From Be X-Ray Binaries to Double Neutron Stars: Exploring the Spin and Orbital Evolution
We explore the evolutionary link between Galactic Be X-ray binaries (BeXBs) and Galactic field double neutron stars (DNSs) based on the properties of the NS spin period—<i>P</i> and binary orbital period—<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML"...
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| author | Yungang Zhou Dehua Wang Chengmin Zhang |
| author_facet | Yungang Zhou Dehua Wang Chengmin Zhang |
| author_sort | Yungang Zhou |
| collection | DOAJ |
| description | We explore the evolutionary link between Galactic Be X-ray binaries (BeXBs) and Galactic field double neutron stars (DNSs) based on the properties of the NS spin period—<i>P</i> and binary orbital period—<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>P</mi><mi>orb</mi></msub></semantics></math></inline-formula>. First, both BeXB and DNS sources show positive correlation trends in <i>P</i> versus <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>P</mi><mi>orb</mi></msub></semantics></math></inline-formula> relation (<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>P</mi><mo>−</mo><msub><mi>P</mi><mi>orb</mi></msub></mrow></semantics></math></inline-formula> diagram), which may relate to the influence of the accretion evolution. Secondly, the two types of sources exhibit similar bi-modal <i>P</i>/<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>P</mi><mi>orb</mi></msub></semantics></math></inline-formula> distributions with the gaps of <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>P</mi><mo>∼</mo><mn>40</mn></mrow></semantics></math></inline-formula> s/<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msub><mi>P</mi><mi>orb</mi></msub><mo>∼</mo><mn>60</mn></mrow></semantics></math></inline-formula> days for BeXBs and <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>P</mi><mo>∼</mo><mn>50</mn></mrow></semantics></math></inline-formula> ms/<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msub><mi>P</mi><mi>orb</mi></msub><mo>∼</mo><mn>1</mn></mrow></semantics></math></inline-formula> day for DNSs, respectively. We propose a possibility that Galactic BeXBs may transfer the bi-modal <i>P</i>/<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>P</mi><mi>orb</mi></msub></semantics></math></inline-formula> classifications to Galactic field DNSs during the evolution process. Furthermore, based on the bi-modal gaps, we infer the contraction factors of <i>P</i> (by <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>∼</mo><mstyle scriptlevel="0" displaystyle="true"><mfrac><mn>1</mn><mn>800</mn></mfrac></mstyle></mrow></semantics></math></inline-formula>) and <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>P</mi><mi>orb</mi></msub></semantics></math></inline-formula> (by <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>∼</mo><mstyle scriptlevel="0" displaystyle="true"><mfrac><mn>1</mn><mn>60</mn></mfrac></mstyle></mrow></semantics></math></inline-formula>) valuesin the evolution from Galactic BeXBs to Galactic field DNSs. We find that the scaled <i>P</i> or <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>P</mi><mi>orb</mi></msub></semantics></math></inline-formula> values of Galactic BeXBs share the similar bi-modal distributions to that of Galactic field DNSs, and these results can offer a reference to trace the classification and evolution between the two types of sources. |
| format | Article |
| id | doaj-art-b6885646bbc141da8204f2bbd6390896 |
| institution | DOAJ |
| issn | 2218-1997 |
| language | English |
| publishDate | 2025-02-01 |
| publisher | MDPI AG |
| record_format | Article |
| series | Universe |
| spelling | doaj-art-b6885646bbc141da8204f2bbd63908962025-08-20T03:12:04ZengMDPI AGUniverse2218-19972025-02-011125110.3390/universe11020051From Be X-Ray Binaries to Double Neutron Stars: Exploring the Spin and Orbital EvolutionYungang Zhou0Dehua Wang1Chengmin Zhang2School of Physics and Electronic Science, Guizhou Normal University, Guiyang 550025, ChinaSchool of Physics and Electronic Science, Guizhou Normal University, Guiyang 550025, ChinaCAS Key Lab of FAST, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, ChinaWe explore the evolutionary link between Galactic Be X-ray binaries (BeXBs) and Galactic field double neutron stars (DNSs) based on the properties of the NS spin period—<i>P</i> and binary orbital period—<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>P</mi><mi>orb</mi></msub></semantics></math></inline-formula>. First, both BeXB and DNS sources show positive correlation trends in <i>P</i> versus <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>P</mi><mi>orb</mi></msub></semantics></math></inline-formula> relation (<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>P</mi><mo>−</mo><msub><mi>P</mi><mi>orb</mi></msub></mrow></semantics></math></inline-formula> diagram), which may relate to the influence of the accretion evolution. Secondly, the two types of sources exhibit similar bi-modal <i>P</i>/<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>P</mi><mi>orb</mi></msub></semantics></math></inline-formula> distributions with the gaps of <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>P</mi><mo>∼</mo><mn>40</mn></mrow></semantics></math></inline-formula> s/<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msub><mi>P</mi><mi>orb</mi></msub><mo>∼</mo><mn>60</mn></mrow></semantics></math></inline-formula> days for BeXBs and <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>P</mi><mo>∼</mo><mn>50</mn></mrow></semantics></math></inline-formula> ms/<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msub><mi>P</mi><mi>orb</mi></msub><mo>∼</mo><mn>1</mn></mrow></semantics></math></inline-formula> day for DNSs, respectively. We propose a possibility that Galactic BeXBs may transfer the bi-modal <i>P</i>/<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>P</mi><mi>orb</mi></msub></semantics></math></inline-formula> classifications to Galactic field DNSs during the evolution process. Furthermore, based on the bi-modal gaps, we infer the contraction factors of <i>P</i> (by <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>∼</mo><mstyle scriptlevel="0" displaystyle="true"><mfrac><mn>1</mn><mn>800</mn></mfrac></mstyle></mrow></semantics></math></inline-formula>) and <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>P</mi><mi>orb</mi></msub></semantics></math></inline-formula> (by <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>∼</mo><mstyle scriptlevel="0" displaystyle="true"><mfrac><mn>1</mn><mn>60</mn></mfrac></mstyle></mrow></semantics></math></inline-formula>) valuesin the evolution from Galactic BeXBs to Galactic field DNSs. We find that the scaled <i>P</i> or <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>P</mi><mi>orb</mi></msub></semantics></math></inline-formula> values of Galactic BeXBs share the similar bi-modal distributions to that of Galactic field DNSs, and these results can offer a reference to trace the classification and evolution between the two types of sources.https://www.mdpi.com/2218-1997/11/2/51pulsarbinary pulsarBe X-ray binarydouble neutron star |
| spellingShingle | Yungang Zhou Dehua Wang Chengmin Zhang From Be X-Ray Binaries to Double Neutron Stars: Exploring the Spin and Orbital Evolution Universe pulsar binary pulsar Be X-ray binary double neutron star |
| title | From Be X-Ray Binaries to Double Neutron Stars: Exploring the Spin and Orbital Evolution |
| title_full | From Be X-Ray Binaries to Double Neutron Stars: Exploring the Spin and Orbital Evolution |
| title_fullStr | From Be X-Ray Binaries to Double Neutron Stars: Exploring the Spin and Orbital Evolution |
| title_full_unstemmed | From Be X-Ray Binaries to Double Neutron Stars: Exploring the Spin and Orbital Evolution |
| title_short | From Be X-Ray Binaries to Double Neutron Stars: Exploring the Spin and Orbital Evolution |
| title_sort | from be x ray binaries to double neutron stars exploring the spin and orbital evolution |
| topic | pulsar binary pulsar Be X-ray binary double neutron star |
| url | https://www.mdpi.com/2218-1997/11/2/51 |
| work_keys_str_mv | AT yungangzhou frombexraybinariestodoubleneutronstarsexploringthespinandorbitalevolution AT dehuawang frombexraybinariestodoubleneutronstarsexploringthespinandorbitalevolution AT chengminzhang frombexraybinariestodoubleneutronstarsexploringthespinandorbitalevolution |