Table 2
Exponents for the dust activity of comet 41P versus solar distance during the 2017 perihelion passage assuming different phase functions (‘linear’, ‘Schleicher et al. (1998)’, ‘Schleicher (2010)’, ‘Müller’, ‘Bowell A’, ‘Bowell B’ and ‘Rosetta’).
| 41P | afρ exponent | afρ exponent | afρ exponent | afρ exponent |
|---|---|---|---|---|
| activity | corrected for | corrected for | corrected for | corrected for |
| Nucleus brightness | No | No | Yes | Yes |
| Gas contamination | No | Yes | No | Yes |
| Linear | 6.4 ± 0.2∕0.97 | 6.7 ± 0.2∕0.97 | 6.2 ± 0.2∕0.97 | 6.4 ± 0.2∕0.97 |
| Schleicher et al. (1998) | 1.5 ± 0.3∕0.37 | 1.8 ± 0.3∕0.43 | 1.3 ± 0.3∕0.25 | 1.5 ± 0.3∕0.31 |
| Schleicher (2010) | 2.5 ± 0.2∕0.67 | 2.7 ± 0.3∕0.72 | 2.2 ± 0.3∕0.60 | 2.5 ± 0.3∕0.62 |
| Müller | 4.3 ± 0.2∕0.87 | 4.5 ± 0.2∕0.87 | 4.0 ± 0.3∕0.82 | 4.2 ± 0.3∕0.83 |
| Bowell A | 6.7 ± 0.2∕0.97 | 6.9 ± 0.2∕0.97 | 6.4 ± 0.2∕0.97 | 6.6 ± 0.2∕0.97 |
| Bowell B | 5.0 ± 0.1∕0.97 | 5.2 ± 0.1∕0.97 | 4.7 ± 0.1∕0.97 | 5.0 ± 0.1∕0.96 |
| Rosetta | 4.5 ± 0.1∕0.97 | 4.8 ± 0.1∕0.95 | 4.3 ± 0.1∕0.95 | 4.5 ± 0.1∕0.95 |
Notes. The heliocentric activity profile for an aperture diameter of 5000 km at the comet was used for the fits. The listed data represent the exponent value and its error. The third number in each cell indicates the coefficient of determination for the linear fit which compares measured and estimated afρ values (confidence values between 0 and 1). The table columns indicate whether or not corrections for the nucleus brightness and coma gas contamination are applied as described in the text.
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