The Experts below are selected from a list of 113073 Experts worldwide ranked by ideXlab platform
Lijia Jiang - One of the best experts on this subject based on the ideXlab platform.
-
enhancements of high order cumulants across the 1st order phase transition boundary
Epj Web of Conferences, 2018Co-Authors: Lijia Jiang, Huichao SongAbstract:In this proceeding, we investigate the Dynamical Evolution of the σ field with a trajectory across the 1st order phase transition boundary, using the Langevin equation from the linear sigma model. We find the high order cumulants of the σ field are largely enhanced during the Dynamical Evolution, compared with the equilibrium values, due to the supercooling effect of the first order phase transition.
-
Dynamical fluctuations in critical regime and across the 1st order phase transition
Nuclear Physics, 2017Co-Authors: Lijia Jiang, Huichao SongAbstract:Abstract In this proceeding, we study the Dynamical Evolution of the sigma field within the framework of Langevin dynamics. We find that, as the system evolves in the critical regime, the magnitudes and signs of the cumulants of sigma field, C 3 and C 4 , can be dramatically different from the equilibrated ones due to the memory effects near T c . For the Dynamical Evolution across the 1st order phase transition boundary, the supercooling effect leads the sigma field to be widely distributed in the thermoDynamical potential, which largely enhances the cumulants C 3 , C 4 , correspondingly.
-
enhancements of high order cumulants across the 1st order phase transition boundary
arXiv: Nuclear Theory, 2017Co-Authors: Lijia Jiang, Huichao SongAbstract:In this proceeding, we investigate the Dynamical Evolution of the $\sigma$ field with a trajectory across the 1st order phase transition boundary, using Langevin dynamics from the linear sigma model. We find the high order cumulants of the $\sigma$ field are largely enhanced during the Dynamical Evolution, compared with the equilibrium values, due to the supercooling effect of the first order phase transition.
Konstantin Batygin - One of the best experts on this subject based on the ideXlab platform.
-
Dynamical Evolution induced by planet nine
The Astronomical Journal, 2017Co-Authors: Konstantin Batygin, Alessandro MorbidelliAbstract:The observational census of trans-Neptunian objects with semimajor axes greater than ~250 au exhibits unexpected orbital structure that is most readily attributed to gravitational perturbations induced by a yet-undetected, massive planet. Although the capacity of this planet to (i) reproduce the observed clustering of distant orbits in physical space, (ii) facilitate the Dynamical detachment of their perihelia from Neptune, and (iii) excite a population of long-period centaurs to extreme inclinations is well-established through numerical experiments, a coherent theoretical description of the Dynamical mechanisms responsible for these effects remains elusive. In this work, we characterize the Dynamical processes at play from semi-analytic grounds. We begin by considering a purely secular model of orbital Evolution induced by Planet Nine and show that it is at odds with the ensuing stability of distant objects. Instead, the long-term survival of the clustered population of long-period Kuiper Belt objects (KBOs) is enabled by a web of mean-motion resonances driven by Planet Nine. Then, by taking a compact-form approach to perturbation theory, we show that it is the secular dynamics embedded within these resonances that regulate the orbital confinement and perihelion detachment of distant KBOs. Finally, we demonstrate that the onset of large-amplitude oscillations of the orbital inclinations is accomplished through the capture of low-inclination objects into a high-order secular resonance, and we identify the specific harmonic that drives the Evolution. In light of the developed qualitative understanding of the governing dynamics, we offer an updated interpretation of the current observational data set within the broader theoretical framework of the Planet Nine hypothesis.
-
Dynamical Evolution induced by planet nine
arXiv: Earth and Planetary Astrophysics, 2017Co-Authors: Konstantin Batygin, Alessandro MorbidelliAbstract:The observational census of trans-Neptunian objects with semi-major axes greater than ~250 AU exhibits unexpected orbital structure that is most readily attributed to gravitational perturbations induced by a yet-undetected, massive planet. Although the capacity of this planet to (i) reproduce the observed clustering of distant orbits in physical space, (ii) facilitate Dynamical detachment of their perihelia from Neptune, and (iii) excite a population of long-period centaurs to extreme inclinations is well established through numerical experiments, a coherent theoretical description of the Dynamical mechanisms responsible for these effects remains elusive. In this work, we characterize the Dynamical processes at play, from semi-analytic grounds. We begin by considering a purely secular model of orbital Evolution induced by Planet Nine, and show that it is at odds with the ensuing stability of distant objects. Instead, the long-term survival of the clustered population of long-period KBOs is enabled by a web of mean-motion resonances driven by Planet Nine. Then, by taking a compact-form approach to perturbation theory, we show that it is the secular dynamics embedded within these resonances that regulates the orbital confinement and perihelion detachment of distant Kuiper belt objects. Finally, we demonstrate that the onset of large-amplitude oscillations of orbital inclinations is accomplished through capture of low-inclination objects into a high-order secular resonance and identify the specific harmonic that drives the Evolution. In light of the developed qualitative understanding of the governing dynamics, we offer an updated interpretation of the current observational dataset within the broader theoretical framework of the Planet Nine hypothesis.
-
instability driven Dynamical Evolution model of a primordially five planet outer solar system
The Astrophysical Journal, 2012Co-Authors: Konstantin Batygin, Michael E Brown, Hayden BettsAbstract:Over the last decade, evidence has mounted that the solar system's observed state can be favorably reproduced in the context of an instability-driven Dynamical Evolution model, such as the "Nice" model. To date, all successful realizations of instability models have concentrated on evolving the four giant planets onto their current orbits from a more compact configuration. Simultaneously, the possibility of forming and ejecting additional planets has been discussed, but never successfully implemented. Here we show that a large array of five-planet (two gas giants + three ice giants) multi-resonant initial states can lead to an adequate formation of the outer solar system, featuring an ejection of an ice giant during a phase of instability. Particularly, our simulations demonstrate that the eigenmodes that characterize the outer solar system's secular dynamics can be closely matched with a five-planet model. Furthermore, provided that the ejection timescale of the extra planet is short, orbital excitation of a primordial cold classical Kuiper Belt can also be avoided in this scenario. Thus, the solar system is one of many possible outcomes of Dynamical relaxation and can originate from a wide variety of initial states. This deems the construction of a unique model of solar system's early Dynamical Evolution impossible.
-
instability driven Dynamical Evolution model of a primordially 5 planet outer solar system
arXiv: Earth and Planetary Astrophysics, 2011Co-Authors: Konstantin Batygin, Michael E Brown, Hayden BettsAbstract:Over the last decade, evidence has mounted that the solar system's observed state can be favorably reproduced in the context of an instability-driven Dynamical Evolution model, such as the "Nice" model. To date, all successful realizations of instability models have concentrated on evolving the four giant planets onto their current orbits from a more compact configuration. Simultaneously, the possibility of forming and ejecting additional planets has been discussed, but never successfully implemented. Here we show that a large array of 5-planet (2 gas giants + 3 ice giants) multi-resonant initial states can lead to an adequate formation of the outer solar system, featuring an ejection of an ice giant during a phase of instability. Particularly, our simulations demonstrate that the eigenmodes which characterize the outer solar system's secular dynamics can be closely matched with a 5-planet model. Furthermore, provided that the ejection timescale of the extra planet is short, orbital excitation of a primordial cold classical Kuiper belt can also be avoided in this scenario. Thus the solar system is one of many possible outcomes of Dynamical relaxation and can originate from a wide variety of initial states. This deems the construction of a unique model of solar system's early Dynamical Evolution impossible.
-
early Dynamical Evolution of the solar system pinning down the initial conditions of the nice model
The Astrophysical Journal, 2010Co-Authors: Konstantin Batygin, Michael E BrownAbstract:In the recent years, the "Nice" model of solar system formation has attained an unprecedented level of success in reproducing much of the observed orbital architecture of the solar system by evolving the planets to their current locations from a more compact configuration. Within the context of this model, the formation of the classical Kuiper Belt requires a phase during which the ice giants have a high eccentricity. An outstanding question of this model is the initial configuration from which the solar system started out. Recent work has shown that multi-resonant initial conditions can serve as good candidates, as they naturally prevent vigorous type-II migration. In this paper, we use analytical arguments, as well as self-consistent numerical N-body simulations to identify fully resonant initial conditions, whose Dynamical Evolution is characterized by an eccentric phase of the ice giants, as well as planetary scattering. We find a total of eight such initial conditions. Four of these primordial states are compatible with the canonical "Nice" model, while the others imply slightly different Evolutions. The results presented here should prove useful in further development of a comprehensive model for solar system formation.
Huichao Song - One of the best experts on this subject based on the ideXlab platform.
-
enhancements of high order cumulants across the 1st order phase transition boundary
Epj Web of Conferences, 2018Co-Authors: Lijia Jiang, Huichao SongAbstract:In this proceeding, we investigate the Dynamical Evolution of the σ field with a trajectory across the 1st order phase transition boundary, using the Langevin equation from the linear sigma model. We find the high order cumulants of the σ field are largely enhanced during the Dynamical Evolution, compared with the equilibrium values, due to the supercooling effect of the first order phase transition.
-
Dynamical fluctuations in critical regime and across the 1st order phase transition
Nuclear Physics, 2017Co-Authors: Lijia Jiang, Huichao SongAbstract:Abstract In this proceeding, we study the Dynamical Evolution of the sigma field within the framework of Langevin dynamics. We find that, as the system evolves in the critical regime, the magnitudes and signs of the cumulants of sigma field, C 3 and C 4 , can be dramatically different from the equilibrated ones due to the memory effects near T c . For the Dynamical Evolution across the 1st order phase transition boundary, the supercooling effect leads the sigma field to be widely distributed in the thermoDynamical potential, which largely enhances the cumulants C 3 , C 4 , correspondingly.
-
enhancements of high order cumulants across the 1st order phase transition boundary
arXiv: Nuclear Theory, 2017Co-Authors: Lijia Jiang, Huichao SongAbstract:In this proceeding, we investigate the Dynamical Evolution of the $\sigma$ field with a trajectory across the 1st order phase transition boundary, using Langevin dynamics from the linear sigma model. We find the high order cumulants of the $\sigma$ field are largely enhanced during the Dynamical Evolution, compared with the equilibrium values, due to the supercooling effect of the first order phase transition.
Michael E Brown - One of the best experts on this subject based on the ideXlab platform.
-
instability driven Dynamical Evolution model of a primordially five planet outer solar system
The Astrophysical Journal, 2012Co-Authors: Konstantin Batygin, Michael E Brown, Hayden BettsAbstract:Over the last decade, evidence has mounted that the solar system's observed state can be favorably reproduced in the context of an instability-driven Dynamical Evolution model, such as the "Nice" model. To date, all successful realizations of instability models have concentrated on evolving the four giant planets onto their current orbits from a more compact configuration. Simultaneously, the possibility of forming and ejecting additional planets has been discussed, but never successfully implemented. Here we show that a large array of five-planet (two gas giants + three ice giants) multi-resonant initial states can lead to an adequate formation of the outer solar system, featuring an ejection of an ice giant during a phase of instability. Particularly, our simulations demonstrate that the eigenmodes that characterize the outer solar system's secular dynamics can be closely matched with a five-planet model. Furthermore, provided that the ejection timescale of the extra planet is short, orbital excitation of a primordial cold classical Kuiper Belt can also be avoided in this scenario. Thus, the solar system is one of many possible outcomes of Dynamical relaxation and can originate from a wide variety of initial states. This deems the construction of a unique model of solar system's early Dynamical Evolution impossible.
-
instability driven Dynamical Evolution model of a primordially 5 planet outer solar system
arXiv: Earth and Planetary Astrophysics, 2011Co-Authors: Konstantin Batygin, Michael E Brown, Hayden BettsAbstract:Over the last decade, evidence has mounted that the solar system's observed state can be favorably reproduced in the context of an instability-driven Dynamical Evolution model, such as the "Nice" model. To date, all successful realizations of instability models have concentrated on evolving the four giant planets onto their current orbits from a more compact configuration. Simultaneously, the possibility of forming and ejecting additional planets has been discussed, but never successfully implemented. Here we show that a large array of 5-planet (2 gas giants + 3 ice giants) multi-resonant initial states can lead to an adequate formation of the outer solar system, featuring an ejection of an ice giant during a phase of instability. Particularly, our simulations demonstrate that the eigenmodes which characterize the outer solar system's secular dynamics can be closely matched with a 5-planet model. Furthermore, provided that the ejection timescale of the extra planet is short, orbital excitation of a primordial cold classical Kuiper belt can also be avoided in this scenario. Thus the solar system is one of many possible outcomes of Dynamical relaxation and can originate from a wide variety of initial states. This deems the construction of a unique model of solar system's early Dynamical Evolution impossible.
-
early Dynamical Evolution of the solar system pinning down the initial conditions of the nice model
The Astrophysical Journal, 2010Co-Authors: Konstantin Batygin, Michael E BrownAbstract:In the recent years, the "Nice" model of solar system formation has attained an unprecedented level of success in reproducing much of the observed orbital architecture of the solar system by evolving the planets to their current locations from a more compact configuration. Within the context of this model, the formation of the classical Kuiper Belt requires a phase during which the ice giants have a high eccentricity. An outstanding question of this model is the initial configuration from which the solar system started out. Recent work has shown that multi-resonant initial conditions can serve as good candidates, as they naturally prevent vigorous type-II migration. In this paper, we use analytical arguments, as well as self-consistent numerical N-body simulations to identify fully resonant initial conditions, whose Dynamical Evolution is characterized by an eccentric phase of the ice giants, as well as planetary scattering. We find a total of eight such initial conditions. Four of these primordial states are compatible with the canonical "Nice" model, while the others imply slightly different Evolutions. The results presented here should prove useful in further development of a comprehensive model for solar system formation.
Giovanni Carraro - One of the best experts on this subject based on the ideXlab platform.
-
surface composition and Dynamical Evolution of two retrograde objects in the outer solar system 2008 yb3 and 2005 vd
Astronomy and Astrophysics, 2013Co-Authors: N Pinillaalonso, A Alvarezcandal, M D Melita, V Lorenzi, J Licandro, J M Carvano, D Lazzaro, Giovanni CarraroAbstract:Most of the objects in the trans-Neptunian belt (TNb) and related populations move in prograde orbits with low eccentricity and inclination. However, the list of icy minor bodies moving in orbits with an inclination above 40 has increased in recent years. The origin of these bodies, and in particular of those objects in retrograde orbits, is not well determined, and di erent scenarios are considered, depending on their inclination and perihelion. In this paper, we present new observational and Dynamical data of two objects in retrograde orbits, 2008 YB3 and 2005 VD. We find that the surface of these extreme objects is depleted of ices and does not contain the ‘ultra-red’ matter typical of some Centaurs. Despite small di erences, these objects share common colors and spectral characteristics with the Trojans, comet nuclei, and the group of grey Centaurs. All of these populations are supposed to be covered by a mantle of dust responsible for their reddish- to neutral-color. To investigate if the surface properties and Dynamical Evolution of these bodies are related, we integrate their orbits for 10 8 years to the past. We find a remarkable di erence in their Dynamical Evolutions: 2005 VD’s Evolution is dominated by a Kozai resonance with planet Jupiter while that of 2008 YB3 is dominated by close encounters with planets Jupiter and Saturn. Our models suggest that the immediate site of provenance of 2005 VD is the in the Oort cloud, whereas for 2008 YB3 it is in the trans-Neptunian region. Additionally, the study of their residence time shows that 2005 VD has spent a larger lapse of time moving in orbits in the region of the giant planets than 2008 YB3. Together with the small di erences in color between these two objects, with 2005 VD being more neutral than 2008 YB3, this fact suggests that the surface of 2005 VD has su ered a higher degree of processing, probably related to cometary activity episodes.
-
surface composition and Dynamical Evolution of two retrograde objects in the outer solar system 2008 yb3 and 2005 vd
arXiv: Earth and Planetary Astrophysics, 2013Co-Authors: N Pinillaalonso, A Alvarezcandal, M D Melita, V Lorenzi, J Licandro, J M Carvano, D Lazzaro, Giovanni CarraroAbstract:Most of the objects in the trans-Neptunian belt (TNb) and related populations move in prograde orbits with low eccentricity and inclination. However, the list of icy minor bodies moving in orbits with an inclination above 40 deg. has increased in recent years. The origin of these bodies, and in particular of those objects in retrograde orbits, is not well determined, and different scenarios are considered. In this paper, we present new observational and Dynamical data of two objects in retrograde orbits, 2008 YB3 and 2005 VD. We find that the surface of these extreme objects is depleted of ices and does not contain the 'ultra-red' matter typical of some Centaurs. Despite small differences, these objects share common colors and spectral characteristics with the Trojans, comet nuclei, and the group of grey Centaurs. All of these populations are supposed to be covered by a mantle of dust responsible for their reddish- to neutral-color. To investigate if the surface properties and Dynamical Evolution of these bodies are related, we integrate their orbits for 10^(8) years to the past. We find a remarkable difference in their Dynamical Evolutions: 2005 VD' s Evolution is dominated by a Kozai resonance with planet Jupiter while that of 2008 YB3 is dominated by close encounters with planets Jupiter and Saturn. Our models suggest that the immediate site of provenance of 2005 VD is the in the Oort cloud, whereas for 2008 YB3 it is in the trans-Neptunian region. Additionally, the study of their residence time shows that 2005 VD has spent a larger lapse of time moving in orbits in the region of the giant planets than 2008 YB3. Together with the small differences in color between these two objects, with 2005 VD being more neutral than 2008 YB3, this fact suggests that the surface of 2005 VD has suffered a higher degree of processing, probably related to cometary activity episodes.
