1. Close-by young isolated neutron stars (and black holes) Sergey Popov (Sternberg Astronomical Institute)

2. Plan of the talk NS: introduction Close-by NSs Population synthesis Test of cooling curves Close-by BHs Final conclusions http://xray.sai.msu.ru/~polar/html/kniga.html

3. Neutron stars: introduction Progenitors – massive stars Born in SN explosions R=10 km  =10 14 g/cm 3 (nuclear density) Appear in many flavours Radio pulsars X-ray binaries AXPs SGRs CCOs RINSs

4. Evolution of NS: spin + magnetic field Ejector → Propeller → Accretor → Georotator (Lipunov 1992) (astro-ph/0101031) 1 – spin-down 2 – passage through a molecular cloud 3 – magnetic field decay

5. Evolution of NSs: temperature Yakovlev et al. (1999) Physics Uspekhi

6. Close-by radioquiet NSs Discovery: Walter et al. (1996) Proper motion and distance: Kaplan et al. No pulsations Thermal spectrum Later on: six brothers RX J1856.5-3754

7. Magnificent Seven NamePeriod, s RX 1856 - RX 0720 8.39 RBS 1223 10.31 RBS 1556 - RX 0806 11.37 RX 0420 3.45 RBS 1774 9.44 Radioquiet Close-by Thermal emission Long periods

8. Population of close-by young NSs Magnificent seven Geminga and 3EG J1853+5918 Four radio pulsars with thermal emission (B0833-45; B0656+14; B1055-52; B1929+10) Seven older radio pulsars, without detected thermal emission. We need population synthesis studies of this population

9. Population synthesis: ingredients Birth rate Initial spatial distribution Spatial velocity (kick) Mass spectrum Thermal evolution Interstellar absorption Detector properties A brief review on population synthesis in astrophysics can be found in astro-ph/04011792

10. Solar vicinity Solar neighborhood is not a typical region of our Galaxy Gould Belt R=300-500 pc Age: 30-50 Myrs 20-30 SN per Myr (Grenier 2000) The Local Bubble Up to six SN in a few Myrs

11. The Gould Belt Poppel (1997) R=300 – 500 pc Age 30-50 Myrs Center at 150 pc from the Sun Inclined respect to the galactic plane at 20 degrees 2/3 massive stars in 600 pc belong to the Belt

12. Mass spectrum of NSs Mass spectrum of local young NSs can be different from the general one (in the Galaxy) Hipparcos data on near- by massive stars Progenitor vs NS mass: Timmes et al. (1996); Woosley et al. (2002) astro-ph/0305599

13. Cooling of NSs Direct URCA Modified URCA Neutrino bremstrahlung Superfluidity Exotic matter (pions, quarks, hyperons, etc.) Kaminker et al. (2001)

14. Log N – Log S Task: to understand the Gould Belt contribution Calculate separately disc (without the belt) and both together Cooling curves from Kaminker et al. (2001) Flat mass spectrum Single maxwellian kick R belt =500 pc astro-ph/0304141

15. Log N – Log S as an additional test Standard test: Age – Temperature Sensitive to ages <10 5 years Uncertain age and temperature Non-uniform sample Log N – Log S Sensitive to ages >10 5 years Definite N (number) and S (flux) Uniform sample Two test are perfect together!!! astro-ph/0411618

16. List of models (Blaschke et al. 2004) Model I. Pions. Model II. No pions. Model III. Pions. Model IV. No pions. Model V. Pions. Model VI. No pions. Model VII. Pions. Model VIII.Pions. Model IX. Pions. Blaschke et al. used 16 sets of cooling curves. They were different in three main respects: 1. Absence or presence of pion condensate 2. Different gaps for superfluid protons and neutrons 3. Different T s -T in

17. Model I Pions. Gaps from Takatsuka & Tamagaki (2004) T s -T in from Blaschke, Grigorian, Voskresenky (2004) Can reproduce observed Log N – Log S

18. Model II No Pions Gaps from Yakovlev et al. (2004), 3 P 2 neutron gap suppressed by 0.1 T s -T in from Tsuruta (1979) Cannot reproduce observed Log N – Log S

19. Model III Pions Gaps from Yakovlev et al. (2004), 3 P 2 neutron gap suppressed by 0.1 T s -T in from Blaschke, Grigorian, Voskresenky (2004) Cannot reproduce observed Log N – Log S

20. Model IV No Pions Gaps from Yakovlev et al. (2004), 3 P 2 neutron gap suppressed by 0.1 T s -T in from Blaschke, Grigorian, Voskresenky (2004) Cannot reproduce observed Log N – Log S

21. Model V Pions Gaps from Yakovlev et al. (2004), 3 P 2 neutron gap suppressed by 0.1 T s -T in from Tsuruta (1979) Cannot reproduce observed Log N – Log S

22. Model VI No Pions Gaps from Yakovlev et al. (2004), 3 P 2 neutron gap suppressed by 0.1 T s -T in from Yakovlev et al. (2004) Cannot reproduce observed Log N – Log S

23. Model VII Pions Gaps from Yakovlev et al. (2004), 3 P 2 neutron gap suppressed by 0.1. 1 P 0 proton gap suppressed by 0.5 T s -T in from Blaschke, Grigorian, Voskresenky (2004) Cannot reproduce observed Log N – Log S

24. Model VIII Pions Gaps from Yakovlev et al. (2004), 3 P 2 neutron gap suppressed by 0.1. 1 P 0 proton gap suppressed by 0.2 and 1 P 0 neutron gap suppressed by 0.5. T s -T in from Blaschke, Grigorian, Voskresenky (2004) Can reproduce observed Log N – Log S

25. Model IX No Pions Gaps from Takatsuka & Tamagaki (2004) T s -T in from Blaschke, Grigorian, Voskresenky (2004) Can reproduce observed Log N – Log S

26. Resume Magnificent Seven and other close-by NSs are genetically connected with the Gould Belt Log N – Log S for close-by NSs can serve as a test for cooling curves Two tests (LogN–LogS and Age-Temperature) are perfect together.

27. Black holes Black holes are born from very massive progenitors It is very difficult to observe as isolated BH: Microlensing Weak accretion …….? It is important to try to estimate at least approximate positions

28. Close-by BHs and runaway stars 56 runaway stars inside 750 pc (Hoogerwerf et al. 2001) Four of them have M > 30 M solar Prokhorov, Popov (2002) StarMassVelocity km/s Age, Myr ξ Per33651 HD 64760 25-35316 ς Pup67622 λ Cep40-65744.5

29. Supernova explosion in a binary

30. ς Pup Distance: 404-519 pc Velocity: 33-58 km/s Error box: 12 o x 12 o N EGRET : 1

31. ξ Per Distance: 537-611 pc Velocity: 19-70 km/s Error box: 7 o x 7 o N EGRET : 1

32. Resume Approximate positions of young close-by BHs can be estimated basing on data on massive runaway stars For two cases we obtained relatively small error boxes For HD 64760 and for λ Cep we obtained very large error boxes (40-50 o ) Several EGRET sources inside

33. Final conclusions We live in the region of the Galaxy enriched with young NSs and BHs NSs appear as radio pulsars, gamma and X-ray sources Local population teaches us that radio pulsars do not represent all young NSs Log N – Log S can be a good additional test for cooling curves of NSs Position of close-by isolated BHs can be roughly estimated for those originated from binary systems