"THE GENERAL THEORY of META-DYNAMICS SYSTEMICITY" Part Four: Early Earth and Origin of Life’S Metadynamics Systemicity
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From: "MESSENGER, SCOTT R
The Starting Materials In: Meteorites and the Early Solar System II S. Messenger Johnson Space Center S. Sandford Ames Research Center D. Brownlee University of Washington Combined information from observations of interstellar clouds and star forming regions and studies of primitive solar system materials give a first order picture of the starting materials for the solar system’s construction. At the earliest stages, the presolar dust cloud was comprised of stardust, refractory organic matter, ices, and simple gas phase molecules. The nature of the starting materials changed dramatically together with the evolving solar system. Increasing temperatures and densities in the disk drove molecular evolution to increasingly complex organic matter. High temperature processes in the inner nebula erased most traces of presolar materials, and some fraction of this material is likely to have been transported to the outermost, quiescent portions of the disk. Interplanetary dust particles thought to be samples of Kuiper Belt objects probably contain the least altered materials, but also contain significant amounts of solar system materials processed at high temperatures. These processed materials may have been transported from the inner, warmer portions of the disk early in the active accretion phase. 1. Introduction A principal constraint on the formation of the Solar System was the population of starting materials available for its construction. Information on what these starting materials may have been is largely derived from two approaches, namely (i) the examination of other nascent stellar systems and the dense cloud environments in which they form, and (ii) the study of minimally altered examples of these starting materials that have survived in ancient Solar System materials. -
Asteroidal Dust 423
Dermott et al.: Asteroidal Dust 423 Asteroidal Dust Stanley F. Dermott University of Florida Daniel D. Durda Southwest Research Institute Keith Grogan NASA Goddard Space Flight Center Thomas J. J. Kehoe University of Florida There is good evidence that the high-speed, porous, anhydrous chondritic interplanetary dust particles (IDPs) collected in Earth’s stratosphere originated from short-period comets. How- ever, by considering the structure of the solar-system dust bands discovered by IRAS, we are able to show that asteroidal collisions are probably the dominant source of particles in the zodiacal cloud. It follows that a significant and probably the dominant fraction of the IDPs collected in Earth’s stratosphere also originated from asteroids. IDPs are the most primitive particles in the inner solar system and represent a class of material quite different from that in our meteorite collections. The structure, mineralogy, and high C content of IDPs dictate that they cannot have originated from the grinding down of known meteorite types. We argue that the asteroidal IDPs were probably formed as a result of prolonged mechanical mixing in the deep regoliths of asteroidal rubble piles in the outer main belt. 1. INTRODUCTION information on the nature of the particles in the preplanetary solar nebula (Bradley, 1999). Observations of microcraters In our collections on Earth, we have an abundance of on the Long Duration Exposure Facility (LDEF) confirmed meteorite samples from three major sources of extraterres- that each year Earth accretes 3 × 107 kg of dust particles, a trial material: the asteroid belt, the Moon, and Mars. Some mass influx ~100× greater than the influx associated with of the source bodies of these meteorites have experienced the much larger meteorites that have masses between 100 g major physical, chemical, and mineralogical changes since and 1000 kg. -
Perspective in Search of Planets and Life Around Other Stars
Proc. Natl. Acad. Sci. USA Vol. 96, pp. 5353–5355, May 1999 Perspective In search of planets and life around other stars Jonathan I. Lunine* Reparto di Planetologia, Consiglio Nazionale delle Ricerche, Istituto di Astrofisica Spaziale, Rome I-00133, Italy The discovery of over a dozen low-mass companions to nearby stars has intensified scientific and public interest in a longer term search for habitable planets like our own. However, the nature of the detected companions, and in particular whether they resemble Jupiter in properties and origin, remains undetermined. The first detection of a planet orbiting around another star like Table 1. Jovian-mass planets around main-sequence stars our Sun came in 1995, after decades of null results and false Star’s Semi-major Period, alarms. As of this writing, 18 objects have been found with masses Star mass axis, AU days Eccentricity* Mass† potentially less than 12 times that of Jupiter, but none less than 40% of Jupiter’s mass, around main-sequence stars (1) (see Table HD187123 1.00 0.042 3.097 0.03 0.57 1). In addition, several planetary-mass bodies have been detected HD75289 1.05 0.046 3.5097 0.00 0.42 orbiting pulsars. Although these are interesting as well, the exotic Tau Boo 1.20 0.047 3.3126 0.00 3.66 environments around neutron stars make it unlikely that their 51 Peg 0.98 0.051 4.2308 0.01 0.44 companions are abodes for life. It is the success in finding planets Ups And 1.10 0.054 4.62 0.15 0.61 around Sun-like stars that provides a technological stepping stone HD217107 0.96 0.072 7.11 0.14 1.28 ‡ to one of the great aspirations of humanity: to find a world like 55 Cnc 0.90 0.110 14.656 0.04 1.5–3 the Earth orbiting around a distant star. -
Urea, Glycolic Acid, and Glycerol in an Organic Residue Produced by Ultraviolet Irradiation of Interstellar=Pre-Cometary Ice Analogs
ASTROBIOLOGY Volume 10, Number 2, 2010 ª Mary Ann Liebert, Inc. DOI: 10.1089=ast.2009.0358 Urea, Glycolic Acid, and Glycerol in an Organic Residue Produced by Ultraviolet Irradiation of Interstellar=Pre-Cometary Ice Analogs Michel Nuevo,1,2 Jan Hendrik Bredeho¨ft,3 Uwe J. Meierhenrich,4 Louis d’Hendecourt,1 and Wolfram H.-P. Thiemann3 Abstract More than 50 stable organic molecules have been detected in the interstellar medium (ISM), from ground-based and onboard-satellite astronomical observations, in the gas and solid phases. Some of these organics may be prebiotic compounds that were delivered to early Earth by comets and meteorites and may have triggered the first chemical reactions involved in the origin of life. Ultraviolet irradiation of ices simulating photoprocesses of cold solid matter in astrophysical environments have shown that photochemistry can lead to the formation of amino acids and related compounds. In this work, we experimentally searched for other organic molecules of prebiotic interest, namely, oxidized acid labile compounds. In a setup that simulates conditions relevant to the ISM and Solar System icy bodies such as comets, a condensed CH3OH:NH3 ¼ 1:1 ice mixture was UV irradiated at *80 K. The molecular constituents of the nonvolatile organic residue that remained at room temperature were separated by capillary gas chromatography and identified by mass spectrometry. Urea, glycolic acid, and glycerol were detected in this residue, as well as hydroxyacetamide, glycerolic acid, and glycerol amide. These organics are interesting target molecules to be searched for in space. Finally, tentative mechanisms of formation for these compounds under interstellar=pre-cometary conditions are proposed. -
The Analysis of Interplanetary Dust Particles
WORKSHOP ON THE ANALYSIS OF INTERPLANETARY DUST PARTICLES LPI Technical Report Number 94-02 Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPIITR--94-02 WORKSHOP ON THE ANALYSIS OF INTERPLANETARY DUST PARTICLES Edited by M. Zolensky Held at Lunar and Planetary Institute May 15-17, 1993 Sponsored by Lunar and Planetary Institute Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPI Technical Report Number 94-02 LPIITR--94-02 Compiled in 1994 by LUNAR AND PLANETARY INSTITUTE The Institute is operated by the University Space Research Association under Contract No. NASW-4574 with the National Aeronautics and Space Administration. Material in this volume may be copied without restraint for library, abstract service, education, or personal research purposes; however, republication of any paper or portion thereof requires the written permission of the authors as well as the appropriate acknowledgment of this publication. This report may be cited as M. Zolensky, ed. (1994) Workshop on the Analysis ofInterplanetary Dust Particles. LPI Tech. Rpt. 94-02, Lunar and Planetary Institute, Houston. 62 pp. This report is distributed by ORDER DEPARTMENT Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Mail order requestors will be invoiced for the cost of shipping and handling. Cover. Backscattered electron image of a hydrated, chondritic interplanetary dust particle, measuring 17).1m across. LPT Technical Report 94-02 iii Program Saturday, May 15, 1993 7:30-8:30 a.m. Registration and Continental Breakfast 8:30 a.m.-5:00 p.m. INVITED PRESENTATIONS AND DISCUSSION TOPICS An Overview ofthe Origin and Role ofDust in the Early Solar System D. -
Production of Cosmic Dust by Hydrous and Anhydrous Asteroids: Implications for the Production of Interplanetary Dust Particles and Micrometeorites
40th Lunar and Planetary Science Conference (2009) 1164.pdf PRODUCTION OF COSMIC DUST BY HYDROUS AND ANHYDROUS ASTEROIDS: IMPLICATIONS FOR THE PRODUCTION OF INTERPLANETARY DUST PARTICLES AND MICROMETEORITES. G. J. Flynn 1, D. D. Durda 2, M. A. Minnick 3, and M. Strait 3. 1Dept. of Physics, SUNY-Plattsburgh, 101 Broad St., Platts- burgh, NY 12901 ([email protected]), 2Southwest Research Institute, 1050 Walnut St., Suite 300, Boul- der, CO, 80302. 3Department of Chemistry, Alma College, Alma, MI 48801 Introduction: In our Solar System the asteroid Measurements: We have performed disruption ex- belt is compositionally zoned, with the asteroids simi- periments on four hydrous meteorite targets, Murchi- lar in reflection spectrum to the carbonaceopus meteor- son and three CM2 meteorites recovered from the Ant- ites dominating the outer-half of the main belt. In the arctic. The projectiles in these experiments were 1/8 th outer-half of the main belt about one-half of the carbo- inch diameter aluminum spheres fired at the meteorite naceous asteroids are hydrous, based on their infrared targets at speeds comparable to the collision velocities spectra [1]. The asteroids in the inner-half of the main in the main-belt. belt are predominantly anhydrous. Thus, about one- Each meteorite target was surrounded by “passive quarter of the main belt asteroids are hydrous. detectors” that included three thicknesses of aluminum Because dust particles from the main-belt asteroids foil to monitor the size of the small debris from the generally encounter the Earth with lower relative ve- distrption. The foil hole diameters were measured, and locities than dust from comets [2], asteroidal dust ex- converted to impacting particle diameters using the periences much less severe atmospheric entry heating calibration data of Hörz et al. -
What Lies Immediately Outside of the Heliosphere in the Very Local Interstellar Medium (VLISM): What Will ISP Detect?
EPSC Abstracts Vol. 14, EPSC2020-68, 2020 https://doi.org/10.5194/epsc2020-68 Europlanet Science Congress 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. What lies immediately outside of the heliosphere in the very local interstellar medium (VLISM): What will ISP detect? Jeffrey Linsky1 and Seth Redfield2 1University of Colorado, JILA, Boulder CO, United States of America ([email protected]) 2Wesleyan University, Astronomy Department, Middletown CT, United States of America ([email protected]) The Interstellar Probe (ISP) will provide the first direct measurements of interstellar gas and dust when it travels far beyond the heliopause where the solar wind no longer influences the ambient medium. We summarize in this presentation what we have been learning about the VLISM from 20 years of remote observations with the high-resolution spectrographs on the Hubble Space Telescope. Radial velocity measurements of interstellar absorption lines seen in the lines of sight to nearby stars allow us to measure the kinematics of gas flows in the VLISM. We find that the heliosphere is passing through a cluster of warm partially ionized interstellar clouds. The heliosphere is now at the edge of the Local Interstellar Cloud (LIC) and heading in the direction of the slighly cooler G cloud. Two other warm clouds (Blue and Aql) are very close to the heliosphere. We find that there is a large region of the sky with very low neutral hydrogen column density, which we call the hydrogen hole. In the direction of the hydrogen hole is the brightest photoionizing source, the star Epsilon Canis Majoris (CMa). -
The Interstellar Medium
The Interstellar Medium http://apod.nasa.gov/apod/astropix.html THE INTERSTELLAR MEDIUM • Total mass ~ 5 to 10 x 109 solar masses of about 5 – 10% of the mass of the Milky Way Galaxy interior to the suns orbit • Average density overall about 0.5 atoms/cm3 or ~10-24 g cm-3, but large variations are seen • Composition - essentially the same as the surfaces of Population I stars, but the gas may be ionized, neutral, or in molecules (or dust) H I – neutral atomic hydrogen H2 - molecular hydrogen H II – ionized hydrogen He I – neutral helium Carbon, nitrogen, oxygen, dust, molecules, etc. THE INTERSTELLAR MEDIUM • Energy input – starlight (especially O and B), supernovae, cosmic rays • Cooling – line radiation and infrared radiation from dust • Largely concentrated (in our Galaxy) in the disk Evolution in the ISM of the Galaxy Stellar winds Planetary Nebulae Supernovae + Circulation Stellar burial ground The The Stars Interstellar Big Medium Galaxy Bang Formation White Dwarfs Neutron stars Black holes Star Formation As a result the ISM is continually stirred, heated, and cooled – a dynamic environment And its composition evolves: 0.02 Total fraction of heavy elements Total 10 billion Time years THE LOCAL BUBBLE http://www.daviddarling.info/encyclopedia/L/Local_Bubble.html The “Local Bubble” is a region of low density (~0.05 cm-3 and Loop I bubble high temperature (~106 K) 600 ly has been inflated by numerous supernova explosions. It is Galactic Center about 300 light years long and 300 ly peanut-shaped. Its smallest dimension is in the plane of the Milky Way Galaxy. -
Size and Scale Attendance Quiz II
Size and Scale Attendance Quiz II Are you here today? Here! (a) yes (b) no (c) are we still here? Today’s Topics • “How do we know?” exercise • Size and Scale • What is the Universe made of? • How big are these things? • How do they compare to each other? • How can we organize objects to make sense of them? What is the Universe made of? Stars • Stars make up the vast majority of the visible mass of the Universe • A star is a large, glowing ball of gas that generates heat and light through nuclear fusion • Our Sun is a star Planets • According to the IAU, a planet is an object that 1. orbits a star 2. has sufficient self-gravity to make it round 3. has a mass below the minimum mass to trigger nuclear fusion 4. has cleared the neighborhood around its orbit • A dwarf planet (such as Pluto) fulfills all these definitions except 4 • Planets shine by reflected light • Planets may be rocky, icy, or gaseous in composition. Moons, Asteroids, and Comets • Moons (or satellites) are objects that orbit a planet • An asteroid is a relatively small and rocky object that orbits a star • A comet is a relatively small and icy object that orbits a star Solar (Star) System • A solar (star) system consists of a star and all the material that orbits it, including its planets and their moons Star Clusters • Most stars are found in clusters; there are two main types • Open clusters consist of a few thousand stars and are young (1-10 million years old) • Globular clusters are denser collections of 10s-100s of thousand stars, and are older (10-14 billion years -
Arxiv:1910.06396V4 [Physics.Pop-Ph] 12 Jun 2021 ∗ Rmtv Ieeitdi H R-Oa Eua(Vni H C System)
Nebula-Relay Hypothesis: Primitive Life in Nebula and Origin of Life on Earth Lei Feng1,2, ∗ 1Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023 2Joint Center for Particle, Nuclear Physics and Cosmology, Nanjing University – Purple Mountain Observatory, Nanjing 210093, China Abstract A modified version of panspermia theory, named Nebula-Relay hypothesis or local panspermia, is introduced to explain the origin of life on Earth. Primitive life, acting as the seeds of life on Earth, originated at pre-solar epoch through physicochemical processes and then filled in the pre- solar nebula after the death of pre-solar star. Then the history of life on the Earth can be divided into three epochs: the formation of primitive life in the pre-solar epoch; pre-solar nebula epoch; the formation of solar system and the Earth age of life. The main prediction of our model is that primitive life existed in the pre-solar nebula (even in the current nebulas) and the celestial body formed therein (i.e. solar system). arXiv:1910.06396v4 [physics.pop-ph] 12 Jun 2021 ∗Electronic address: [email protected] 1 I. INTRODUCTION Generally speaking, there are several types of models to interpret the origin of life on Earth. The two most persuasive and popular models are the abiogenesis [1, 2] and pansper- mia theory [3]. The modern version of abiogenesis is also known as chemical origin theory introduced by Oparin in the 1920s [1], and Haldane proposed a similar theory independently [2] at almost the same time. In this theory, the organic compounds are naturally produced from inorganic matters through physicochemical processes and then reassembled into much more complex living creatures. -
Theoretical and Experimental Evidence for Wet Accretion of Earth
Theoretical and experimental evidence for wet accretion of Earth Krishna Muralidharan1, Abu Asaduzzaman1, Luca Vattuone2, Mario Rocca2 1 Department of Materials Science and Engineering, University of Arizona, Tucson, AZ 85721, USA 2 Dipartimento di Fisica dell’Università di Genova and IMEM-CNR Unità operativa di Genova, Via Dodecaneso 33, 16146 Genova, Italy † In memory of Prof. Michael J. Drake There has been an ongoing debate on the origin of water on Earth and other inner-solar system planets. So far, there is no consensus regarding the water-delivery mechanism(s) to the terrestrial planets. While water delivery via comets and asteroids is widely accepted, an upper limit for water delivery to Earth of about 15% is necessary, to ensure consistency with the measurements of D/H and Ar/H2O ratio in water-bearing comets. On similar lines, although asteroids are considered as a plausible source of water, the Os isotope ratio in Earth’s mantle rules out of asteroids as being the dominant source of Earth’s water. In this context, given that water and solid particulates coexisted in the accretion disk prior to planet formation, it was recently hypothesized that some of Earth’s water could be endogenous, with the delivery occurring via direct adsorption of water onto mineral surfaces. To confirm this hypothesis, we have carried out experimental and computational investigations examining water adsorption on olivine grains. The strong binding energy characterizing the adsorption process as seen by both theory and experiments unequivocally indicate that significant amounts of water can be adsorbed on to grains in the accretion disk prior to planetary accretion. -
Origin of Water Ice in the Solar System 309
Lunine: Origin of Water Ice in the Solar System 309 Origin of Water Ice in the Solar System Jonathan I. Lunine Lunar and Planetary Laboratory The origin and early distribution of water ice and more volatile compounds in the outer solar system is considered. The origin of water ice during planetary formation is at least twofold: It condenses beyond a certain distance from the proto-Sun — no more than 5 AU but perhaps as close as 2 AU — and it falls in from the surrounding molecular cloud. Because some of the infalling water ice is not sublimated in the ambient disk, complete mixing between these two sources was not achieved, and at least two populations of icy planetesimals may have been present in the protoplanetary disk. Added to this is a third reservoir of water ice planetesimals representing material chemically processed and then condensed in satellite-forming disks around giant planets. Water of hydration in silicates inward of the condensation front might be a sepa- rate source, if the hydration occurred directly from the nebular disk and not later in the parent bodies. The differences among these reservoirs of icy planetesimals ought to be reflected in diverse composition and abundance of trapped or condensed species more volatile than the water ice matrix, although radial mixing may have erased most of the differences. Possible sources of water for Earth are diverse, and include Mars-sized hydrated bodies in the asteroid belt, smaller “asteroidal” bodies, water adsorbed into dry silicate grains in the nebula, and comets. These different sources may be distinguished by their deuterium-to-hydrogen ratio, and by pre- dictions on the relative amounts of water (and isotopic compositional differences) between Earth and Mars.