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Formation of Redback and Black Widow Binary Millisecond Pulsars

Formation of Redback and Black Widow Binary Millisecond Pulsars. Kun Jia and Xiang-Dong Li Department of Astronomy Nanjing University. Millisecond Pulsar (MSP)-Low-mass X-ray Binary (LMXB) Relation. Recycling Scenario (Alpar 1982; Radakrishnan & Srinivasan 1982) – Spin up to ms periods

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Formation of Redback and Black Widow Binary Millisecond Pulsars

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  1. Formation of Redback and Black Widow Binary Millisecond Pulsars Kun Jia and Xiang-Dong Li Department of Astronomy Nanjing University KIAA-WAP

  2. Millisecond Pulsar (MSP)-Low-mass X-ray Binary (LMXB) Relation Recycling Scenario (Alpar 1982; Radakrishnan & Srinivasan 1982) – Spin up to ms periods – Magnetic field decay High mass star PSR LMXB MSP KIAA-WAP

  3. Observational evidence for the recycling scenario • Millisecond X-ray pulsations from LMXBs SAX J1808.4-3658 Wijnands & van der Klis 1998 Patruno & Watts 2012 2013-04-25 3 KIAA KIAA-WAP

  4. Observational evidence for the recycling scenario • Transitions between rotation and accretion power in MSPs • PSR J1023+ 0038 (Archibald et al. 2009) • IGR J18245-2452/PSR J1824–2452I (Papitto et al. 2013) • XSS J12270-4859 (Bogdanov et al. 2014) X-ray radio KIAA-WAP

  5. The three transitional pulsars are also eclipsing MSPs Roberts 2013 • Black widows • (semi)-degenerate companion (~0.02 M⊙-0.05 M⊙) • Redbacks • non-degenerate companion (~0.2 M⊙-0.4 M⊙) KIAA-WAP

  6. The eclipsing material possibly originates from the companions evaporated by the high-energy particles from the MSPs KIAA-WAP

  7. Gamma-ray MSPs • > ⅓ of known MSPs are Gamma-ray MSPs • For Ė>5×1033 erg/s is >¾ (!) • Most Fermi MSPs are black widows and redbacks KIAA-WAP

  8. A significant variation in the accretion rate is required to explain the transitional behavior in LMXBs. Linares 2014 KIAA-WAP

  9. The disrupted magnetic braking (MB) model (Chen et al. 2013) MB GR KIAA-WAP

  10. The irradiation-induced cyclic mass transfer model (Benvenuto et al. 2014, 2015) KIAA-WAP

  11. The accretion-induced collapse (AIC) model (Smedley et al. 2015) • Collapse of an accreting white dwarf (WD) to form a MSP • The companion star becomes detached from its Roche lobe because of sudden orbital expansion • Formation rates uncertain • Difficult or impossible for the occurrence of AIC in traditional CVs KIAA-WAP

  12. Transient LMXBs Outburst Quiescence KIAA-WAP

  13. The parameter space for the disk instability • Covers the distribution of known redbacks • If the MSP activity switches on during the quiescent phase of LMXBs, they may evolve to be redbacks KIAA-WAP

  14. Evolution with evaporation • Evaporative wind mass loss rate v2,esc - escape velocity at the surface of the companion star Lp - NS’s spin-down luminosity f- efficiency of evaporation KIAA-WAP

  15. Cases with f = 0.1 KIAA-WAP

  16. Changing f and angular momettum KIAA-WAP

  17. Results • Binary evolution sensitively depends on the angular momentum of the evaporative wind and f • The redback companions • The redback orbital periods • Redback - black widow relation KIAA-WAP

  18. Conclusions • Almost all LMXBs are subject to the thermal and viscous instability during their evolution • The resultant redbacks can possess main-sequence, evolved, and (proto-)WD companions with either Roche lobe filling or under-filling • Part of redbacks may become black widows, while others form MSP/He WD binaries KIAA-WAP

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