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pro vyhledávání: '"Chambers, John E."'
The inner solar system's modern orbital architecture provides inferences into the epoch of terrestrial planet formation; a ~100 Myr time period of planet growth via collisions with planetesimals and other proto-planets. While classic numerical simula
Externí odkaz:
http://arxiv.org/abs/2301.09646
In spite of substantial advancements in simulating planet formation, the planet Mercury's diminutive mass, isolated orbit, and the absence of planets with shorter orbital periods in the solar system continue to befuddle numerical accretion models. Re
Externí odkaz:
http://arxiv.org/abs/2112.00044
We introduce our new code, SMERCURY-T, which is based on existing codes SMERCURY (Lissauer et al. 2012) and Mercury-T (Bolmont et al. 2015). The result is a mixed-variable symplectic N-body integrator that can compute the orbital and spin evolution o
Externí odkaz:
http://arxiv.org/abs/2109.03347
The formation of the solar system's giant planets predated the ultimate epoch of massive impacts that concluded the process of terrestrial planet formation. Following their formation, the giant planets' orbits evolved through an episode of dynamical
Externí odkaz:
http://arxiv.org/abs/2106.05276
Autor:
Clement, Matthew S., Deienno, Rogerio, Kaib, Nathan A., Izidoro, Andre, Raymond, Sean N., Chambers, John E.
In a recent paper we proposed that the giant planets' primordial orbits may have been eccentric (~0.05), and used a suite of dynamical simulations to show outcomes of the giant planet instability that are consistent with their present-day orbits. In
Externí odkaz:
http://arxiv.org/abs/2105.10985
The absence of planets interior to Mercury continues to puzzle terrestrial planet formation models, particularly when contrasted with the relatively high derived occurrence rates of short-period planets around Sun-like stars. Recent work proposed tha
Externí odkaz:
http://arxiv.org/abs/2104.11246
Autor:
Clement, Matthew S., Chambers, John E.
Modern terrestrial planet formation models are highly successful at consistently generating planets with masses and orbits analogous to those of Earth and Venus. In stark contrast to classic theoretical predictions and inferred demographics of multi-
Externí odkaz:
http://arxiv.org/abs/2104.11252
Autor:
Clement, Mattthew S., Raymond, Sean N., Kaib, Nathan A., Deienno, Rogerio, Chambers, John E., Izidoro, Andre
An episode of dynamical instability is thought to have sculpted the orbital structure of the outer solar system. When modeling this instability, a key constraint comes from Jupiter's fifth eccentric mode (quantified by its amplitude M55), which is an
Externí odkaz:
http://arxiv.org/abs/2009.11323
The solar system's terrestrial planets are thought to have accreted over millions of years out of a sea of smaller embryos and planetesimals. Because it is impossible to know the surface density profile for solids and size frequency distribution in t
Externí odkaz:
http://arxiv.org/abs/2005.03668
Retrograde-rotating exoplanets experience obliquity excitations in an eccentricity-enabled resonance
Autor:
Kreyche, Steven M., Barnes, Jason W., Quarles, Billy L., Lissauer, Jack J., Chambers, John E., Hedman, Matthew M.
Previous studies have shown that planets that rotate retrograde (backwards with respect to their orbital motion) generally experience less severe obliquity variations than those that rotate prograde (the same direction as their orbital motion). Here
Externí odkaz:
http://arxiv.org/abs/2003.13864