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Anti-glitch induced by collision of a solid body with the magnetar 1E 2259+586

Anti-glitch induced by collision of a solid body with the magnetar 1E 2259+586. Y. F. Huang Collaborator: J. J. Geng Nanjing University. Outline. 1. Background: glitches 2. Anti-glitch from 1E 2259+586 3. Our model: collision event 4. Discussion. 30 years timing history of PSR B1930+22.

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Anti-glitch induced by collision of a solid body with the magnetar 1E 2259+586

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  1. Anti-glitch induced by collision of a solid body with the magnetar 1E 2259+586 Y. F. Huang Collaborator: J. J. Geng Nanjing University

  2. Outline 1. Background: glitches 2. Anti-glitch from 1E 2259+586 3. Our model: collision event 4. Discussion

  3. 30 years timing history of PSR B1930+22 Espinoza et al. 2011 MNRAS

  4. 4 large glitches in the Crab pulsar Espinoza et al. 2011 MNRAS

  5. More glitches Espinoza et al. 2011 MNRAS

  6. Espinoza et al. 2011 MNRAS

  7. Glitches of Magnetars RXS J170849.0-400910 and 1E 1841-045 Dib et al. 2008, ApJ

  8. Shapiro & Teukolsky 2004

  9. Explanations for glitches The origin is still debated: • Superfluidity: interaction of quantized neutron vortex lines with the neutron-rich nuclear clusters in the inner crust (Pines & Alpar 1985; Negele & Vautherin 1973; Pizzochero 2011) • Crust-cracking events (Ruderman et al. 1998) ? http://www.eskesthai.com/search/label/Bose%20Condensate Pines & Alpar 1985

  10. Outline 1. Background: glitches 2. Anti-glitch from 1E 2259+586 3. Our model 4. Discussion

  11. The Magnetar 1E2259+586 • P=6.979 s (v = 0.143 Hz) • d = 4+/-0.8 kpc • A few history glitches observed 1E 2259+586. Credit: ESA/XMM-Newton/M. Sasaki et al.

  12. History glitches: 2002 outburst 2002 outburst On June 18 Woods et al. 2004

  13. History glitches: 9 years overview 2002 glitch Possible micro anti-glitch? Icdem et al. 2012

  14. An anti-glitch in April 2012 Archibald et al. 2013, Nat.

  15. Timing events in around April 2012 Archibald et al. 2013, Nat.

  16. + x2=45.4/44 Model 1: Model 2: x2=38.1/44 + Archibald et al. 2013, Nat.

  17. A hard X-ray burst: Exb=1.1e38 erg (36ms, Fermi/GBM,10-1000keV) An X-ray afterglow: Ex=2.1e41 erg (2-10 keV, Fx ~ t-0.38) Pulse profile: changed Foley et al. 2012 + x2=45.4/44 Model 1:

  18. Possible models for anti-glitches Internal mechanisms • Internal superfluid spins slower than the crust? (Thompson et al. 2000; Garcia & Ranea-Sandoval 2014, arXiv:1402.0848) External mechanisms • Strong outflows (Tong 2013) • Sudden twisting of magnetic fields (Lyutikov 2013) • Accretion disk of retrograde matter (Katz 2013; Ouyed et al. 2013) Cannot explain the rarity or Not a sudden glitch, cannot explain the outburst.

  19. Outline 1. Background: glitches 2. Anti-glitch from 1E 2259+586 3. Our model 4. Discussion

  20. Our model: collision of a solid body with the magnetar Huang & Geng, ApJ, 2014, 782, L20 (arXiv:1310.3324)

  21. Our model: collision of a solid body with the magnetar Huang & Geng, ApJ, 2014, 782, L20 (arXiv:1310.3324)

  22. Colgate & Petschek 1981

  23. Our model: collision process broken up distance: Collision duration: (Colgate & Petschek 1981) Huang & Geng, ApJ, 2014, 782, L20 (arXiv:1310.3324)

  24. Consistency with observations Association with an outburst Duration of the outburst (36ms) Energy release in the afterglow (2.1e41 erg) Amplitude of the anti-glitch ( ) Huang & Geng, ApJ, 2014, 782, L20 (arXiv:1310.3324) Credit: NASA http://www.futuretimeline.net/blog/2013/06/2.htm#.U9Mhi7flpQI

  25. Outline 1. Background: glitches 2. Anti-glitch from 1E 2259+586 3. Our model 4. Discussion

  26. Discussion: more collision events are possible Tremaine & Zytkow 1986, ApJ The capture radius could be as large as: 20Rns --- 80 Rns

  27. Collision possibility • Asteroids disturbed by other planets? • Oort-like cloud objects scatterd toward the NS? • Collision of planets, generating small bodies? • Neutron star escaping its original planet system? • …… • Collision rate: 1 per 5,000 --- 3e7 years for a single NS. (Mitrofanov & Sadgeev 1990)

  28. Collision-induced glitches/anti-glitches • Collision can produce either glitches or anti-glitches • They can be either radiatively active or inactive • Unlikely show any periodicity for a single NS • More likely happen in young pulsars than old ones • May have already been observed previously • A new method to probe the capture events of neutron stars. Thank You!

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