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Table 1
Overview of luminous efficiency studies with mass range of the investigated objects, utilised data sources, and derived range of τ-values.
| Literature | Mass range | τ range | Sources |
|---|---|---|---|
| Verniani (1965) | Order of 10−2 kg | 0.02–0.2% | Harvard photographic meteor project, 413 Super-Schmidt meteors, −1 to +0.5 mag |
| Ceplecha & McCrosky (1976) | 10−1–102 kg | 0.2–2% | Photographic fireball data, 232 observations, the Prairie networks + laboratory measurements of τ + artificial meteors (Friichtenicht et al. (1968) + Ayers (1970) were taken into account) |
| Halliday et al. (1996) | 10−3–102 kg | 1–7% | 259 fireballs detected by a Canadian camera network |
| Hill et al. (2005) | 10−13–10−6 kg | 0.02–0.7% | Numerical, high-velocity meteors |
| Weryk & Brown (2013) | 10−8–10−5 kg | 0.5–6% | Canadian meteor radar system and optical video camera systems |
| Gritsevich & Koschny (2011) | 1–102 kg | 0.6–8%. | Three fireballs of the sample published by Halliday et al. (1996) |
| Nemtchinov et al. (1997) | 0.2–20 m (10–107 kg) | 5–10% (bolometric) | Light flashes detected from space by satellites’ optical sensors |
| Svetsov & Shuvalov (2019) | 0.3–3 km (1010–1013 kg) | 1–18% (bolometric) | Simulations |
| Svetsov & Shuvalov (2018) | 30 m and 100 m (107–109 kg) | 2–40% (bolometric) 1–19% (390–775 nm) | Simulations |
| Brown et al. (2013) | 19 m (106 kg) | 17% (bolometric) | Chelyabinsk meteoroid |
| Svettsov et al. (2018) | 19 m (106 kg) | 17% (bolometric) 6% (350–650 nm) | Chelyabinsk meteoroid |
| Halliday et al. (1981) | 20–40 kg | 4–8% | Innisfree meteorite fall from 1977 |
| Subasinghe & Campbell-Brown (2018) | 10−6–10−4 kg | 0.04–1% (some up to 30%) | Small, non-fragmenting and non-iron meteoroids |
| Čapek et al. (2019) | 10−6–10−3 kg | 0.08–6% | Double station video observations of faint, slow, and low-altitude meteors |
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