Table 1.
Physical parameters of the ICM in the periphery of galaxy clusters.
| Quantity | Definition | Value |
|---|---|---|
| χ0 | Eq. (1) | 1.65 × 102 kpc2 Myr−1 |
| ωT | Eq. (8) | (600 Myr)−1 ≃ 5.3 × 10−17s−1 |
| N | Eq. (8) | ≃ωT |
| ρe | Eq. (3) | 2.73 × 10−14 kpc |
| λmfp,e | Eq. (2) | 5.83 kpc |
| lχ | Eq. (10)( ‡ ) | 320 kpc |
| H | |dlnp/dR|−1 | 300 − 600 kpc |
| cs | (γT/μmp)1/2 | 890 μ−1/2 km s−1 |
| vcond | Eq. (22)( ‡ ) | 510 km s−1 |
| vA | B/(4πρ)1/2 | 140 km s−1 |
| βe | 8πneTe/B2 | 50 |
| Kn | λmfp,e/H | 0.01 − 0.02 |
| α | Eq. (19) | 0.01 − 0.05 |
 |
Eq. (20) | 2 − 24 |
| σ | Eq. (21) | ≲1 (in MTI turbulence) |
Notes. To compute the estimates above, we assumed quasi-neutrality (ne ≃ ni) and equal temperature between ions and electrons (Te ≃ Ti ≃ T). Moreover, we took as reference parameters ne = 10−3cm−3, Te = 5 keV, B = 2 μG. For the suppression parameter α and the modified plasma beta 
, instead, we quote the realistic range of values that they could take in the periphery of galaxy clusters, as discussed in the main text. The values of ωT and N were taken from PL22a, using data from Ghirardini et al. (2019). The ( ‡ ) symbol means that the quantity has been evaluated assuming diffusivity equal to the Spitzer value. To compute H we assumed a power-law profile with slope −2 to −3 and evaluated it at R = 1 Mpc.
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