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Evolution of X-ray Binaries and the Formation of Binary Pulsars

Evolution of X-ray Binaries and the Formation of Binary Pulsars. Xiang-Dong Li Department of Astronomy Nanjing University. Millisecond Pulsar (MSP)-X-ray Binary (XRB) Relation. ATNF PSR Database. Spin Frequency Distribution in LMXBs. Binary Pulsar Populations. Binary Pulsar Populations.

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Evolution of X-ray Binaries and the Formation of Binary Pulsars

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  1. Evolution of X-ray Binaries and the Formation of Binary Pulsars Xiang-Dong Li Department of Astronomy Nanjing University NAOC

  2. Millisecond Pulsar (MSP)-X-ray Binary (XRB) Relation ATNF PSR Database NAOC

  3. Spin Frequency Distribution in LMXBs NAOC

  4. Binary Pulsar Populations NAOC

  5. Binary Pulsar Populations From Breton (2009) NAOC

  6. Classification of X-ray Binaries High-mass X-ray binaries (wind-fed X-ray sources) Supergiant HMXBs Be/X-ray binaries Intermediate-mass X-ray binaries Low-mass X-ray binaries (disk-fed X-ray sources) NAOC

  7. Stability of Mass Transfer • The characteristics of binary pulsars depends on mass transfer processes during the XRB phase • The stability of mass transfer depends on • The mass ratio of the donor and accretor • The evolutionary state of the donor NAOC

  8. Ways of Mass Transfer in XRBs • Stable mass transfer on nuclear timescale • Thermal timescale mass transfer • Unstable mass transfer  common envelope Deloye (2008) NAOC

  9. Initial – Final Binary Relation Tauris & Savonije (2000) NAOC

  10. HMXB Evolution Single mildly recycled NS NAOC

  11. Evolution of LMXBs Wide recycled PSR + He WD binary Nuclear evolution-driven mass transfer Close recycled PSR + He WD binary Angular momentum-driven mass transfer Ultracompact X-ray binary or black widow X-ray binary NAOC

  12. Evolution of IMXBs IMXB LMXB NAOC

  13. Binary Pulsars Evolved from I/LMXBs LMXBs IMXBs From Podsiadlowski et al. (2001) NAOC

  14. Other Possibilities NAOC

  15. RGB/AGB PSR J1903+0327 Ps=2.15 ms Porb=95 days Mpsr~1.74 Msun M2>0.88 Msun e = 0.44! Comparison with Observations TTMT CV-like UC-LMXBs NAOC

  16. Mass Accretion and Mass Loss during LMXB Evolution Zhang et al. (2011) NAOC

  17. Conclusions • The standard model for H/I/LMXBs can roughly reproduce the main features of the observed binary pulsars. • However, there are still many unresolved issues… NAOC

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