How do black hole jets keep cluster cores from cooling? · revision history

Revision 2

Accepted · core change · record

Changes against revision 1:

Title
How do black hole jets keep cluster cores from cooling?
Plain
Gas at the centers of galaxy clusters radiates away its heat in less than a billion years, yet it forms stars at only a few percent of the expected rate. Jets from the central black hole carry enough energy, but how that energy spreads evenly through the gas is not known.
Precise · changed · core
Revision 1: In cool-core clusters the central gas has cooling time $t_{\mathrm{cool}}<1\ \mathrm{Gyr}$ within $\sim 100\ \mathrm{kpc}$, while star formation rates are $\sim 1\text{-}10\ \mathrm{percent}$ of classical cooling-flow rates of $10^2\text{-}10^3\ M_{\mathrm{sun}}/\mathrm{yr}$. Determine how jet mechanical power $P_{\mathrm{jet}}\sim 10^{44}\text{-}10^{46}\ \mathrm{erg/s}$ is converted to heat nearly isotropically: weak shocks, sound waves, turbulent dissipation, cosmic-ray heating, or turbulent mixing. The answer is the heating rate per channel versus radius matched to the cooling rate.
Revision 2: In cool-core clusters the central gas has cooling time $t_{\mathrm{cool}}<1\ \mathrm{Gyr}$ within $\sim 100\ \mathrm{kpc}$, while star formation rates are $\sim 1\text{-}10\%$ of classical cooling-flow rates of $10^2\text{-}10^3\ M_{\mathrm{sun}}/\mathrm{yr}$. Determine how jet mechanical power $P_{\mathrm{jet}}\sim 10^{44}\text{-}10^{46}\ \mathrm{erg/s}$ is converted to heat nearly isotropically: weak shocks, sound waves, turbulent dissipation, cosmic-ray heating, or turbulent mixing. The answer is the heating rate per channel versus radius matched to the cooling rate.
Settled by
High-resolution X-ray spectroscopy of gas velocities and temperatures in cluster cores (XRISM and successors) combined with simulations reproducing the measured velocity structure and the heating balance.
Kind
phenomenon
Answer type
mechanism
References
(empty)
Literature status
partially-resolved
Status note
Jet cavity energetics match the cooling luminosity; Hitomi in 2016 measured a line-of-sight velocity dispersion of about $1.6x10^{7}\,\mathrm{cm}/\mathrm{s}$ in the Perseus core, and XRISM has been measuring cluster core velocities since 2024.
Posed since
(empty)

Decisions