Activity of Comets Constrains the Chemistry and Structure of the Protoplanetary Disk
Abstract
:1. Introduction
2. How Much Ice in the Outer Solar System?
3. The Structure of Nuclei of Comets
4. The WEB Activity Model
5. Nucleus Ice-Depletion Versus Erosion
- A water-rich area of and depleted of other ices, where the activity is driven by water ejecting icy dust of size , Equations (1)–(5), at the ejection rate
- A water-poor area of , where the activity is driven by CO gas diffusing among the pebbles and ejecting chunks of size , because at au, the CO sublimation front is deeper than [37]. The chunk erosion exposes anyway pebbles rich in water ice, thus the water loss rate is given by . Erosion of dust of sizes during the dehydration of the water-poor superficial pebbles is inhibited by the high values in areas, preventing any thermal equilibrium in the surface pebbles [20].
- The negligible water distributed sources observed in 67P coma [52], because most refractory mass is ejected in forms of chunks which are water-inactive at 67P perihelion and fall back on the northern nucleus hemisphere in polar winter [20,22], where water ice is again distributed uniformly inside the chunks by frosting effects [53].
- The inbound activity of the dust deposits during the northern polar summer, because chunks of become water-active at au [32].
6. The Heliocentric Dependence of the Water Loss Rate
- The steep exponential dependence on the temperature of Equation (1).
- The strong increase of the number of nucleus facets at K as decreases.
7. The Heliocentric Dependence of the Nucleus and Coma Colors
8. Water-Poor versus Water-Rich Pebbles
- All supervolatiles must sublimate at the disk water-snow line and cannot recondense on dust due to the dust temperature. This fact explains why all dm-sized chunks are water-poor and water-distributed sources in comae have sizes (Section 5).
- The amorphous water ice condensed on the dust grains in the molecular cloud becomes necessarily crystalline after condensation at the disk water-snow line, characterized by temperatures much larger than those making stable amorphous water ice [65].
9. Deuterium-To-Hydrogen Ratio in Water
10. Activity of Comets beyond Jupiter
- The dust ejection velocity from the inner coma, constraining the tail width.
- The dispersion of the lognormal distribution, constraining the tail orientation.
- The -dependence of the icy dust loss rate , constraining the tail length.
11. Outbursts
12. Conclusions
Funding
Data Availability Statement
Conflicts of Interest
References
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Kuiper Belt Object | Amorphous Ice CI-Chondritic | Crystalline Ice CI-Chondritic | Amorphous Ice Solar End-Case | Crystalline Ice Solar End-Case |
---|---|---|---|---|
Charon | 3.6 | 4.1 | 6.8 | 9.4 |
Haumea | 5.3 | 6.4 | 15.0 | 37.0 |
Pluto | 6.1 | 7.6 | 24.0 | 190.0 |
Triton | 16.0 | 30.0 | ∞ | ∞ |
Ice | |||||
---|---|---|---|---|---|
Pa | K | J kg | K | au | |
HO | 6135 | 205 | |||
CO | 3271 | 111 | 13 | ||
CH | 2520 | 89 | 18 | ||
CH | 1182 | 52 | 52 | ||
O | 998 | 44 | 60 | ||
CO | 942 | 40 | 85 |
Physical Quantity | Water-Poor Pebbles | Water-Rich Pebbles |
---|---|---|
50 | 2 | |
Water Ice | amorphous | crystalline |
Supervolatiles | rich | depleted |
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Fulle, M. Activity of Comets Constrains the Chemistry and Structure of the Protoplanetary Disk. Universe 2022, 8, 417. https://0-doi-org.brum.beds.ac.uk/10.3390/universe8080417
Fulle M. Activity of Comets Constrains the Chemistry and Structure of the Protoplanetary Disk. Universe. 2022; 8(8):417. https://0-doi-org.brum.beds.ac.uk/10.3390/universe8080417
Chicago/Turabian StyleFulle, Marco. 2022. "Activity of Comets Constrains the Chemistry and Structure of the Protoplanetary Disk" Universe 8, no. 8: 417. https://0-doi-org.brum.beds.ac.uk/10.3390/universe8080417