Evolution of Xray Binaries and the Formation of
Evolution of X-ray Binaries and the Formation of Binary Pulsars Xiang-Dong Li Department of Astronomy Nanjing University 2011 -5 -11 NAOC 1
Millisecond Pulsar (MSP)-X-ray Binary (XRB) Relation ATNF PSR Database 2011 -5 -11 NAOC 2
Spin Frequency Distribution in LMXBs 2011 -5 -11 NAOC 3
Binary Pulsar Populations Main type Sub-type Recycled PSR + low-mass PSR + (He) WD comp. (MC≤ 0. 45 M⊙) Observational examples PSR J 0437 -4715 PSR J 1640+2224 Mildly recycled PSR + high 1. PSR + NS (double) 1. PSR B 1913+16 -mass compact comp. 2. PSR + (ONe. Mg) WD 2. PSR J 1435 -6100 (0. 5≤MC/M⊙≤ 1. 4) 3. PSR + (CO) WD 3. PSR J 2145 -0750 Non-recycled pulsar (CO) WD + PSR Un-evolved companion 1. PSR + B-type comp. 1. PSR B 1259 -63 2. PSR + low-mass MS 2. PSR B 1820 -11 comp. 2011 -5 -11 NAOC PSR B 2303+46 4
Binary Pulsar Populations 2011 -5 -11 From Breton (2009)NAOC 5
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 2011 -5 -11 Low-mass X-ray binaries (disk-fed X-ray sources) NAOC 6
Stability of Mass Transfer n n The characteristics of binary pulsars depends on mass transfer processes during the XRB phase The stability of mass transfer depends on q q 2011 -5 -11 The mass ratio of the donor and accretor The evolutionary state of the donor NAOC 7
Ways of Mass Transfer in XRBs n n n Stable mass transfer on nuclear timescale Thermal timescale mass transfer Unstable mass transfer common envelope Deloye (2008) 2011 -5 -11 NAOC 8
Initial – Final Binary Relation Tauris & Savonije (2000) 2011 -5 -11 NAOC 9
HMXB Evolution Single mildly recycled NS 2011 -5 -11 NAOC 10
Evolution of LMXBs Wide recycled PSR + He WD binary Nuclear evolutiondriven mass transfer Close recycled PSR + He WD binary Angular momentumdriven mass transfer Ultracompact X-ray binary or black widow Xray binary 2011 -5 -11 NAOC 11
Evolution of IMXBs IMXB 2011 -5 -11 LMXB NAOC 12
Binary Pulsars Evolved from I/LMXBs IMXBs From Podsiadlowski et al. (2001) 2011 -5 -11 NAOC 13
Other Possibilities 2011 -5 -11 NAOC 14
RGB/AGB PSR J 1903+0327 Ps=2. 15 ms Porb=95 days Mpsr~1. 74 Msun M 2>0. 88 Msun e = 0. 44! TTMT CV-like Comparison with Observations UC-LMXBs 2011 -5 -11 NAOC 15
Mass Accretion and Mass Loss during LMXB Evolution Zhang et al. (2011) 2011 -5 -11 NAOC 16
Conclusions n n 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… 2011 -5 -11 NAOC 17
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