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Title: Neutron Stars Exclude Light Dark Baryons

Abstract

Exotic particles carrying baryon number and with a mass of the order of the nucleon mass have been proposed for various reasons including baryogenesis, dark matter, mirror worlds, and the neutron lifetime puzzle. Here, we show that the existence of neutron stars with a mass greater than 0.7 M places severe constraints on such particles, requiring them to be heavier than 1.2 GeV or to have strongly repulsive self-interactions.

Authors:
; ; ;
Publication Date:
Research Org.:
Univ. of Washington, Seattle, WA (United States)
Sponsoring Org.:
USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)
OSTI Identifier:
1463061
Alternate Identifier(s):
OSTI ID: 1498995
Grant/Contract Number:  
[FG02-00ER41132; SC0011637]
Resource Type:
Published Article
Journal Name:
Physical Review Letters
Additional Journal Information:
[Journal Name: Physical Review Letters Journal Volume: 121 Journal Issue: 6]; Journal ID: ISSN 0031-9007
Publisher:
American Physical Society (APS)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; 72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS

Citation Formats

McKeen, David, Nelson, Ann E., Reddy, Sanjay, and Zhou, Dake. Neutron Stars Exclude Light Dark Baryons. United States: N. p., 2018. Web. doi:10.1103/PhysRevLett.121.061802.
McKeen, David, Nelson, Ann E., Reddy, Sanjay, & Zhou, Dake. Neutron Stars Exclude Light Dark Baryons. United States. doi:10.1103/PhysRevLett.121.061802.
McKeen, David, Nelson, Ann E., Reddy, Sanjay, and Zhou, Dake. Mon . "Neutron Stars Exclude Light Dark Baryons". United States. doi:10.1103/PhysRevLett.121.061802.
@article{osti_1463061,
title = {Neutron Stars Exclude Light Dark Baryons},
author = {McKeen, David and Nelson, Ann E. and Reddy, Sanjay and Zhou, Dake},
abstractNote = {Exotic particles carrying baryon number and with a mass of the order of the nucleon mass have been proposed for various reasons including baryogenesis, dark matter, mirror worlds, and the neutron lifetime puzzle. Here, we show that the existence of neutron stars with a mass greater than 0.7 M⊙ places severe constraints on such particles, requiring them to be heavier than 1.2 GeV or to have strongly repulsive self-interactions.},
doi = {10.1103/PhysRevLett.121.061802},
journal = {Physical Review Letters},
number = [6],
volume = [121],
place = {United States},
year = {2018},
month = {8}
}

Journal Article:
Free Publicly Available Full Text
Publisher's Version of Record
DOI: 10.1103/PhysRevLett.121.061802

Citation Metrics:
Cited by: 13 works
Citation information provided by
Web of Science

Figures / Tables:

Figure 1 Figure 1: Hybrid EOS and underlying nuclear EOS. The standard nuclear matter is shown as dash-dotted curves. The stiff EOS makes a second-order transition to a causal EOS at nB = 1.5ns. This is the stiffest possible EOS and predicts a maximum mass of ≃3.3 M (Fig. 2). Adding amore » dark baryon with mχ = 938 MeV results in solid curves, which are dominated by χ’s Fermi gas EOS for ϵ ≳ 0.1 MeV=fm3. Dotted lines show a hybrid EOS with mχ = 1.2 GeV. All curves are truncated at maximum central densities inside stable neutron stars.« less

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    Figures / Tables found in this record:

      Figures/Tables have been extracted from DOE-funded journal article accepted manuscripts.