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Heating of the ICM due to mixing of fossil plasma Matthias Hoeft Marcus Brüggen International University Bremen Gustavo

Heating of the ICM due to mixing of fossil plasma Matthias Hoeft Marcus Brüggen International University Bremen Gustavo Yepes Universidad Autonoma de Madrid. Formation of a galaxy cluster. Identifying a merger. Radio relics. Contours: X-ray Grey-scale: Radio Abell 1664 [Govoni01].

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Heating of the ICM due to mixing of fossil plasma Matthias Hoeft Marcus Brüggen International University Bremen Gustavo

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  1. Heating of the ICM due to mixing of fossil plasma Matthias Hoeft Marcus Brüggen International University Bremen Gustavo Yepes Universidad Autonoma de Madrid

  2. Formation of a galaxy cluster

  3. Identifying a merger

  4. Radio relics Contours: X-ray Grey-scale: Radio Abell 1664 [Govoni01]

  5. Model AGN fossil radio plasma relic

  6. Ghost cavities Abell 2597 [McNamara et al 01]

  7. Bubbles rise buoyantly Relic? dini = 60 kpc remission = 20 kpc Mvir = 1015 Msun Cavity AGN

  8. Rayleigh-Taylor splitting

  9. Buoyant rise with RT

  10. Volume

  11. Effervescent heating dE = pdV

  12. Total pdV-heat steeper P no splitting 1/3 volume

  13. e- momentum spectrum 300 Myr 100 Myr

  14. Bubble in shock front [Enßlin&Brüggen01]

  15. Merger of galaxie clusters

  16. Temperature

  17. Reviving fossil plasma

  18. Conclusion Bubbles of radio-plasma rise in the ICM They may deposit heat by pdV and by mixing the plasma to the ICM Heated region depends on stability of bubbles Pressure profile strongly affects the amount of heat Old plasma may be revived by compression in, e.g., merger shock fronts

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