Cosmic rays cannot explain the high ionisation rates in the Galactic centre

Open Access

Fig. 2.

Characteristic timescales for CR energy losses in the CMZ (see Table 1 to see what parameters were adopted). Proton loss times for ionisation and p-p interactions (left panel) and electron loss times for ionisation, synchrotron, bremsstrahlung, and inverse Compton scattering (right panel).

Table 1.

Physical parameters adopted to model the CMZ.

This figure is made of several images, please see below:

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