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Papers to read for exams etc.

Papers to read for exams etc. 1 . physics/0503245 Baym, Lamb "Neutron stars" 2 . astro-ph/0405262 Lattimer, Prakash "Physics of neutron stars" 3 . 0705.2708 Weber et al. "Neutron stars interiors and equation of state of superdense matter"

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Papers to read for exams etc.

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  1. Papers to read for exams etc. 1. physics/0503245 Baym, Lamb "Neutron stars" 2. astro-ph/0405262 Lattimer, Prakash "Physics of neutron stars" 3. 0705.2708 Weber et al. "Neutron stars interiors and equation of state of superdense matter" 4. 0802.2227 Reisenegger "Neutron stars and their magnetic fields« 5. astro-ph/0610593 Popov “The zoo of neutron stars” (to be continued up to 15 items....)

  2. Lecture 2. Isolated Neutron Stars. Intro. Sergei Popov (SAI MSU)

  3. Prediction ... Neutron stars have been predicted in 30s: L.D. Landau: Star-nuclei (1932) + anecdote Baade and Zwicky: neutron stars and supernovae (1934) (Landau) (Zwicky) (Baade)

  4. Some historical remarks (from a lecture by Dmitrii Yakovlev)

  5. (from lectures by D. Yakovlev) Shapiro,Teukolsky (1983)

  6. Rosenfeld L. 1974. In: Astrophysics & Gravitation, Proceeding of the 16th Solvay Conference on Physics, Brussels, Belgium, p. 174

  7. Gordon Baym (2000)

  8. Landau paper BEFORE neutron discovery Physikalische Zeitschrift der Sowjetunion Vol. 1, No. 2, 285-188, 1932 Written: Feb. 1931, Zurich Received: Jan. 7, 1932 Published: Feb. 1932

  9. S. Chandrasekhar. The maximum mass of ideal white dwarfs, ApJ 74, 81, 1931 (submitted: Nov. 12, 1930) E.C. Stoner, Phil. Mag. 9, 944, 1930 Necessary to violate quantum mechanics

  10. This is correct! Disappered in reprints,so we have difficulties

  11. Baade and Zwicky – theoretical prediction W. Baade (Mt. Wilson Observatory) F. Zwicky (Caltech) The meeting of American Physical Society (Stanford, December 15-16, 1933) Published in Physical Review (January 15, 1934)

  12. Phys. Rev. 46, 76, 1934 July 1

  13. A.G.W. Cameron, recalling his postdoc academic year 1959-1960 at Caltech reminds (Cameron, 1999): “For years Fritz [Zwicky] had been pushing his ideas about neutron stars to anyone who would listen and had been universally ignored. I believe that the part of the problem was his personality, which implied strongly that people were idiots if they did not believe in neutron stars.” Los Angeles Times January 19, 1934

  14. Good old classics For years two main types of NSs have been discussed:radio pulsars and accreting NSs in close binary systems The pulsar in the Crab nebula A binary system

  15. The old zoo of neutron stars In 60s the first X-ray sources have been discovered. They were neutron stars in close binary systems, BUT ... .... theywere «notrecognized».... Now we know hundreds of X-ray binaries with neutron stars in the Milky Way and in other galaxies.

  16. Rocket experimentsSco X-1 Giacconi, Gursky, Hendel 1962 In 2002 R.Giacconi was awarded with the Nobel prize.

  17. UHURU The satellite was launched on December 12, 1970. The program was ended in March 1973. The other nameSAS-1 2-20keV The first full sky survey. 339 sources.

  18. Accretion in close binaries Accretion is the most powerful source of energy realized in Nature, which can give a huge energy output. When matter fall down onto the surface of a neutron star up to 10% of mc2 can be released.

  19. Accretion disc The theory of accretion discs was developed in 1972-73 by N.I. Shakura and R.A. Sunyaev. Accretion is important not only in close binaries, but also in active galactic nuclei and many other types of astrophysical sources.

  20. Close binary systems About ½ of massive stars Are members of close binary systems. Now we know many dozens of close binary systems with neutron stars. • L=Mηc2 The accretion rate can be up to 1020g/s; Accretion efficiency – up to 10%; Luminosity –thousands of hundreds of the solar.

  21. Discovery !!!! 1967: JocelynBell. Radio pulsars. Seredipitous discovery.

  22. The pulsar in the Crab nebula

  23. Isolated neutron stars population: in the Galaxy and at the backyard • INSs appear in many flavours • Radio pulsars • AXPs • SGRs • CCOs • RINSs • Local population of young NSs is different (selection) • Radio pulsars • Geminga+ • RINSs

  24. The new zoo of neutron stars • During last>10 years • it became clear that neutron stars • can be born very different. • In particular, absolutely • non-similar to the Crab pulsar. • Compact central X-ray sources • in supernova remnants. • Anomalous X-ray pulsars • Soft gamma repeaters • The Magnificent Seven • Unidentified EGRET sources • Transient radio sources (RRATs) • Calvera ….

  25. Compact central X-ray sources in supernova remnants Cas A RCW 103 New result: 6.7 hour period (de Luca et al. 2006) Problem: small emitting area

  26. Puppis A One of the most famous central compact X-ray sources in supernova remnants. Age about 3700 years. Probably the progenitor was a very massive star (mass about 30 solar). • New results: • Vkick=1500 km/s • Winkler, Petre 2006 • (astro-ph/0608205)

  27. Magnetars • dE/dt > dErot/dt • By definition:The energy of the magnetic field is released • P-Pdot • Direct measurements of the field (Ibrahim et al.) Magnetic fields 1014–1015G

  28. SGRs 0526-66 1627-41 1806-20 1900+14 +candidates AXPs CXO 010043.1-72 4U 0142+61 1E 1048.1-5937 CXOU J164710.3- 1 RXS J170849-40 XTE J1810-197 1E 1841-045 AX J1844-0258 1E 2259+586 Known magnetars (СТВ 109)

  29. SGRs: monitoring and extraG SRG detectors can contribute to observations of SGRs. [D. Frederiks et al. astro-ph/0609544]

  30. Transient radio emission from AXP Radio emission was detected from XTE 1810-197during its active state. One another magnetar was reported to be detectedat low frequencies in Pushchino, however, this resulthas to be checked. (Camilo et al. astro-ph/0605429)

  31. Another AXP detected in radio 1E 1547.0-5408 P= 2 sec SNR G327.24-0.13 0802.0494

  32. Transient radiopulsar PSR J1846-0258 P=0.3 sec B=5 1013 G The pulsar increased its luminosity in X-rays. Magnetar-like X-ray bursts. 0802.1242, 0802.1704

  33. ROSAT ROentgen SATellite German satellite (with participation of US and UK). Launched 01June 1990. The program was successfully ended on 12 Feb 1999.

  34. 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

  35. Magnificent Seven Radioquiet (?) Close-by Thermal emission Absorption features Long periods

  36. Unidentified EGRET sources Grenier (2000), Gehrels et al. (2000) Unidentified sources are divided into several groups. One of them has sky distribution similar to the Gould Belt objects. It is suggested that GLAST (and, probably, AGILE) Can help to solve this problem. Actively studied subject (see for example papers byHarding, Gonthier) New results: no radio pulsars in 56 EGRET error boxes (Crawford et al. 2006)

  37. Radio pulsars Crab nebula spectrum Crab pulsar spectrum (Kuiper et al. astro-ph/0109200)

  38. Pulsars invisible in radio? (Grenier astro-ph/0011298)

  39. Binaries with radio pulsars PSR B1259-63 Cutoff at 5 Mev depends on the model of electron injection (Aharonian et al. astro-ph/0506280, see alsoKirk et al. astro-ph/9808112)

  40. Discovery of radio transients McLaughlin et al. (2006) discovered a new type of sources– RRATs (Rotating Radio Transients). For most of the sources periodsabout few seconds were discovered. The result was obtained during the Parkes survey of the Galactic plane. These sources can be related to The Magnificent seven. Thermal X-rays were observed from one of the RRATs (Reynolds et al. 2006). This one seems to me the youngest.

  41. P-Pdot diagram forRRATs McLaughlin et al. 2006Nature Estimates show that there should be about 400 000 Sources of this type in the Galaxy. Young or old??? Relatives of the Magnificent seven? (astro-ph/0603258)

  42. RRATs • 11 sources detected in the Parkes Multibeam survey (McLaughlin et al 2006) • Burst duration 2-30 ms, interval 4 min-3 hr • Periods in the range 0.4-7 s • Period derivative measured in 3 sources: B ~ 1012-1014 G, age ~ 0.1-3 Myr • RRAT J1819-1458 detected in the X-rays, spectrum soft and thermal, kT ~ 120 eV (Reynolds et al 2006)

  43. RRATs • P, B, ages and X-ray properties of RRATs very similar to those of XDINSs • Estimated number of RRATs ~ 3-5 times that of PSRs • If τRRAT ≈ τPSR, βRRAT ≈ 3-5 βPSR • βXDINS > 3 βPSR (Popov et al 2006) • Are RRATs far away XDINSs ?

  44. RRATs. Recent data X-ray pulses overlaped onradio data of RRAT J1819-1458. (arXiv: 0710.2056)

  45. Calvera et al. Recently, Rutledge et al. reported the discovery of an enigmatic NS candidated dubbed Calvera. It can be an evolved (aged) version of Cas A source, but also it can be a M7-like object, who’s progenitor was a runaway (or, less probably, hypervelocity) star. No radio emission was found.

  46. Conclusion • There are several types of sources: CCOs, M7, SGRs, AXPs, RRATs ... • Magnetars (?) • Significant fraction of all newborn NSs • Unsolved problems: 1. Are there links? 2. Reasons for diversity

  47. Main reviews • NS basics: physics/0503245 • astro-ph/0405262 • SGRs & AXPs: astro-ph/0406133 • CCOs: astro-ph/0311526 • Quark stars:astro-ph/0608360 • The Magnificent Seven: astro-ph/0502457 • astro-ph/0609066 • RRATs: astro-ph/0511587 • Cooling of NSs:astro-ph/0508056 • astro-ph/0402143 • NS structure astro-ph/0608360 • EoS astro-ph/0612440 • NS atmospheres astro-ph/0206025 • Some recent results astro-ph/0610593

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