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Thermal / Non-thermal plasma Interactions in Clusters

Thermal / Non-thermal plasma Interactions in Clusters. The Good, the Bad & the Puzzling. L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100. The BIG Questions. • How can relativistic plasmas, seen through synchrotron radiation, reveal the dynamics and evolution of clusters?

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Thermal / Non-thermal plasma Interactions in Clusters

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  1. Thermal / Non-thermal plasmaInteractions in Clusters The Good, the Bad & the Puzzling L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100

  2. The BIG Questions • How can relativistic plasmas, seen through synchrotron radiation, reveal the dynamics and evolution of clusters? SYNCHROTRON, clues to  DYNAMICS ? • How does the dynamics of the thermal plasma affect the growth of the magnetic field and the acceleration of relativistic particles? DYNAMICS causes  B field and CRs ? L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100

  3. GOOD NEWS: хорошие новости • AGN influences on thermal X-ray plasma are well documented (heating, cavities, etc) • Shocks seen in radio, sometimes in X-ray & S-Z, are consistent with expectations from theory, connected to cluster mergers • Radio halos likely result from expected turbulence in mergers Key Messages ЮрийНикулин BAD NEWS:плохиеновости • Mach numbers expected from simulations and measured in X-ray inconsistent with spectral index of radio emission. • Missing shocks, either radio or X-ray PUZZLING NEWS: головоломки • Mild mergers with no shocks also produce giant radio halos. • 3D structure of giant shock in Abell 2256 is not simple to explain • Radio galaxies sometimes seen at edge of shocks – why? Max Otto von Stierlitz Максим Максимович Исаев L. Rudnick MN Inst. for Astrophysics Zeldovich 100 with support from U.S. NSF, AST112195

  4. The GOOD News PASSIVE ACTIVE Radio galaxy  ICM interactions L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100

  5. The GOOD News Vazza et al. 2012, MNRAS 421 1868 • Merger shocks: simulations and observed relics L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100

  6. Keeping electrons energized: CRe lifetimes ~ 108 yCRediffusion times ~ 1010 y The GOOD News Merger-driven turbulence W. Couch M. Owers L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100

  7. Halos DISTURBED The GOOD News Cassano+ 2011 • Radio halos  mergers RELAXED L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100

  8. Consistent shock story - Radio, X-ray, S-Z X-RAY A. Simionescu et al. 2013 ApJ 775 4 The GOOD News RADIO S-Z Brown & Rudnick, 2011 Planck intermediate results. X. Physics of the hot gas in the Coma cluster, 2013 L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100

  9. The BAD News Mismatched Mach numbers ? X-ray shock Ogrean+2013 ainj= -0.6 to -0.7 X-ray shock radio spectrum M < 2 3.3 < M < 4.6 van Weeren+ 12 radio spectrum

  10. The BAD News Do shocks look too efficient? Tension with g-ray limits?

  11. The BAD News X-ray shock Radio shock Why the offset? Where’s the radio shock?

  12. The PUZZLING News Exploring low surface brightness radio emission PUZZLING головоломки Farnsworth+2013 L. Rudnick, MN Inst. for Astrophysics, Zeldovich 100

  13. The PUZZLING News Can MILD mergers  Giant Radio Halos? X-Ray RADIO Rossetti+ 2013 Abell 2142 Farnsworth+ 2013

  14. The PUZZLING News Abell 2256 – where’s the shock? Radio X-ray with F. Owen, NRAO & J. Eilek, NMIMT

  15. The PUZZLING News Abell 2256 – where’s the shock? Flat spectrum Steep spectrum with F. Owen, NRAO & J. Eilek, NMIMT

  16. The PUZZLING News Radio Galaxy – relic/shock connection? van Weeren+ 2010 Bonafede+14 Pizzo+2010

  17. GOOD NEWS: хорошие новости • AGN influences on thermal X-ray plasma are well documented (heating, cavities, etc) • Shocks seen in radio, sometimes in X-ray & S-Z, are consistent with expectations from theory, connected to cluster mergers • Radio halos likely result from expected turbulence in mergers Key Messages ЮрийНикулин BAD NEWS:плохиеновости • Mach numbers expected from simulations and measured in X-ray inconsistent with spectral index of radio emission. • Missing shocks, either radio or X-ray PUZZLING NEWS: головоломки • Mild mergers with no shocks also produce giant radio halos. • 3D structure of giant shock in Abell 2256 is not simple to explain • Radio galaxies sometimes seen at edge of shocks – why? Max Otto von Stierlitz Максим Максимович Исаев L. Rudnick MN Inst. for Astrophysics Zeldovich 100 with support from U.S. NSF, AST112195

  18. radio.galaxyzoo.org

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