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Table D.1.
Possible scenarios for intra-night variability and how they fit observational constraints.
| Observational fact/Possible scenario | Variability amplitude in narrow Hα > SDSS g | Similar temporal pattern | Timescale ∼1.7 h in Hα |
|---|---|---|---|
| Case (a): dominant source of narrow Hα variability is BLR; AD and NLR contributions are negligible. | 1. Contribution of AD to SDSS g is < contribution of BLR to narrow Hα (∼20%). | Coincidence of the same phase | The variability timescale ∼ outer AD size; The minimal possible AD-to-inner-BLR light travel time as a consequence of the same phase (can be N timescales bigger). |
| 2. BLR can be amplified by gravitational microlensing (Nemiroff 1988). | |||
| 3. BLR is breathing; responsivity is increasing towards bigger BLR radii (Goad & Korista 2014). | |||
| Case (b): dominant source of narrow Hα variability is AD; BLR and NLR also contribute. | 1. The difference in widths of filters (integration over wavelength means averaging amplitude over different spatial AD regions ΔRSDSSg ∼ 13 × ΔRHα) (Zdziarski 2005). | AD is dominant in both filters; delays between different parts of AD are smaller than the individual exposure time. | Light travel time between different parts of outer AD. |
| 2. Optically thin BLR on the line-of-sight, the addition of BLR and NLR variability trends on top of AD variability. | |||
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