the range of this parameter space that supports working stars, along with a determination of the dominant nuclear reactions over the different regimes. Deuterium burning dominates the energy generation in stars when the weak force is sufficiently weak, whereas proton-proton burning into helium-3 dominates for the regime where the weak force is much stronger than in our Universe. Finally, although stars in these universes are somewhat different, they have comparable surface temperatures, luminosities, radii, and lifetimes so that a wide range of such universes remain potentially habitable.},
doi = {10.1103/PhysRevD.98.063014},
journal = {Physical Review D},
number = 6,
volume = 98,
place = {United States},
year = {2018},
month = {9}
}

Journal Article:

Citation Metrics:
Cited by: 2 works
Citation information provided by
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Figures / Tables:

FIG. 1 FIG. 1: The $n$↔ $p$ rates in standard BBN versus decreasing comoving temperature parameter (equivalent to increasing time) from Ref. [26]. Plotted for comparison is the Hubble expansion rate $H$ as a dotted black line.

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