Migration of Dust Particles and Delivery of Volatiles to the Terrestrial Planets

Marov, M. Ya.; Ипатов, С. И.

doi:10.1007/s11208-005-0050-1

Cited by 9 publications

(4 citation statements)

References 13 publications

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“…In different runs of calculations, the integration step was varied from 10 to 30 days and was constant in each of the runs. Earlier, we considered the evolution of orbits of more than 30000 bodies with initial orbits close to those of Jupiter-family comets (JFC), comet Halley, longperiod comets and asteroids under the 3/1 and 5/2 resonances with Jupiter, and more than 20000 dust grains produced by these small bodies (Marov and Ipatov, 2005;Ipatov and Mather, 2004Ipatov, 2010). In our previous calculations, we used the Bulirsch-Stoer algorithm (BULSTO) and the symplectic method of integration, which yielded almost the same results.…”

Section: Initial Data and Algorithms To Modelmentioning

confidence: 99%

“…The exogenous sources could originate from the migration of bodies from the outer part of the Main asteroid belt (O'Brien et al, 2014;Morbidelli et al, 2000Morbidelli et al, , 2012Petit et al, 2001;Raymond et al, 2004;Lunine et al, 2003Lunine et al, , 2007 and migration of planetesimals from beyond Jupiter's orbit (Morbidelli et al, 2000;Levison et al, 2001;Marov and Ipatov, 2001;2005;Ipatov and Mather, 2004Ipatov, 2010). For the Grand Tack model, Rubie et al (2015) considered the migration of planetesimals from a zone of 6−9.5 AU.…”

Section: Introductionmentioning

confidence: 99%

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Delivery of Water and Volatiles to the Terrestrial Planets and the Moon

Marov

Ипатов

2018

Sol Syst Res

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From modeling the evolution of disks of planetesimals under the influence of planets, it has been shown that the mass of water delivered to the Earth from beyond Jupiter's orbit could be comparable to the mass of terrestrial oceans. A considerable portion of the water could have been delivered to the Earth's embryo, when its mass was smaller than the current mass of the Earth. While the Earth's embryo mass was growing to half the current mass of the Earth, the mass of water delivered to the embryo could be near 30% of the total amount of water delivered to the Earth from the feeding zone of Jupiter and Saturn. Water of the terrestrial oceans could be a result of mixing the water from several sources with higher and lower D/H ratios. The mass of water delivered to Venus from beyond Jupiter's orbit was almost the same as that for the Earth, if normalized to unit mass of the planet. The analogous per-unit mass of water delivered to Mars was two−three times as much as that for the Earth. The mass of water delivered to the Moon from beyond Jupiter's orbit could be less than that for the Earth by a factor not more than 20.

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Section: Initial Data and Algorithms To Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Delivery of Water and Volatiles to the Terrestrial Planets and the Moon

Marov

Ипатов

2018

Sol Syst Res

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“…In other words, the volatile and moderately volatile components were deficient in the iner regions of the solar system. According to the models developed [42] [43] the bulk of Earth's ad terrestrial planets water was obtained later on through migration of volatile-rich objects (comets ad asteroids) from the outer regions of the solar system, mainly from its outskirt in the Kuiper belt, which was responsible for heterogeneous accretion of these planets mostly during period of the Late Heavy Bombardment (LHB).…”

Section: Gas-dust Protoplanetary Disc Evolutionmentioning

confidence: 99%

Gas-Dust Protoplanetary Disc: Modeling Collisional Interaction of Primordial Bodies

Marov¹,

Rusol²

2015

JMP

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One of the key problems in the concept of planetary systems origin and early evolution is solid bodies formation in the protoplanetary gas-dust disc around young stars. Dust particles interactions inside the original fluffy dust clusters of fractal nature resulted from gravitational instability and fragmentation in the disc's central plane areassumed as the most plausible mechanism of primary bodies set up owing to particles integration within the clusters. Follow upcollisions are regarded to be responsible for eventual growth of primary bodies to the size of planetesimals. We discuss this scenario including chemical nature of particles depending on the disc's radial temperature distribution and phase transitions. The mathematical model is developed based on the method of penetrating particles with the account for internal structure/properties of bodies involved, complicated patterns of their interaction, and phenomenological approach to describe energy distribution in the contact zone. The model is mainly addressed to the stage of formed solid bodies collisions. The results of numerical evaluation of the model are described involving some constraints for complete or partial destruction of colliding bodies followed by either scattering of collisional fragments orpartial back accumulation.

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“…Small bodies which collided with planets could deliver volatiles and organic/prebiotic compounds needed for life origin. Marov & Ipatov (2005) concluded that dust particles could be most efficient in the delivery of organic or even biogenic matter to the Earth, because they experience substantially weaker heating when passing through the atmosphere (an excess heat is radiated effectively due to high total surface-to-mass ratio for dust particles). They assumed that life forms drastically different from the terrestrial analogs are unlikely to be found elsewhere in the solar system (if any), e.g., either extinct or extant life on Mars.…”

Section: Delivery Of Water and Volatiles To Planetsmentioning

confidence: 99%

Migration of comets to the terrestrial planets

Ипатов

Mather²

2006

Proc. IAU

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We studied the orbital evolution of Jupiter-family comets (JFCs), Halley-type comets (HTCs), and long-period comets, and probabilities of their collisions with planets. In our runs the probability of a collision of one object with the Earth could be greater than the sum of probabilities for thousands of other objects. Even without a contribution of such a few bodies, the probability of a collision of a former JFC with the Earth was greater than 4·10 −6 . This probability is enough for delivery of all the water to Earth's oceans during formation of the giant planets. The ratios of probabilities of collisions of JFCs and HTCs with Venus and Mars to the mass of a planet usually were not smaller than that for Earth. Among 30,000 considered objects with initial orbits close to those of JFCs, a few objects got Earth-crossing orbits with semi-major axes a<2 AU and aphelion distances Q<4.2 AU, or even got inner-Earth (Q<0.983 AU), Aten, or typical asteroidal orbits, and moved in such orbits for more than 1 Myr (up to tens or even hundreds of Myrs). From a dynamical point of view, the fraction of extinct comets among near-Earth objects can exceed several tens of percent, but, probably, many extinct comets disintegrated into mini-comets and dust during a smaller part of their dynamical lifetimes if these lifetimes were large.

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Migration of Dust Particles and Delivery of Volatiles to the Terrestrial Planets

Cited by 9 publications

References 13 publications

Delivery of Water and Volatiles to the Terrestrial Planets and the Moon

Delivery of Water and Volatiles to the Terrestrial Planets and the Moon

Gas-Dust Protoplanetary Disc: Modeling Collisional Interaction of Primordial Bodies

Migration of comets to the terrestrial planets

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