%0 Generic %1 obrien2014water %A O'Brien, David P. %A Walsh, Kevin J. %A Morbidelli, Alessandro %A Raymond, Sean N. %A Mandell, Avi M. %D 2014 %K 2014 a:Mandell a:Morbidelli a:OBrien a:Raymond a:Walsh dynamics grand-tack planets stability %R 10.1016/j.icarus.2014.05.009 %T Water Delivery and Giant Impacts in the 'Grand Tack' Scenario %U http://arxiv.org/abs/1407.3290 %X A new model for terrestrial planet formation (Hansen 2009, Walsh et al. 2011) has explored accretion in a truncated protoplanetary disk, and found that such a configuration is able to reproduce the distribution of mass among the planets in the Solar System, especially the Earth/Mars mass ratio, which earlier simulations have generally not been able to match. Walsh et al. tested a possible mechanism to truncate the disk--a two-stage, inward-then-outward migration of Jupiter and Saturn, as found in numerous hydrodynamical simulations of giant planet formation. In addition to truncating the disk and producing a more realistic Earth/Mars mass ratio, the migration of the giant planets also populates the asteroid belt with two distinct populations of bodies--the inner belt is filled by bodies originating inside of 3 AU, and the outer belt is filled with bodies originating from between and beyond the giant planets (which are hereafter referred to as `primitive' bodies). We find here that the planets will accrete on order 1-2% of their total mass from primitive planetesimals scattered onto planet-crossing orbits during the formation of the planets. For an assumed value of 10% for the water mass fraction of the primitive planetesimals, this model delivers a total amount of water comparable to that estimated to be on the Earth today. While the radial distribution of the planetary masses and the dynamical excitation of their orbits are a good match to the observed system, we find that the last giant impact is typically earlier than 20 Myr, and a substantial amount of mass is accreted after that event. However, 5 of the 27 planets larger than half an Earth mass formed in all simulations do experience large late impacts and subsequent accretion consistent with the dating of the Moon-forming impact and the estimated amount of mass accreted by Earth following that event.

@misc{obrien2014water, abstract = {A new model for terrestrial planet formation (Hansen 2009, Walsh et al. 2011) has explored accretion in a truncated protoplanetary disk, and found that such a configuration is able to reproduce the distribution of mass among the planets in the Solar System, especially the Earth/Mars mass ratio, which earlier simulations have generally not been able to match. Walsh et al. tested a possible mechanism to truncate the disk--a two-stage, inward-then-outward migration of Jupiter and Saturn, as found in numerous hydrodynamical simulations of giant planet formation. In addition to truncating the disk and producing a more realistic Earth/Mars mass ratio, the migration of the giant planets also populates the asteroid belt with two distinct populations of bodies--the inner belt is filled by bodies originating inside of 3 AU, and the outer belt is filled with bodies originating from between and beyond the giant planets (which are hereafter referred to as `primitive' bodies). We find here that the planets will accrete on order 1-2% of their total mass from primitive planetesimals scattered onto planet-crossing orbits during the formation of the planets. For an assumed value of 10% for the water mass fraction of the primitive planetesimals, this model delivers a total amount of water comparable to that estimated to be on the Earth today. While the radial distribution of the planetary masses and the dynamical excitation of their orbits are a good match to the observed system, we find that the last giant impact is typically earlier than 20 Myr, and a substantial amount of mass is accreted after that event. However, 5 of the 27 planets larger than half an Earth mass formed in all simulations do experience large late impacts and subsequent accretion consistent with the dating of the Moon-forming impact and the estimated amount of mass accreted by Earth following that event.}, added-at = {2014-07-15T15:44:05.000+0200}, author = {O'Brien, David P. and Walsh, Kevin J. and Morbidelli, Alessandro and Raymond, Sean N. and Mandell, Avi M.}, biburl = {https://www.bibsonomy.org/bibtex/2f256d19ded789466a260d205ed5e7043/danielcarrera}, description = {Water Delivery and Giant Impacts in the 'Grand Tack' Scenario}, doi = {10.1016/j.icarus.2014.05.009}, interhash = {accff3f3b28b3d2b54aeba4fe70dbe70}, intrahash = {f256d19ded789466a260d205ed5e7043}, keywords = {2014 a:Mandell a:Morbidelli a:OBrien a:Raymond a:Walsh dynamics grand-tack planets stability}, note = {cite arxiv:1407.3290}, timestamp = {2014-07-16T13:01:04.000+0200}, title = {Water Delivery and Giant Impacts in the 'Grand Tack' Scenario}, url = {http://arxiv.org/abs/1407.3290}, year = 2014 }