Table 1.
Physical characteristics of the 46P nucleus (diameter D and fraction of active area fa) and meteoroid ejection parameters considered for the simulations.
| Model | Ejection model | Perihelion passages | fa | D (km) | Description |
|---|---|---|---|---|---|
| QY1 | 0.1 × W50 | 1900–2000 | Ye et al. (2016) | ||
| QY2 | 1 × W50 | 1900–2000 | |||
| QY3 | 5 × W50 | 1900–2000 | |||
| JV | CR97 | 1901– | 20% | 1.2 | Vaubaillon et al. (2005a,b) |
| AE1 | CR97 | 1830–2050 | 20% | 1.2 | Egal et al. (2019) |
| AE2 | CR97 | 1830–2050 | 40% | 1.4 | |
| DM | JB96 | 1900–2050 | 50% | 1.2 | Moser & Cooke (2004, 2008) |
| SW | fit | 1974 | Watanabe et al. (2005) | ||
Notes. (The QY models do not use this information.) Meteoroids were ejected from the nucleus within the limiting heliocentric distance rh ≤ 3 AU, with speeds following the model of CR97 (Crifo & Rodionov 1997), JB96 (Jones & Brown 1996), or W50 (Whipple 1950). The model by Watanabe et al. (2005) explores the ejection velocity needed to bring the meteoroids to Earth for a given year, so the ejection velocity is tuned for a specific prediction.
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