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Title: Nuclear Reactions in the Crusts of Accreting Neutron Stars

Abstract

X-ray observations of transiently accreting neutron stars during quiescence provide information about the structure of neutron star crusts and the properties of dense matter. Interpretation of the observational data requires an understanding of the nuclear reactions that heat and cool the crust during accretion and define its non-equilibrium composition. We identify here in detail the typical nuclear reaction sequences down to a depth in the inner crust where the mass density is rho = 2 times 10^12 g cm-3 using a full nuclear reaction network for a range of initial compositions. The reaction sequences differ substantially from previous work. We find a robust reduction of crust impurity at the transition to the inner crust regardless of initial composition, though shell effects can delay the formation of a pure crust somewhat to densities beyond rho = 2 times 10^12 g cm^-3. This naturally explains the small inner crust impurity inferred from observations of a broad range of systems. The exception are initial compositions with A > 102 nuclei, where the inner crust remains impure with an impurity parameter of Qimp≈20 owing to the N=82 shell closure. In agreement with previous work, we find that nuclear heating is relatively robust and independentmore » of initial composition, while cooling via nuclear Urca cycles in the outer crust depends strongly on initial composition. This work forms a basis for future studies of the sensitivity of crust models to nuclear physics and provides profiles of composition for realistic crust models.« less

Authors:
 [1];  [2];  [3]; ORCiD logo [4];  [5];  [4]; ORCiD logo [6];  [7];  [8]; ORCiD logo [9];  [10];  [11];  [12]; ORCiD logo [13];  [2];  [14]
  1. Michigan State Univ., East Lansing, MI (United States); Univ. of Notre Dame, Notre Dame, IN (United States); Technological and Higher Education Institute of Hong Kong (Hong Kong)
  2. Univ. of Notre Dame, Notre Dame, IN (United States)
  3. Indian Institute of Technology Ropar, Punjab (India)
  4. Michigan State Univ., East Lansing, MI (United States); Univ. of Notre Dame, Notre Dame, IN (United States)
  5. Mississippi State Univ., Mississippi State, MS (United States)
  6. Michigan State Univ., East Lansing, MI (United States); Univ. of Notre Dame, Notre Dame, IN (United States); Indiana Univ., Bloomington, IN (United States)
  7. Instituto de Fisica da Univ. de Sao Paulo, Sao Paulo (Brazil)
  8. Coastal Carolina Univ., Conway, SC (United States)
  9. Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States); Univ. of Tennessee, Knoxville, TN (United States)
  10. Michigan State Univ., East Lansing, MI (United States); Univ. of Notre Dame, Notre Dame, IN (United States); Univ. of Maryland, College Park, MD (United States)
  11. Univ. of Notre Dame, Notre Dame, IN (United States); Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
  12. Ioffe Institute, Saint Petersburg (Russia)
  13. Univ. of Notre Dame, Notre Dame, IN (United States); Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States); Univ. of Tennessee, Knoxville, TN (United States)
  14. Extreme Light Infrastructure-Nuclear Physics, Ilfov (Romania)
Publication Date:
Research Org.:
Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States); Mississippi State Univ., Mississippi State, MS (United States); Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Sponsoring Org.:
USDOE Office of Science (SC), Nuclear Physics (NP); USDOE National Nuclear Security Administration (NNSA)
OSTI Identifier:
1454393
Alternate Identifier(s):
OSTI ID: 1459442; OSTI ID: 1463562
Report Number(s):
LA-UR-18-22864
Journal ID: ISSN 1538-4357; TRN: US1901006
Grant/Contract Number:  
AC05-00OR22725; SC0013037; AC52-06NA25396
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal (Online)
Additional Journal Information:
Journal Name: The Astrophysical Journal (Online); Journal Volume: 859; 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; dense matter; nuclear reactions; nucleosynthesis; abundances; stars: neutron; X-rays: binaries; 73 NUCLEAR PHYSICS AND RADIATION PHYSICS; dense matter – nuclear reactions, nucleosynthesis, abundances – stars: neutron – X-rays: binaries; Atomic and Nuclear Physics; Astronomy and Astrophysics

Citation Formats

Lau, Rita, Beard, Mary, Gupta, Sanjib S., Schatz, H., Afanasjev, A. V., Brown, Edward F., Deibel, A. T., Gasques, Leandro R., Hitt, George Wesley, Hix, William Raphael, Keek, Laurens, Moller, Peter, Shternin, Peter S., Steiner, Andrew W., Wiescher, Michael, and Xu, Yi. Nuclear Reactions in the Crusts of Accreting Neutron Stars. United States: N. p., 2018. Web. doi:10.3847/1538-4357/aabfe0.
Lau, Rita, Beard, Mary, Gupta, Sanjib S., Schatz, H., Afanasjev, A. V., Brown, Edward F., Deibel, A. T., Gasques, Leandro R., Hitt, George Wesley, Hix, William Raphael, Keek, Laurens, Moller, Peter, Shternin, Peter S., Steiner, Andrew W., Wiescher, Michael, & Xu, Yi. Nuclear Reactions in the Crusts of Accreting Neutron Stars. United States. https://doi.org/10.3847/1538-4357/aabfe0
Lau, Rita, Beard, Mary, Gupta, Sanjib S., Schatz, H., Afanasjev, A. V., Brown, Edward F., Deibel, A. T., Gasques, Leandro R., Hitt, George Wesley, Hix, William Raphael, Keek, Laurens, Moller, Peter, Shternin, Peter S., Steiner, Andrew W., Wiescher, Michael, and Xu, Yi. Thu . "Nuclear Reactions in the Crusts of Accreting Neutron Stars". United States. https://doi.org/10.3847/1538-4357/aabfe0. https://www.osti.gov/servlets/purl/1454393.
@article{osti_1454393,
title = {Nuclear Reactions in the Crusts of Accreting Neutron Stars},
author = {Lau, Rita and Beard, Mary and Gupta, Sanjib S. and Schatz, H. and Afanasjev, A. V. and Brown, Edward F. and Deibel, A. T. and Gasques, Leandro R. and Hitt, George Wesley and Hix, William Raphael and Keek, Laurens and Moller, Peter and Shternin, Peter S. and Steiner, Andrew W. and Wiescher, Michael and Xu, Yi},
abstractNote = {X-ray observations of transiently accreting neutron stars during quiescence provide information about the structure of neutron star crusts and the properties of dense matter. Interpretation of the observational data requires an understanding of the nuclear reactions that heat and cool the crust during accretion and define its non-equilibrium composition. We identify here in detail the typical nuclear reaction sequences down to a depth in the inner crust where the mass density is rho = 2 times 10^12 g cm-3 using a full nuclear reaction network for a range of initial compositions. The reaction sequences differ substantially from previous work. We find a robust reduction of crust impurity at the transition to the inner crust regardless of initial composition, though shell effects can delay the formation of a pure crust somewhat to densities beyond rho = 2 times 10^12 g cm^-3. This naturally explains the small inner crust impurity inferred from observations of a broad range of systems. The exception are initial compositions with A > 102 nuclei, where the inner crust remains impure with an impurity parameter of Qimp≈20 owing to the N=82 shell closure. In agreement with previous work, we find that nuclear heating is relatively robust and independent of initial composition, while cooling via nuclear Urca cycles in the outer crust depends strongly on initial composition. This work forms a basis for future studies of the sensitivity of crust models to nuclear physics and provides profiles of composition for realistic crust models.},
doi = {10.3847/1538-4357/aabfe0},
journal = {The Astrophysical Journal (Online)},
number = 1,
volume = 859,
place = {United States},
year = {Thu May 24 00:00:00 EDT 2018},
month = {Thu May 24 00:00:00 EDT 2018}
}

Journal Article:
Free Publicly Available Full Text
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Citation Metrics:
Cited by: 25 works
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Figures / Tables:

Figure 1 Figure 1: Column density as a function of mass density for extreme burst ashes. The change in slope around $ρ$ = 6 x 1011 g cm-3 indicates the change of the dominant pressure source from electrons to neutrons.

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text, January 2001


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text, January 2007


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text, January 2008


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text, January 2008


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text, January 2008


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text, January 2008


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text, January 2010


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text, January 2014


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preprint, January 2015


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text, January 2015


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text, January 2016


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text, January 2016


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text, January 2018


Charting the temperature of the Hot Neutron Star in a Soft X-ray Transient
text, January 2000


Thermonuclear Stability of Material Accreting onto a Neutron Star
text, January 2003


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text, January 1993


Works referencing / citing this record:

Continued cooling of the accretion-heated neutron star crust in the X-ray transient IGR J17480–2446 located in the globular cluster Terzan 5
journal, May 2019

  • Ootes, L. S.; Vats, S.; Page, D.
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Long-term temperature evolution of neutron stars undergoing episodic accretion outbursts
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Quiescent X-ray variability in the neutron star Be/X-ray transient GRO J1750−27
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Spallation-altered Accreted Compositions for X-Ray Bursts: Impact on Ignition Conditions and Burst Ashes
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Crust of accreting neutron stars within simplified reaction network
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Crust-cooling Models Are Insensitive to the Crust–Core Transition Pressure for Realistic Equations of State
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Thermal evolution and quiescent emission of transiently accreting neutron stars
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Nuclear Physics of the Outer Layers of Accreting Neutron Stars
text, January 2018


Quiescent X-ray variability in the neutron star Be/X-ray transient GRO J1750-27
text, January 2018


Crust of accreting neutron stars within simplified reaction network
text, January 2019