The Impacts of Neutron Star Structure and Base Heating on Type I X-Ray Bursts and Code Comparison
Abstract Type I X-ray bursts are rapidly brightening phenomena triggered by thermonuclear burning on the accreting layers of a neutron star (NS). The light curves represent the physical properties of NSs and the nuclear reactions on the proton-rich nuclei. The numerical treatments of the accreting N...
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Published in | The Astrophysical journal Vol. 950; no. 2; pp. 110 - 120 |
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Main Authors | , , , , , , , , |
Format | Journal Article |
Language | English |
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The American Astronomical Society
01.06.2023
IOP Publishing |
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Abstract | Abstract
Type I X-ray bursts are rapidly brightening phenomena triggered by thermonuclear burning on the accreting layers of a neutron star (NS). The light curves represent the physical properties of NSs and the nuclear reactions on the proton-rich nuclei. The numerical treatments of the accreting NS and physics of the NS interior are not established, which shows uncertainty in modeling for observed X-ray light curves. In this study, we investigate theoretical X-ray burst models compared with burst light curves with GS 1826-24 observations. We focus on the impacts of the NS mass and radius and base heating on the NS surface using the
MESA
code. We find a monotonic correlation between the NS mass and the parameters of the light curve. The higher the mass, the longer the recurrence time and the greater the peak luminosity. While the larger the radius, the longer the recurrence time, the peak luminosity remains nearly constant. In the case of increasing base heating, both the recurrence time and peak luminosity decrease. We also examine the above results with a different numerical code,
HERES
, based on general relativity and consider the central NS. We find that the burst rate, energy, and strength are almost the same in two X-ray burst codes by adjusting the base heat parameter in
MESA
(the relative errors ≲5%), while the duration and rise times are significantly different between (the relative error is possibly ∼50%). The peak luminosity and the e-folding time change irregularly between two codes for different accretion rates. |
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AbstractList | Type I X-ray bursts are rapidly brightening phenomena triggered by thermonuclear burning on the accreting layers of a neutron star (NS). The light curves represent the physical properties of NSs and the nuclear reactions on the proton-rich nuclei. The numerical treatments of the accreting NS and physics of the NS interior are not established, which shows uncertainty in modeling for observed X-ray light curves. In this study, we investigate theoretical X-ray burst models compared with burst light curves with GS 1826-24 observations. We focus on the impacts of the NS mass and radius and base heating on the NS surface using the MESA code. We find a monotonic correlation between the NS mass and the parameters of the light curve. The higher the mass, the longer the recurrence time and the greater the peak luminosity. While the larger the radius, the longer the recurrence time, the peak luminosity remains nearly constant. In the case of increasing base heating, both the recurrence time and peak luminosity decrease. We also examine the above results with a different numerical code, HERES , based on general relativity and consider the central NS. We find that the burst rate, energy, and strength are almost the same in two X-ray burst codes by adjusting the base heat parameter in MESA (the relative errors ≲5%), while the duration and rise times are significantly different between (the relative error is possibly ∼50%). The peak luminosity and the e-folding time change irregularly between two codes for different accretion rates. Abstract Type I X-ray bursts are rapidly brightening phenomena triggered by thermonuclear burning on the accreting layers of a neutron star (NS). The light curves represent the physical properties of NSs and the nuclear reactions on the proton-rich nuclei. The numerical treatments of the accreting NS and physics of the NS interior are not established, which shows uncertainty in modeling for observed X-ray light curves. In this study, we investigate theoretical X-ray burst models compared with burst light curves with GS 1826-24 observations. We focus on the impacts of the NS mass and radius and base heating on the NS surface using the MESA code. We find a monotonic correlation between the NS mass and the parameters of the light curve. The higher the mass, the longer the recurrence time and the greater the peak luminosity. While the larger the radius, the longer the recurrence time, the peak luminosity remains nearly constant. In the case of increasing base heating, both the recurrence time and peak luminosity decrease. We also examine the above results with a different numerical code, HERES , based on general relativity and consider the central NS. We find that the burst rate, energy, and strength are almost the same in two X-ray burst codes by adjusting the base heat parameter in MESA (the relative errors ≲5%), while the duration and rise times are significantly different between (the relative error is possibly ∼50%). The peak luminosity and the e-folding time change irregularly between two codes for different accretion rates. |
Author | Xu, Renxin Lü, Guoliang Zhen, Guoqing Zhu, Chunhua Nishimura, Nobuya Song, Liyu Liu, Helei Dohi, Akira Wang, Weiyang |
Author_xml | – sequence: 1 givenname: Guoqing surname: Zhen fullname: Zhen, Guoqing organization: Xinjiang University School of Physical Science and Technology, Urumqi 830046, People's Republic of China – sequence: 2 givenname: Guoliang surname: Lü fullname: Lü, Guoliang organization: Chinese Academy of Science Xinjiang Astronomical Observatory, 150 Science 1-Street, Urumqi 830011, People's Republic of China – sequence: 3 givenname: Helei orcidid: 0000-0001-8706-1882 surname: Liu fullname: Liu, Helei organization: Xinjiang University School of Physical Science and Technology, Urumqi 830046, People's Republic of China – sequence: 4 givenname: Akira orcidid: 0000-0001-8726-5762 surname: Dohi fullname: Dohi, Akira organization: Interdisciplinary Theoretical and Mathematical Sciences Program (iTHEMS) , RIKEN, Wako, Saitama 351-0198, Japan – sequence: 5 givenname: Nobuya orcidid: 0000-0002-0842-7856 surname: Nishimura fullname: Nishimura, Nobuya organization: RIKEN Nishina Center for Accelerator-Based Science , RIKEN, Wako, Saitama 351-0198, Japan – sequence: 6 givenname: Chunhua surname: Zhu fullname: Zhu, Chunhua organization: Xinjiang University School of Physical Science and Technology, Urumqi 830046, People's Republic of China – sequence: 7 givenname: Liyu surname: Song fullname: Song, Liyu organization: Xinjiang University School of Physical Science and Technology, Urumqi 830046, People's Republic of China – sequence: 8 givenname: Weiyang orcidid: 0000-0001-9036-8543 surname: Wang fullname: Wang, Weiyang organization: Peking University Kavli Institute for Astronomy and Astrophysics, Beijing 100871, People's Republic of China – sequence: 9 givenname: Renxin orcidid: 0000-0002-9042-3044 surname: Xu fullname: Xu, Renxin organization: Peking University Kavli Institute for Astronomy and Astrophysics, Beijing 100871, People's Republic of China |
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Type I X-ray bursts are rapidly brightening phenomena triggered by thermonuclear burning on the accreting layers of a neutron star (NS). The light... Type I X-ray bursts are rapidly brightening phenomena triggered by thermonuclear burning on the accreting layers of a neutron star (NS). The light curves... |
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SubjectTerms | Accretion Neutron stars Nuclear abundances X-ray bursts |
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Title | The Impacts of Neutron Star Structure and Base Heating on Type I X-Ray Bursts and Code Comparison |
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