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脉冲星研究的现状与展望

脉冲星研究的现状与展望. 乔国俊 北京大学文理学院天文学系. 脉冲星研究的现状与展望. I. 简介 II. 引力波的检测 III. 新天体的搜寻 IV . 对 “ 磁星 ” 的挑战 V . 广阔的前景 、 （守时性和导航）. 近 50 年来的发现. Many discoveries over the past 50yr 脉冲星 微波背景 Cosmic Evolution Dark Matter in galaxies Quasars Jets + Superluminal motion 引力辐射间接验证 Aperture Synthesis

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脉冲星研究的现状与展望

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  1. 脉冲星研究的现状与展望 乔国俊北京大学文理学院天文学系

  2. 脉冲星研究的现状与展望 I. 简介II. 引力波的检测III. 新天体的搜寻IV.对“磁星”的挑战V. 广阔的前景、（守时性和导航）

  3. 近50年来的发现 Many discoveries over the past 50yr 脉冲星 微波背景 Cosmic Evolution Dark Matter in galaxies Quasars Jets + Superluminal motion 引力辐射间接验证 Aperture Synthesis Cosmic Masers Giant Molecular Clouds 脉冲星的发现 大约70%脉冲星是Parkes 射电望远镜发现的

  4. 脉冲辐射的产生：灯塔模型

  5. PSR 0329+54, P=0.715s PSR 0833-45, P=89 毫秒 PSR 1937+21, P=1.558 毫秒 PSR 1937+21: P=0.001,557,806,448,872,75(3)秒

  6. High B Radio Pulsars SGRs, AXPs GRB Millisecond Radio Pulsars V. Kaspi 2006

  7. Observations of gamma-ray pulsars

  8. Where we are… Pulses at 1/10th true rate

  9. Thompson, astro-ph/0312272 Abdo et al. 2010,ApJS

  10. 脉冲星研究的现状与展望 I.研究历史简介II. 引力波的检测1）间接检测2）直接检测3）作为引力波源被检测III. 新天体的搜寻IV.对“磁星”的挑战V、广阔的前景

  11. 脉冲双星B1913+16 Hulse & Taylor , 1975

  12. Taylor, J.Astrophys.Astr. 1995

  13. Post-Keplerian Timing Parameters：PSR B1913+16 Taylor, J.Astrophys.Astr.1995

  14. PSR B1913+16 Weisberg, 2005

  15. Weisberg &Taylor, 2004 astr-ph/0407149

  16. Weisberg &Taylor, 2004 astr-ph/0407149

  17. Rate of orbital period change in other gravitational theories, normalized to G.R Weisberg 2005

  18. PSR J0737-3039 Kramer et al. 2005,astr-ph/0503386

  19. PSR J0737-3039： the advantages of Double PSR Lyne 2005

  20. The future fate of B1913+16 in 50 Million Year Timesteps Now 250 M.Y. Size of Sun Weisberg 2004

  21. Double Pulsar J3037-3039

  22. 脉冲星研究的现状与展望 I.研究历史与已有成果II. 引力波的检测1）间接检测2）直接检测3）作为引力波源被检测III. 新天体的搜寻IV. 脉冲星是中子星还是夸克星？V. 脉冲星-磁星-伽玛暴

  23. Kip,S.T. 2001

  24. 大爆炸（年） 0.00001 1 100,000 1,000,000 1,000,000,000 15,000,000,000 第 一 代 恒 星 今 天 宇宙 微波 背景 辐射 黑 暗 带 元素 形成 大爆炸

  25. Direct Observations of gravitational waves (GW) GW: nanometers The Laser Interferometer Space Antenna (LISA) Base line:5 million KM, Frequency: 10－1 to 10－4HzObjects: Massive BH merging …

  26. Direct Observations of gravitational waves (GW) Laser Interferometer Gravitational-wave Observatory (LIGO) in the USA consisting of two facilities, one at Hanford (WA) and the other at Livingston (LA), hosting two 4-km and one 2-km interferometers

  27. Possible GW Possible detections of GW

  28. Gravitational wave background Pulsars=arms of huge gravitational wave detectorSearch for spatial patterns in timing residuals! Manchester & Lyne, 2003

  29. Error in Earth Velocity Manchester & Lyne, 2003 Quadrupole -Opposite sign in orthogonal directions Dipole-Opposite sign in opposite directions

  30. 脉冲星研究的现状与展望 I.研究历史与已有成果II. 引力波的检测1）间接检测2）直接检测3）作为引力波源被检测III. 新天体的搜寻IV. 脉冲星是中子星还是夸克星？V. 脉冲星-磁星-伽玛暴

  31. Neutro-star/Neutron-star Inspiral Kip,S.T. 2001

  32. Binary Black Hole Mergers Kip,S.T. 2001

  33. Rogan,et al. astro-ph/0605034 Kip S. Thorne,2001

  34. Gravitational wave background from Big Bang For example,van Straten et al. (2001) ： over 40months of observing PSR J0437-4715obtained a residual root-mean-square of only 130 nsTo be improved. ～3GHzor higherDM(dispersion measure)

  35. 脉冲星研究的现状与展望 I.研究历史与已有成果II. 引力波的检测III. 新天体的搜寻脉冲星-黑洞；亚毫秒脉冲星； IV. 脉冲星是中子星还是夸克星？V. 脉冲星-磁星-伽玛暴

  36. The BH-PSRsystem 1). Strong gravitational effects;2). Gravitational microlensing effects(Self-lensing by binary, Gould,1995)3). Effects of event horizon!4). Particle beam action with the BH

  37. Supernova Stellar mass BH: a compact object with Mass>3Msun • neutron star neutron degeneracy pressure balances gravity • Oppenheimer • black hole so massive that nothing can balance gravity  collapse to a point  singularity Mass of an invisible star > 3 M⊙: black hole ! Zhang X.N., 2005

  38. Difficulties to search for BH-PSR system Several groups have been searching for BH-PSR system, but It does not find one! ●For shout orbit period binary: it is very difficult to find it! DM, P, Tobt, e,… ●Can we find it at X-ray bands? Zhang, Qiao, Han, 1998,PABei,16,274

  39. If a pulsar: P<0.5ms?=>Quark Star! Accretion induced collapse (AIC) of WD=>0.1ms SS Du,Xu,Qiao,Han,. MN， 2009

  40. Possible test of SS and NS 1. Rotational period: SS can reach sub-millisecond2. Mass-radius.3. Solid strange star or NS?4. Binding energy of the surface. Bare strange star.Can we take a test from radiation: The difference between vacuum gap and free flow?

  41. Pulsars: Neutron or quark stars? Neutron Stars v.s. QuarkStars http://chandra.harvard.edu/photo/2002/0211/0211_illustration.pdf “To probe pulsars by GW” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

  42. Milestones in detecting PSRs faster and faster Only possible in QS model ! Spin frequency Keplerian frequency (Mass-shedding limit) Stable axis-symmetric spin (GW radiation) P = 0.89ms (2007)? XTE 1739 Sub-ms periods (P < 1 ms) P = 1.4ms (2006) P = 1.6ms (1982) PSR 1748 PSR 1937 P = 33ms (1968) P ~ 1s (1967) Crab “To probe pulsars by GW” http://vega.bac.pku.edu.cn/rxxu R. X. Xu

  43. 脉冲星研究的现状与展望 I.研究历史与已有成果II. 引力波的检测III. 新天体的搜寻IV.对“磁星”的挑战V. 广阔的情景

  44. High B Radio Pulsars 反常X射线脉冲星（AXP） & 软伽玛重复暴（SGR） SGRs, AXPs Radio Pulsars Millisecond Radio Pulsars V. Kaspi 2006

  45. Basic observations:AXP • spin periodsP: 2-- 12 s , 10 Know • Pdot≈10-13to 10-11 s/s, spinning down • Large timing noise •  Edot< LX • spin down time scales:103—105 yr •  verysoft X--ray spectra • lack of bright optical counter parts •  SNR Mereghetti, et al. astroph/0205122

  46. Basic observations:SGR • super-outbursts1044reg/s • (low-energy gamma-ray and X-ray bursts) • Observations for AXP: • spin periods P: 5-- 8 s • Pdot ≈ 10^-13 to 10-11 s/s •  Large timing noise • Edot <LX •  soft X--ray spectra •  secular spin down on time scales: 103—105 yr • lack of bright optical counter parts • SNR Mereghetti, et al. astroph/0205122 7-29-2009

  47. Models Edot < LX == • Accretion => energy • B => energy: Magnetar • Glitch NS => energy • Quark star => energy

  48. 对 magnetar 模型的挑战 • 射电脉冲星J1847-0130 ●Anti-Magnetar: PSR J1718-3718 PSR J1852+0040 B～9.4 × 10^13 G ; Lx = 5.3×10^33 erg/s B～7.4 × 10^13 GX-ray E_dot = 3.0 × 10^32 erg s^−1 Bs = 3.1×10^10 G 强磁场≠》 X-ray 辐射 辐射≠》强磁场 • Radio: XTE J1810–197 AXP 1E 1547.05408 AXP 1E2259+586, 射电 《≠》弱磁场 B～5.9 × 10^13 G

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