Effects of protoplanetary nebula on orbital dynamics of planetesimals in the outer Solar system
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F20%3A10422087" target="_blank" >RIV/00216208:11320/20:10422087 - isvavai.cz</a>
Result on the web
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=fHeTWM78w2" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=fHeTWM78w2</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1007/s10569-019-9941-1" target="_blank" >10.1007/s10569-019-9941-1</a>
Alternative languages
Result language
angličtina
Original language name
Effects of protoplanetary nebula on orbital dynamics of planetesimals in the outer Solar system
Original language description
Massive gaseous nebula has been a key element to formation of large solid objects (planetesimals, giant planet cores) in the early phase of the Solar system evolution. Here, we focus on its effects during the stagewhen giant planets have already fully formed. Dynamical effects of the nebula onmotion of planetesimals stirred by planets were twofold: (i) global gravitational acceleration, and (ii) local aerodynamic drag. Thanks to decreasing gas density with radial distance, in the outer Solar system the effect of the drag was deemed to be important only for small planetesimals (sizes 10 km). However, we find that it was possibly important up to the sizes of 100 km as well. The gravitational field of the nebula produces secular oscillations of the orbital eccentricity and inclination of planetesimals. Eventually, their pericenter may be lifted away from strong planetary influence, exhibited during close encounters, even for small bodies born in the planetary heliocentric zone. It has been previously suggested that such pathway may, in some nebula models, launch planetesimals onto large-inclination and small-eccentricity orbits in the trans-Neptunian region. These orbits would be dynamically stable to present epoch. Our simulations generally do not support such extreme cases, but we find that, after the nebula disperses, some planetesimals may indeed reach low-inclination and low-eccentricity orbits exterior to Neptune. These bodies may have been implanted into the Kuiper belt during subsequent planetesimal-driven migration of planets. This raises a possibility that some present-day KBOs may have formed in the giant-planet zone (5-20 au).
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
<a href="/en/project/GA18-06083S" target="_blank" >GA18-06083S: Evolution of solid bodies in protoplanetary disks and during collisions</a><br>
Continuities
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)
Others
Publication year
2020
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Celestial Mechanics and Dynamical Astronomy
ISSN
0923-2958
e-ISSN
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Volume of the periodical
132
Issue of the periodical within the volume
1
Country of publishing house
NL - THE KINGDOM OF THE NETHERLANDS
Number of pages
30
Pages from-to
3
UT code for WoS article
000504188100001
EID of the result in the Scopus database
2-s2.0-85076902381