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Databases on NSs

Databases on NSs. ATNF. Pulsar catalogue http://www.atnf.csiro.au/research/pulsar/psrcat/ Magnetar database in McGill http://www.physics.mcgill.ca/~pulsar/magnetar/main.html Be/X-ray binaries http://xray.sai.msu.ru/~raguzova/BeXcat/. Lecture 3 Population synthesis.

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Databases on NSs

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  1. Databases on NSs • ATNF. Pulsar catalogue http://www.atnf.csiro.au/research/pulsar/psrcat/ • Magnetar database in McGillhttp://www.physics.mcgill.ca/~pulsar/magnetar/main.html • Be/X-ray binaries • http://xray.sai.msu.ru/~raguzova/BeXcat/

  2. Lecture 3Population synthesis Sergei Popov (SAI MSU) Dubna “Dense Matter In Heavy Ion Collisions and Astrophysics”, July 2008

  3. Population synthesis in astrophysics A population synthesis is a method of a direct modeling of relatively large populations of weakly interacting objects with non-trivial evolution. As a rule, the evolution of the objects is followed from their birth up to the present moment. see astro-ph/0411792 and Physics-Uspekhi 50, 1123 (УФН 2007 г., N11; http://www.ufn.ru)

  4. Why PS is necessary? • No direct experiments computer experiments • Long evolutionary time scales • Selection effects. We see just a top of an iceberg. • Expensive projects for which it is necessary to make predictions

  5. Tasks • To test and/or to determine initial and evolutionary parameters. • To do it one has to compare calculated and observed populations. • This task is related to the main pecularity of astronomy: we cannot make direct experiments under controlled conditions. • To predict properties of unobserved populations. • Population synthesis is actively used to define programs for futureobservational projects: satellites, telescopes, etc.

  6. Two variants Evolutionary and Empirical • Evolutionary PS.The evolution is followed from some early stage. • Typically, an artificial population is formed(especially, in Monte Carlo simulations) • Empirical PS. • It is used, for example, to study integral properties(speсtra) of unresolved populations. • A library of spectra is used to predict integral properties.

  7. Examples • PS of radiopulsars • PS of gamma-ray pulsars • PS of close-by cooling NSs • PS of isolated NSs • PS of close binary systems

  8. Population synthesis of radio pulsars The idea was to make an advance population synthesis study of normalradio pulsar to reproduce the data observed in PMBPS and Swinburne. Comparison between actual data and calculations should help to understandbetter the underlying parameteres and evolution laws. Only normal (non-millisecond, non-binary, etc.) pulsars are considered. Note, however, that the role of pulsars originated in close binaries can be important. The observed PSR sample is heavily biased. It is necessary to model the process of detection,i.e. to model the same surveys in the synthetic Galaxy. A synthetic PSR is detected if it appears in thearea covered by on pf the survey, and if itsradio flux exceeds some limit. 2/3 of known PSRs were detected in PBMPSor/and SM (914 and 151). • Ingredients • Velocity distribution • Spatial distribution • Galactic model • Initial period distribution • Initial magnetic field distribution • Field evolution (and angle) • Radio luminosity • Dispersion measure model • Modeling of surveys (following Faucher-Giguere and Kaspi astro-ph/0512585)

  9. Velocity distribution Observational data for 34 PSRs. Vmax=1340 km/s (PSR B2011+38). The authors checked different velocity distributions: single maxwellian,double maxwellian, loretzian, paczynski mode, and double-side exponential.The last one was takes for the reference model. Single maxwellian was shown to be inadequate.

  10. Spatial distribution • Initial spatial ditribution of PSRs was calculated in a complicated realistic way. • exponential dependences (R and Z) were taken into account • Spiral arms were taken into account • Decrease of PSR density close to the Galactic center was used However, some details are still missing.For example, the pattern is assumed tobe stable during all time of calculations(i.e. corotating with the Sun).

  11. Galactic potential • The potential was taken from Kuijken and Gilmore (1989): • disc-halo • buldge • nuclei

  12. Initial spin periods and fields Spin periods were randomly taken from a normal distribution. Magnetic fields – also from a normal distribution for log B. The authors do not treat separately the magnetic field and inclination angle evolution. Purely magneto-dipole model with n=3 and sin χ=1 is used. RNS=106 cm, I=1045. P~(P20+K t)1/2 The death-line is taken in the usual form:

  13. [Shown to be bad] 2 Radio luminosity and beaming Model I Lto = 2 mJy kpc2α1=-19/15 α2=-2 Llow= 0.1 mJy kpc2 Model II Average beaming fraction is about 10%

  14. Optimal model and simulations The code is run till the number of “detected” synthetic PSR becomes equal tothe actual number of detected PSRs in PBMPS and SM. For each simulation the “observed” distributions of b,l, DM, S1400, P, and B,are compared with the real sample. It came out to be impossible to to apply only statistical tests.Some human judgement is necessary for interpretation.

  15. Solid lines – calculation, hatched diagrams - real observations Results

  16. Discussion of the results • No significant field decay (or change in the inclination angle) is necessary toexplain the data. • Results are not very sensitive to braking index distribution • Birthrate is 2.8+/-0.1 per century.If between 13% and 25% of core collapse SN produceBHs, thenthere is no necessity to assume a large population of radio quiet NSs.120 000 PSRs in the Galaxy

  17. Population synthesis of gamma-ray PSRs Ingredients • Geometry of radio and gamma beam • Period evolution • Magnetic field evolution • Initial spatial distribuion • Initial velocity distribution • Radio and gamma spectra • Radio and gamma luminosity • Properties of gamma detectors • Radio surveys to comapre with. Tasks • To test models • To make predictions for GLAST and AGILE (following Gonthier et al astro-ph/0312565)

  18. Beams 1. Radio beam 2. Gamma beam. Geometry of gamma-ray beam was adapted from the slot gap model (Muslimov, Harding 2003)

  19. Other properties • Pulsars are initially distributed in an exponential (in R and z) disc, following Paczynski (1990). • Birthrate is 1.38 per century • Velocity distribution from Arzoumanian, Chernoff and Cordes (2002). • Dispersion measure is calculated with the new model by Cordes and Lazio • Initial period distribution is taken to be flat from 0 to 150 ms. • Magnetic field decays with the time scale 2.8 Myrs (note, that it can be mimiced by the evolution of the inclination angle between spin and magnetic axis). The code is run till the number of detected (artificially) pulsars is 10 timeslarger than the number of really detected objects. Results are compared with nine surveys (including PMBPS)

  20. P-Pdot diagrams Detected Simulated

  21. Shaded – detected, plain - simulated

  22. Distributions on the sky

  23. Crosses – radio-quiet Dots – radio-loud Examples of pulse profiles

  24. Predictions for GLAST and AGILE

  25. Spatial distribution of gamma sources

  26. 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. To understand the origin of these populations and predict future detectionsit is necessary to use population synthesis.

  27. Population synthesis: ingredients • Birth rate of NSs • Initial spatial distribution • Spatial velocity (kick) • Mass spectrum • Thermal evolution • Interstellar absorption • Detector properties Task: To build an artificial model of a population of some astrophysical sources and to compare the results of calculations with observations.

  28. Cooling curves by • Blaschke et al. • Mass spectrum Gould Belt : 20 NS Myr-1 Gal. Disk (3kpc) : 250 NS Myr-1 ROSAT 18° Gould Belt Arzoumanian et al. 2002 Population synthesis – I.

  29. 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

  30. 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

  31. Mass spectrum of compact objects Results of numerical modeling (Timmes et al. 1996, astro-ph/9510136)

  32. Comparison with observations (Timmes et al. 1996, astro-ph/9510136)

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

  34. Progenitor mass vs. NS mass Woosley et al. 2002

  35. calculations -3/2 sphere: number ~ r3 flux ~ r-2 -1 disc: number ~ r2 flux ~ r-2 Log N – Log S Log of the number of sources brighter than the given flux Log of flux (or number counts)

  36. Cooling of NSs • Direct URCA • Modified URCA • Neutrino bremstrahlung • Superfluidity • Exotic matter (pions, quarks, hyperons, etc.) (see a recent review in astro-ph/0508056) In our study for illustrative purposes we use a set of cooling curves calculated by Blaschke, Grigorian and Voskresenski (2004) in the frame of the Nuclear medium cooling model

  37. Some results of PS-I:Log N – Log S and spatial distribution Log N – Log S for close-by ROSAT NSs can be explained by standard cooling curves taking into account the Gould Belt. Log N – Log S can be used as an additional test of cooling curves More than ½ are in +/- 12 degrees from the galactic plane. 19% outside +/- 30o 12% outside +/- 40o (Popov et al. 2005 Ap&SS 299, 117)

  38. Population synthesis – II.recent improvements 1. Spatial distribution of progenitor stars We use the same normalization for NS formation rate inside 3 kpc: 270 per Myr. Most of NSs are born inOB associations. For stars <500 pc we eventry to take into accountif they belong to OB assoc.with known age. a) Hipparcos stars up to 500 pc [Age: spectral type & cluster age (OB ass)] b) 49 OB associations: birth rate ~ Nstar c) Field stars in the disc up to 3 kpc

  39. Effects of the new spatial distribution on Log N – Log S There are no significanteffects on the Log N – Log Sdistribution due to moreclumpy initial distributionof NSs. But, as we’ll see below,the effect is strong forsky distribution. Solid – new initial XYZ Dashed – Rbelt = 500 pc Dotted – Rbelt = 300 pc

  40. Population synthesis – II.recent improvements 3. Spatial distribution of ISM (NH) instead of : NH inside 1 kpc (see astro-ph/0609275 for details) now : Modification of the old one Hakkila

  41. Popov et al. 2005 Count rate > 0.05 cts/s b= +90° Cep?Per? Sco OB Ori b= -90° PSRs+ Geminga+ M7 PSRs- First results: new maps Clearly several rich OB associations start to dominate in the spatial distribution

  42. 50 000 tracks, new ISM model Predictions for future searches Candidates: Agueros Chieregato radiopulsars Magn. 7 (Posselt et al. arXiv: 0801.4567)

  43. Standard test: temperature vs. age Kaminker et al. (2001)

  44. Log N – Log S as an additional test • Standard test: Age – Temperature • Sensitive to ages <105 years • Uncertain age and temperature • Non-uniform sample • Log N – Log S • Sensitive to ages >105 years (when applied to close-by NSs) • Definite N (number) and S (flux) • Uniform sample • Two test are perfect together!!! astro-ph/0411618

  45. Model I. Yes C A Model II. No D B Model III. Yes C B Model IV. No C B Model V. Yes D B Model VI. No E B Model VII. Yes C B’ Model VIII.Yes C B’’ Model IX. No C A Blaschke et al. used 16 sets of cooling curves. They were different in three main respects: Absence or presence of pion condensate Different gaps for superfluid protons and neutrons Different Ts-Tin List of models (Blaschke et al. 2004) Pions Crust Gaps

  46. Model I • Pions. • Gaps from Takatsuka & Tamagaki (2004) • Ts-Tin from Blaschke, Grigorian, Voskresenky (2004) Can reproduce observed Log N – Log S (astro-ph/0411618)

  47. Model II • No Pions • Gaps from Yakovlev et al. (2004), 3P2 neutron gap suppressed by 0.1 • Ts-Tin from Tsuruta (1979) Cannot reproduce observed Log N – Log S

  48. Sensitivity of Log N – Log S • Log N – Log S is very sensitive to gaps • Log N – Log S is not sensitive to the crust if it is applied to relatively old objects (>104-5 yrs) • Log N – Log S is not very sensitive to presence or absence of pions We conclude that the two test complement each other

  49. Mass constraint • Mass spectrum has to be taken • into account when discussing • data on cooling • Rare masses should not be used • to explain the cooling data • Most of data points on T-t plot • should be explained by masses • <1.4 Msun • In particular: • Vela and Geminga should not be • very massive Cooling curves from Kaminker et al. Phys. Rev .C (2006) nucl-th/0512098 (published as a JINR preprint)

  50. Another attempt to test a set of models. Hybrid stars. Astronomy meets QCD We studied several models for hybrid stars applying all possible tests: - T-t - Log N – Log S - Brightness constraint - Mass constraint We also tried to present examples when a model successfully passes the Log N – Log S test, but fails to pass the standard T-t test or fails to fulfill the mass constraint. nucl-th/0512098

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