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PWN Studies Around High Spin-Down Power Fermi-LAT Pulsars

  • Alba Fernández Barral
Chapter
Part of the Springer Theses book series (Springer Theses)

Abstract

As shown in Chap. 7, pulsars are highly magnetized rotating neutron stars born in SN explosions which are constantly releasing their rotational energy in the form of relativistic Poynting and particle flux, the so-called pulsar wind. This wind interacts with the ISM, giving rise to a termination shock in which particles are accelerated. When flowing out, the relativistic particles can in turn interact with the surrounding medium generating a magnetized bubble known as PWN. For the first thousand years, this nebula is mainly synchrotron dominated and detected between radio and X-rays.

References

  1. Abdo AA et al (2009a) Science 325:840Google Scholar
  2. Abdo AA et al (2009b) 700, L127Google Scholar
  3. Abdo AA et al (2014) Astroparticle Physics 57:16ADSCrossRefGoogle Scholar
  4. Abdo AA et al (2010) 188, 405Google Scholar
  5. Abdo AA et al (2013) 208, 17Google Scholar
  6. Aleksić J et al (2015) Journal of High Energy Astrophysics 5:30Google Scholar
  7. Aleksić J et al (2010) 725, 1629Google Scholar
  8. Aleksić J et al (2014) 567, L8Google Scholar
  9. Arumugasamy P et al (2014) 790, 103Google Scholar
  10. Arzoumanian Z et al (2011) 739, 39Google Scholar
  11. Collaboration HESS et al (2017). ArXiv e-printsGoogle Scholar
  12. Gaensler BM et al (2006) 44, 17Google Scholar
  13. Manchester RN et al (2005) 129, 1993Google Scholar
  14. Nolan PL et al (2012) 199, 31Google Scholar
  15. Pletsch HJ et al (2012) 744, 105Google Scholar
  16. Saz Parkinson PM et al (2010) 725, 571Google Scholar
  17. Tian WW et al (2006) 455, 1053Google Scholar
  18. Winkel B et al (2016) 585, A41Google Scholar

Copyright information

© Springer Nature Switzerland AG 2018

Authors and Affiliations

  1. 1.CTAO gGmbH (Headquarters)HeidelbergGermany
  2. 2.CTAO gGmbH (Local Office)BolognaItaly

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