Table C.1.
Processes accounted for in this study for the CO evolution once released from the KB. We show the dominant process at the KB location in the column with an asterisk.
Processes | interactions | quantity of interest | value | * |
---|---|---|---|---|
CO | ||||
Ionization | SW protons | charge exchange cross-section (López-Patiño et al. 2017) | 1.5 × 10−15 cm2 | |
solar photons | photoionization rate (at 1 au) (Huebner et al. 1992) | 6 × 10−7 s−1 | x | |
SW e− impacts | ionization rate (Rubin et al. 2009) | 5.49 × 10−9 cm3/s | ||
Dissociation | SW protons | dissociation cross-section (López-Patiño et al. 2017) | 1.5 × 10−17 cm2 | |
solar photons | photodissociation rate (at 1 au) (Huebner & Mukherjee 2015) | 5 × 10−7 s−1 | x | |
ISM photons | photodissociation rate (Heays et al. 2017) | 2.4 × 10−10 s−1 | ||
Collisions | SW protons | radial velocity after first collision | ∼ 3 au/yr | x |
collisional frequency (at 45 au) | ∼ 2.7 yr | |||
LISM protons | radial velocity after collision | depends on vCO | ||
collisional frequency | ∼ 1.7 yr | |||
CO+ | ||||
Dissociation | solar photons | photodissociation rate (at 1 au) (Heays et al. 2017) | 5 × 10−8 s−1 | |
ISM photons | photodissociation rate (Heays et al. 2017) | 1 × 10−10 s−1 | x | |
Collisions | SW protons | radial velocity after first collision | ∼ 3 au/yr | x |
collisional frequency (at 45 au) | ∼ 24 min | |||
LISM protons | radial velocity after collision | depends on vCO+ | ||
collisional frequency | ∼ 15 min | |||
C | ||||
Ionization | solar photons | photoionization rate (at 1 au) (Huebner & Mukherjee 2015) | 4 × 10−7 s−1 | |
ISM photons | photoionization rate (Heays et al. 2017) | 3.4 × 10−10 s−1 | x | |
O | ||||
Ionization | SW protons | charge exchange cross-sectiona (Izmodenov et al. 1997) | 1.1 × 10−15 cm2 | x |
solar photons | photoionization rate (at 1 au) (Huebner & Mukherjee 2015) | 4 × 10−7 s−1 | ||
ISM photons | photoionization rate | 0 |
Notes. a We note that some extra ionization comes from electron impact ionization while crossing the heliosphere, but CO mainly photo-dissociates farther out (Izmodenov et al. 1999).
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