We fit a new vertically extended corona model to previously measured reverberation time lags observed by XMM-Newton in two extremely variable Narrow Line Seyfert 1 Active Galactic Nuclei (AGN), 1H 0707-495 and IRAS 13224-3809, in a variety of similarly observed flux groups and explore the model in all observations over a 16 year period. The model employs two X-ray sources located along the black hole rotational axis at height, ℎ 1 and ℎ 2 respectively. These sources have their associated photon indices Γ 1 and Γ 2 which respond to fluctuations in the disc with a maximum response duration of 𝑡 max and a propagation delay between the response of the two of 𝑡 shift . We find that for 1H 0707-495, ℎ 2 is significantly correlated with Γ 1 and anti-correlated with ionisation 𝜉. Whilst the 1H 0707-495 corona extends upwards, the emission appears softer and the disc is less ionised. We find similarities in IRAS 13224-3809, but significant anti-correlation between Γ 2 and both 𝑡 max and 𝑡 shift . This suggests that when the IRAS 13224-3809 corona becomes softer while extending vertically upwards, the overall corona response occurs faster. This may also suggest that the inner disc also becomes more active. In addition, Γ 1 and Γ 2 are extreme, relatively less variable, but more separate in IRAS 13224-3809 than in 1H 0707-495. This suggests that the IRAS 13224-3809 corona may be more patchy in the sense that it has two more clear distinct spectral zones of Γ 1 and Γ 2 (possibly relating to two distinct zones of coronal temperature) when compared to 1H 0707-495.