"how does the stability of technological civilizations affect the probability that they can be detected from Earth? "
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Dynamical Evolution of Astroid Belt and the Parent Bodies of Iron Meteorites
Project Investigators: Nader Haghighipour, Ed Scott
Summary
This project focuses on the study of the origin and mechanism of the delivery of the parent bodies of iron meteorites to the inner part of the asteroid belt. The goal of the project is to portray a comprehensive picture of the growth and scattering of meteorite parent bodies in the inner part of the solar system by studying the interactions among protoplanets and planetesimals, and the influence of a growing giant planet on the dynamics of these objects.
Astrobiology Roadmap Objectives:
Project Progress
Iron meteorites provide the best clues to the nature of the collisions among planetesimals and the initial stage of accretion and growth of small bodies. The parent bodies of these objects were traditionally assumed to have formed and differentiated in the main asteroid belt. Observational evidence, however, is in disagreement with this assumption and indicates that differentiated bodies are not currently common in that area. In an attempt to overcome these difficulties, Bottke et al (2006) suggested that the iron meteorite parent bodies probably formed inside 2 AU and were scattered into the main belt as a result of the collisions and interactions between the protoplanets in that region. The accretion and scattering of planetesimals through interactions with protoplanets must have occurred during the time that the cores of the giant planets were growing. We numerically integrated the orbits of several thousands planetesimals, protoplanets, and a proto-Jupiter to examine the effect of the growth of Jupiter on the accretion and scattering of planetesimals. Our results indicate that
1) when the mass of the giant planet’s core was smaller than 50M⊕, the perturbation of the giant planet did not play a significant role and the dynamics of planetesimals were mainly governed by their interactions with the planetary embryos.
2) The range of 50M⊕ to 100M⊕ for the core of the giant planet presents a transitional case. In this case the perturbation of the giant planet were detectable approximately 40% through the simulations.
3) When the mass of the giant planet was larger than 100M⊕, its perturbation was the dominant effect. Simulations show that in this case, the inner region of the asteroid belt is populated by planetesimals that were back-scattered from the region between 1.5 AU and 2 AU. The forward scattering of outer planetesimals into this region was insignificant.Scattering of planetary embryos. The mass of the giant planet is 50 Earth-mass. In this case, the dominant effect in scattering of protoplanets is the interactions among these objects.Scattering of planetary embryos. The mass of the giant planet is 300 Earth-mass. In this case, the dominant effect in scattering of protoplanets is their interactions with the giant planet.
Publications
Haghighipour, N. & Scott, E.R.D. (2008). Meteorite Constraints on the Early Stages of Planetary Growth in the Inner Solar System. Publications of the Lunar and Planetary Science Conference, 39:1679.
- HANDBOOK OF STAR FORMING REGIONS
- A Rare low mass quadruple spectroscopic AND eclipsing binary
- A search for Main Belt Comets in Pan-STARRS 1
- A search for primordial water from deep in the Earth's mantle
- A spectroscopically unique Main Belt asteroid: 10537 (1991 RY16)
- A Supertree Analysis of the Metazoan Phylogeny
- Acquisition and Installation of a new Cameca ims 1280 ion microprobe
- Acquisition and Installation of Witec Confocal Raman microscope scanning system
- Amorphization of Crystalline Water Ice in the Solar System
- Assessing the likelihood of supernova impact of protoplanetary disks
- Carbonate Lithologies on Devon Island, Canada
- Chemistry and biology of ultramafic-hosted alkaline springs
- Chemistry of the NH3/H2O system
- DIVERSITY AND BIOGEOGRAPHY OF THE UNIQUE TROPICAL PHYLUM PLACOZOA
- Dynamical Evolution of Astroid Belt and the Parent Bodies of Iron Meteorites
- Ecology of a Hawaiian lava cave microbial mat
- FMARS Long Duration Mission: a simulation of manned Mars exploration in an analogue environment, Devon Island, Canada
- Formation and Detection of Hot-Earth Objects in Systems with Close-in Jupiters
- Formation and the Prospects of the Detection of Habitable Planets in Extreme Planetary Systems
- Formation of Molecular Hydrogen via Interaction of Ionizing Radiation with Hydrocarbon Ices in the Interstellar Medium
- Formation of Planetesimals in a Dynamically Evolving Nebula
- FU ORIONIS ERUPTIONS
- Ice Ages on Mars
- Ice at the Mars Phoenix Landing Site
- Ice on Main Belt Comets
- Icelandic subglacial lakes
- Mechanisms of Marine Microbial Community Structuring
- Mechanistical Studies on the Non-Equilibrium Chemistry of Unusual Carbon Oxide in Solar System Ices
- Modeling grain surface reaction pathways for large organic molecules
- Molecular Deuteration on grain surfaces
- NEWBORN BINARIES
- Observations and Models of comet 17P/Holmes
- Origin and Activation Mechanism of Main Belt Comets
- Origin of Irregular Satellites
- Recovery of comet 85P/Boethin for the Deep Impact Extended Mission
- Sediment-buried basement deep biosphere
- Serpentinazation and abiogenic methane in the Mariana Forearc
- Sleeping through the Arctic Martian Sol
- Spectropolarimetric studies of stars with hot jupiters
- TES study of intracrater low albedo deposits, Amazonis Planitia, Mars
- The delivery of short-lived radionucleides to the solar system
- The effect of lunar-like satellites on the orbital infrared lightcurves of Earth-analog planets
- The Main Belt distribution of basaltic asteroids
- The Size Distribution of Small KBOs
- THE VYSOS PROJECT
- Ultra-violet processing of ices in the Rosette Nebula
- Unveiling the evolution and interplay of ice and gas in quiescent clouds
- Variable Young Stellar Objects Survey (VYSOS)
- Water on Mars
- X-ray- and UV-bright low-mass stars in the solar neighborhood