Figure 7.
![The power spectrum densities of three different disc configurations with inclination i = 10°. For the case of hot disc Rhigh = 1, the stokes parameter $\mathcal {Q}$ and $\mathcal {U}$ show a peak at f = 1[1/h] while the $\mathcal {I}$ follows the red noise variability. For the case of the cold disc (Rhigh = 160), the emission is coming from the jet which has less variability. Consequentially, no variability excess is obtained in the case of jet dominated emission with non-rotating black hole (a* = 0).](https://oup.silverchair-cdn.com/oup/backfile/Content_public/Journal/mnras/531/4/10.1093_mnras_stae1343/1/stae1343fig7.jpeg?Expires=1748973678&Signature=RmkE6m61YJvHlXkybM6BX5cZFp82R91ZquMengRm0CoEBg~-~lWK~25J2g6rh90AQWFFB7jSMC~DzoVyget4qEUByKX9IdPyzJiyuQWqIOYW-0dbO0m4VANXosGV3-sFpinftPNjUREX~Uf1hOTW98IiRZgg3DJpXKevYAKhWjXf1LDV7N8VBvX81qE26SwhCmMbBy9JuUjgl3rlZl-uB59ytrAGr3Knj7ssf1ToK77txbyQzwZahWED4xoJswVsBT9ZDRjZR4JTtnRSfrQ5bmDVYDUlB8xHqhA7IPXqVIHiZRKWXwqgAKQO8Tj0rX0tWOTUxy-6yDLicRDHb8xSrw__&Key-Pair-Id=APKAIE5G5CRDK6RD3PGA)
The power spectrum densities of three different disc configurations with inclination i = 10°. For the case of hot disc Rhigh = 1, the stokes parameter |$\mathcal {Q}$| and |$\mathcal {U}$| show a peak at f = 1[1/h] while the |$\mathcal {I}$| follows the red noise variability. For the case of the cold disc (Rhigh = 160), the emission is coming from the jet which has less variability. Consequentially, no variability excess is obtained in the case of jet dominated emission with non-rotating black hole (a* = 0).
