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


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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 Yepes Universidad Autonoma de Madrid

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Heating of the icm due to mixing of fossil plasma matthias hoeft marcus br ggen international university bremen gustav

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

Formation of a galaxy cluster


Identifying a merger

Identifying a merger


Radio relics

Radio relics

Contours: X-ray

Grey-scale: Radio

Abell 1664

[Govoni01]


Model

Model

AGN fossil radio plasma relic


Ghost cavities

Ghost cavities

Abell 2597

[McNamara et al 01]


Bubbles rise buoyantly

Bubbles rise buoyantly

Relic?

dini = 60 kpc

remission = 20 kpc

Mvir = 1015 Msun

Cavity

AGN


Rayleigh taylor splitting

Rayleigh-Taylor splitting


Buoyant rise with rt

Buoyant rise with RT


Volume

Volume


Effervescent heating

Effervescent heating

dE = pdV


Total pdv heat

Total pdV-heat

steeper P

no splitting

1/3 volume


E momentum spectrum

e- momentum spectrum

300 Myr

100 Myr


Bubble in shock front

Bubble in shock front

[Enßlin&Brüggen01]


Merger of galaxie clusters

Merger of galaxie clusters


Temperature

Temperature


Reviving fossil plasma

Reviving fossil plasma


Conclusion

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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