Emergence of a Habitable Planet
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Timeline of Natural History
Timeline of natural history This timeline of natural history summarizes significant geological and Life timeline Ice Ages biological events from the formation of the 0 — Primates Quater nary Flowers ←Earliest apes Earth to the arrival of modern humans. P Birds h Mammals – Plants Dinosaurs Times are listed in millions of years, or Karo o a n ← Andean Tetrapoda megaanni (Ma). -50 0 — e Arthropods Molluscs r ←Cambrian explosion o ← Cryoge nian Ediacara biota – z ←Earliest animals o ←Earliest plants i Multicellular -1000 — c Contents life ←Sexual reproduction Dating of the Geologic record – P r The earliest Solar System -1500 — o t Precambrian Supereon – e r Eukaryotes Hadean Eon o -2000 — z o Archean Eon i Huron ian – c Eoarchean Era ←Oxygen crisis Paleoarchean Era -2500 — ←Atmospheric oxygen Mesoarchean Era – Photosynthesis Neoarchean Era Pong ola Proterozoic Eon -3000 — A r Paleoproterozoic Era c – h Siderian Period e a Rhyacian Period -3500 — n ←Earliest oxygen Orosirian Period Single-celled – life Statherian Period -4000 — ←Earliest life Mesoproterozoic Era H Calymmian Period a water – d e Ectasian Period a ←Earliest water Stenian Period -4500 — n ←Earth (−4540) (million years ago) Clickable Neoproterozoic Era ( Tonian Period Cryogenian Period Ediacaran Period Phanerozoic Eon Paleozoic Era Cambrian Period Ordovician Period Silurian Period Devonian Period Carboniferous Period Permian Period Mesozoic Era Triassic Period Jurassic Period Cretaceous Period Cenozoic Era Paleogene Period Neogene Period Quaternary Period Etymology of period names References See also External links Dating of the Geologic record The Geologic record is the strata (layers) of rock in the planet's crust and the science of geology is much concerned with the age and origin of all rocks to determine the history and formation of Earth and to understand the forces that have acted upon it. -
Argon Ages and Geochemistry of Lunar Breccias 67016 and 67455
Available online at www.sciencedirect.com Geochimica et Cosmochimica Acta 74 (2010) 763–783 www.elsevier.com/locate/gca Imbrium provenance for the Apollo 16 Descartes terrain: Argon ages and geochemistry of lunar breccias 67016 and 67455 M.D. Norman a,b,*, R.A. Duncan c, J.J. Huard c a Research School of Earth Sciences, Australian National University, Canberra 0200, Australia b Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston TX 77058, USA c College of Oceanic and Atmospheric Sciences, Oregon State University, Corvallis, OR 97331, USA Received 23 January 2009; accepted in revised form 16 September 2009; available online 21 October 2009 Abstract In order to improve our understanding of impact history and surface geology on the Moon, we obtained 40Ar–39Ar incre- mental heating age data and major + trace element compositions of anorthositic and melt breccia clasts from Apollo 16 feld- spathic fragmental breccias 67016 and 67455. These breccias represent the Descartes terrain, a regional unit often proposed to be ejecta from the nearby Nectaris basin. The goal of this work is to better constrain the emplacement age and provenance of the Descartes breccias. Four anorthositic clasts from 67016 yielded well-defined 40Ar–39Ar plateau ages ranging from 3842 ± 19 to 3875 ± 20 Ma. Replicate analyses of these clasts all agree within measurement error, with only slight evidence for either inheritance or youn- ger disturbance. In contrast, fragment-laden melt breccia clasts from 67016 yielded apparent plateau ages of 4.0–4.2 Ga with indications of even older material (to 4.5 Ga) in the high-T fractions. -
Astronomy 201 Review 2 Answers What Is Hydrostatic Equilibrium? How Does Hydrostatic Equilibrium Maintain the Su
Astronomy 201 Review 2 Answers What is hydrostatic equilibrium? How does hydrostatic equilibrium maintain the Sun©s stable size? Hydrostatic equilibrium, also known as gravitational equilibrium, describes a balance between gravity and pressure. Gravity works to contract while pressure works to expand. Hydrostatic equilibrium is the state where the force of gravity pulling inward is balanced by pressure pushing outward. In the core of the Sun, hydrogen is being fused into helium via nuclear fusion. This creates a large amount of energy flowing from the core which effectively creates an outward-pushing pressure. Gravity, on the other hand, is working to contract the Sun towards its center. The outward pressure of hot gas is balanced by the inward force of gravity, and not just in the core, but at every point within the Sun. What is the Sun composed of? Explain how the Sun formed from a cloud of gas. Why wasn©t the contracting cloud of gas in hydrostatic equilibrium until fusion began? The Sun is primarily composed of hydrogen (70%) and helium (28%) with the remaining mass in the form of heavier elements (2%). The Sun was formed from a collapsing cloud of interstellar gas. Gravity contracted the cloud of gas and in doing so the interior temperature of the cloud increased because the contraction converted gravitational potential energy into thermal energy (contraction leads to heating). The cloud of gas was not in hydrostatic equilibrium because although the contraction produced heat, it did not produce enough heat (pressure) to counter the gravitational collapse and the cloud continued to collapse. -
Workshop on Moon in Transition: Apollo 14, Kreep, and Evolved Lunar Rocks
WORKSHOP ON MOON IN TRANSITION: APOLLO 14, KREEP, AND EVOLVED LUNAR ROCKS (NASA-CR-I"'-- N90-I_02o rRAN31TION: APJLLN l_p KRFEP, ANu _VOLVFD LUNAR ROCKS (Lunar and Pl_net3ry !nst.) I_7 p C_CL O3B Unclas G3/91 0253133 LPI Technical Report Number 89-03 UNAR AND PLANETARY INSTITUTE 3303 NASA ROAD 1 HOUSTON, TEXAS 77058-4399 7 WORKSHOP ON MOON IN TRANSITION: APOLLO 14, KREEP, AND EVOLVED LUNAR ROCKS Edited by G. J. Taylor and P. H. Warren Sponsored by Lunar and Planetary Institute NASA Johnson Space Center November 14-16, 1988 Houston, Texas Lunar and Planetary Institute 330 ?_NASA Road 1 Houston, Texas 77058-4399 LPI Technical Report Number 89-03 Compiled in 1989 by the LUNAR AND PLANETARY INSTITUTE The Institute is operated by Universities Space Research Association under Contract NASW-4066 with the National Aeronautics and Space Administration. Material in this document may be copied without restraint for Library, abstract service, educational, or personal research purposes; however, republication of any portion requires the written permission of the authors as well as appropriate acknowledgment of this publication. This report may be cited as: Taylor G. J. and Warren PI H., eds. (1989) Workshop on Moon in Transition: Apo{l_ 14 KREEP, and Evolved Lunar Rocks. [PI Tech. Rpt. 89-03. Lunar and Planetary Institute, Houston. 156 pp. Papers in this report may be cited as: Author A. A. (1989) Title of paper. In W_nkshop on Moon in Transition: Ap_llo 14, KREEP, and Evolved Lunar Rocks (G. J. Taylor and P. H. Warren, eds.), pp. xx-yy. LPI Tech. Rpt. -
Arxiv:2007.01446V1 [Astro-Ph.EP] 3 Jul 2020 Disk
MNRAS 000,1{9 (2020) Preprint 6 July 2020 Compiled using MNRAS LATEX style file v3.0 Losing Oceans: The Effects of Composition on the Thermal Component of Impact-driven Atmospheric Loss John B. Biersteker1? and Hilke E. Schlichting1;2 1Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139-4307, USA 2UCLA, 595 Charles E. Young Drive East, Los Angeles, CA 90095, USA Accepted XXX. Received YYY; in original form ZZZ ABSTRACT The formation of the solar system's terrestrial planets concluded with a period of gi- ant impacts. Previous works examining the volatile loss caused by the impact shock in the moon-forming impact find atmospheric losses of at most 20{30 per cent and essentially no loss of oceans. However, giant impacts also result in thermal heating, which can lead to significant atmospheric escape via a Parker-type wind. Here we show that H2O and other high-mean molecular weight outgassed species can be effi- ciently lost through this thermal wind if present in a hydrogen-dominated atmosphere, substantially altering the final volatile inventory of terrestrial planets. Specifically, we demonstrate that a giant impact of a Mars-sized embryo with a proto-Earth can re- move several Earth oceans' worth of H2O, and other heavier volatile species, together with a primordial hydrogen-dominated atmosphere. These results may offer an expla- nation for the observed depletion in Earth's light noble gas budget and for its depleted xenon inventory, which suggest that Earth underwent significant atmospheric loss by the end of its accretion. Because planetary embryos are massive enough to accrete primordial hydrogen envelopes and because giant impacts are stochastic and occur concurrently with other early atmospheric evolutionary processes, our results suggest a wide diversity in terrestrial planet volatile budgets. -
Workshop on Geology of the Apollo 17 Landing Site
NASA-CR-191637 \ WORKSHOP ON GEOLOGY OF THE APOLLO 17 LANDING SITE (NASA-CR-191637) WORKSHOP ON N93-18786 GEOLOGY OF THE APOLLO 17 LANDING --THRU-- SITE (Lunar Science Inst.) 70 p N93-18817 Unclas G3/91 0141290 __ LPI Technical Report Number 92-09, Part 1 LUNAR AND PLANETARY INSTITUTE 3600 BAY AREA BOULEVARD HOUSTON TX 77058-1113 LPI/TR--92-09, Part 1 WORKSHOP ON GEOLOGY OF THE APOLLO 17 LANDING SITE Edited by G. Ryder, H. H. Schmitt, and P. D. Spudis Held at Houston, Texas December 2-4, 1992 Sponsored by Lunar and Planetary Sample Team Lunar and Planetary Institute Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPI Technical Report Number 92-09, Part 1 LPI/TR--92-09, Part 1 Compiledin 1992by LUNAR AND PLANETARY INSTITUTE TheInstituteis operatedby theUniversitySpaceResearchAssociationunderContractNo. NASW- 4574with theNationalAeronauticsandSpaceAdministration. Materialin this volume may be copied without restraint for library, abstract service, education, or per- sonal 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 Ryder G., Schmitt H. H., and Spudis P. D., eds. (1992) Workshop on Geology of the Apollo 17 Landing Site. LPI Tech. Rpt. 92-09, Part 1, Lunar and Planetary Institute, Houston. 63 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: Station 4 at Taurus-LiUrow, Apollo 17 landing site. -
HW9 (106 Points Possible)
Name: ______________________ Class: _________________ Date: _________ ID: A HW9 (106 points possible) True/False (2 points each) Indicate whether the statement is true or false. ____ 1. The atmosphere of Mars is mostly composed of carbon dioxide; therefore the greenhouse effect makes the average temperature 35 degrees warmer than it would be without its atmosphere. ____ 2. In the absence of a greenhouse effect, water on the surface of Earth would be frozen. ____ 3. Aurorae are produced only near the northern and southern magnetic poles of a planet because charged particles arriving in the solar wind cannot cross the magnetic field lines. ____ 4. Winds are generated on Earth primarily because the Sun unevenly heats our rotating planet. ____ 5. Venus’s atmospheric clouds are so thick that the surface of the planet is not seen when observing it in visible light. Multiple Choice (4 points each) Identify the choice that best completes the statement or answers the question. ____ 1. Which is NOT a reason that we suspect that the extinction of the dinosaurs was caused by a large impact by a large object? a. Many dinosaur fossils are found below the K-T boundary, but none above it. b. The material in the K-T boundary is rich in iridium. c. Soot is found in the material in the K-T boundary, which probably came from fires caused by the impact. d. An impact crater has been found near Mexico’s Yucatan Peninsula. e. The remaining meteorite has been identified on the bottom of the Gulf of Mexico. -
Horizons and OPPORTUNITIES in LUNAR SAMPLE Science
HORIZOnS and OPPORTUNITIES in LUNAR SAMPLE SCIEnCE BY LUNAR AND PLANETARY SAMPLE TEAM (LAPST) MEMBERS Luwrence A. Taylor, Chairman; University of Tennessee Ran@ Korotev; Washington University David S. McKay; Johnson Space Center Graham Wdec Lunar & Planetary Institute Paul Spudis; U.S. Geological Survey, Flagstafl G. JeJrey TqyIoc University of New Mscico David Vaniman; Los Alamos National Lab Paul Warren; University of Califbmia Los Angeles LPI TECHNICAL REPORT 85-04 Compiled in 1985by the LUNAR AND PLANETARY INSTITUTE The Institute is operated by Universities Space Research Association under Contract NASW-3389 with the National Aeronautics and Space Administration. Material in this document may be copied without restraint for library, abstract service, educational or personal research purposes; however, republication of any portion requires the written permission of the authors as well as appropriate acknowledgment of this publication. This report may be cited as: Lunar and Planetary Sample Team (LAPST) (1985) Horizons and Opportunities in Lunar Sample Science. LPI Tech. Rpt 85-04. Lunar and Planetary Institute, Houston. 44 pp. This report is distributedby LIBRARY/INFORMATION CENTER Lunar and Planetary Institute 3303 NASA Road 1 Houston, TX 77058-4399 Mail order requestors will be invoiced for the cost of postage and handling. Rontlspkce, Mission commander Llave Scott samples mare bosolt bedrock at the rim of Hadly Rille dur- ing the Apollo 15 mimion on August 3, 1971. On the boulder rests thegnoman (sun composs) and rock hammec thegouge in the boulder just below the mid-point of the rock hammer is the locotion of pxene (quartz-normative)basoll sample 155% (seen in sample bag in Scott's lep hand, at right). -
Early Earth - W
EARTH SYSTEM: HISTORY AND NATURAL VARIABILITY - Vol. I - Early Earth - W. Bleeker EARLY EARTH W. Bleeker Continental Geoscience Division, Geological Survey of Canada, Ottawa, Canada Keywords: early Earth, accretion, planetesimals, giant impacts, Moon, Hadean, Archaean, Proterozoic, late heavy bombardment, origin of life, mantle convection, mantle plumes, plate tectonics, geological time-scale, age dating Contents 1. Introduction 2. Early Earth: Concepts 2.1. Divisions of Geological Time 2.2. Definition of the“Early Earth” 2.3. Age Dating 3. Early Earth Evolution 3.1. Origin of the Universe and Formation of the Elements 3.2. Formation of the Solar System 3.3. Accretion, Differentiation, and Formation of the Earth–Moon System 3.4. Oldest Rocks and Minerals 3.5. The Close of the Hadean: the Late Heavy Bombardment 3.6. Earth’s Oldest Supracrustal Rocks and the Origin of Life 3.7. Settling into a Steady State: the Archean 4. Conclusions Acknowledgements Glossary Bibliography Biographical Sketch Summary The “ early Earth” encompasses approximately the first gigayear (Ga, 109 y) in the evolution of our planet, from its initial formation in the young Solar System at about 4.55 Ga to sometimeUNESCO in the Archean eon at about 3.5– Ga. EOLSS This chapter describes the evolution of the early Earth and reviews the evidence that pertains to this interval from both planetary and geological science perspectives. Such a description, even in general terms, can only be given with some background knowledge of the origin and calibration of the geological timescale, modernSAMPLE age-dating techniques, the foCHAPTERSrmation of solar systems, and the accretion of terrestrial planets. -
Lecture 21: Venus
Lecture 21: Venus 1 Venus Terrestrial Planets Animation Venus •The orbit of Venus is almost circular, with eccentricity e = 0.0068 •The average Sun-Venus distance is 0.72 AU (108,491,000 km) •Like Mercury, Venus always appears close to the Sun in the sky Venus 0.72 AU 47o 1 AU Sun Earth 2 Venus •Venus is visible for no more than about three hours •The Earth rotates 360o in 24 hours, or o o 360 = 15 24 hr hr •Since the maximum elongation of Venus is 47o, the maximum time for the Sun to rise after Venus is 47o ∆ t = ≈ 3 hours 15o / hr Venus •The albedo of an object is the fraction of the incident light that is reflected Albedo = 0.1 for Mercury Albedo = 0.1 for Moon Albedo = 0.4 for Earth Albedo = 0.7 for Venus •Venus is the third brightest object in the sky (Sun, Moon, Venus) •It is very bright because it is Close to the Sun Fairly large (about Earth size) Highly reflective (large albedo) Venus •Where in its orbit does Venus appears brightest as viewed from Earth? •There are two competing effects: Venus appears larger when closer The phase of Venus changes along its orbit •Maximum brightness occurs at elongation angle 39o 3 Venus •Since Venus is closer to the Sun than the Earth is, it’s apparent motion can be retrograde •Transits occur when Venus passes in front of the solar disk as viewed from Earth •This happens about once every 100 years (next one is in 2004) Venus (2 hour increments) Orbit of Venus •The semi-major axis of the orbit of Venus is a = 0.72 AU Venus Sun a •Kepler’s third law relates the semi-major axis to the orbital period -
Exoplanet Secondary Atmosphere Loss and Revival 2 3 Edwin S
1 Exoplanet secondary atmosphere loss and revival 2 3 Edwin S. Kite1 & Megan Barnett1 4 1. University of Chicago, Chicago, IL ([email protected]). 5 6 Abstract. 7 8 The next step on the path toward another Earth is to find atmospheres similar to those of 9 Earth and Venus – high-molecular-weight (secondary) atmospheres – on rocky exoplanets. 10 Many rocky exoplanets are born with thick (> 10 kbar) H2-dominated atmospheres but 11 subsequently lose their H2; this process has no known Solar System analog. We study the 12 consequences of early loss of a thick H2 atmosphere for subsequent occurrence of a high- 13 molecular-weight atmosphere using a simple model of atmosphere evolution (including 14 atmosphere loss to space, magma ocean crystallization, and volcanic outgassing). We also 15 calculate atmosphere survival for rocky worlds that start with no H2. Our results imply that 16 most rocky exoplanets interior to the Habitable Zone that were formed with thick H2- 17 dominated atmospheres lack high-molecular-weight atmospheres today. During early 18 magma ocean crystallization, high-molecular-weight species usually do not form long-lived 19 high-molecular-weight atmospheres; instead they are lost to space alongside H2. This early 20 volatile depletion makes it more difficult for later volcanic outgassing to revive the 21 atmosphere. The transition from primary to secondary atmospheres on exoplanets is 22 difficult, especially on planets orbiting M-stars. However, atmospheres should persist on 23 worlds that start with abundant volatiles (waterworlds). Our results imply that in order to 24 find high-molecular-weight atmospheres on warm exoplanets orbiting M-stars, we should 25 target worlds that formed H2-poor, that have anomalously large radii, or which orbit less 26 active stars. -
Astr150 Summer 2014 : Section Notes
UNIVERSITYOF WASHINGTON,DEPARTMENT OF ASTRONOMY AND ASTROPHYSICS Astr150 Summer 2014 : section notes Chris Suberlak July 24, 2014 1 SECTION 6: ATMOSPHERIC ESCAPE In the previous section we discussed plate tectonics, which shows how the heat from initial contraction and the ensuing heat of the radioactive decay, provide energy necessary to drive plate tectonics and volcanism. Sometimes water is not present, which results in a lack of plate tectonics, but doesn’t stop volcanism - like in a case of Venusian ’blob tectonics’. Initially a planet is formed with many gases primordially present in the Solar System, such as Hydrogen and Helium - this is called the Primary Atmosphere. Such atmosphere may be quickly lost if the v 1 v . This is true because v - the gas velocity, is linked to escape È 6 g as g as temperature, as we can equate the thermal and kinetic energies of particles: mv2 k T (1.1) b Æ 2 where kb is the Boltzmann constant, T is the temperature at that distance from the Sun, m - mass of the gas molecules, and v - velocity of gas particles. From that equation a rearrangement of variables yields: s 2kbT vg as (1.2) Æ m and if we express m in atomic mass units : 1 amu = 1.66E 27 [kg], and insert kb 1.38E 23 2 2 1 ¡ Æ ¡ [m kg s¡ K ¡ ] then the constants simplify : s T vg as 157 (1.3) Æ m which is precisely the equation used in the lab. 1 This shows us that not all bodies can hold on to all types of atmospheres: the escape velocity of the Earth is v 11200 [m/s], and so we need v (1/6)11200, thus v 1866 Ear th Æ g as Ç g as Ç [m/s].