A Sound Nebula: the Origin of the Solar System in the Field of a Standing
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Lecture 3 - Minimum Mass Model of Solar Nebula
Lecture 3 - Minimum mass model of solar nebula o Topics to be covered: o Composition and condensation o Surface density profile o Minimum mass of solar nebula PY4A01 Solar System Science Minimum Mass Solar Nebula (MMSN) o MMSN is not a nebula, but a protoplanetary disc. Protoplanetary disk Nebula o Gives minimum mass of solid material to build the 8 planets. PY4A01 Solar System Science Minimum mass of the solar nebula o Can make approximation of minimum amount of solar nebula material that must have been present to form planets. Know: 1. Current masses, composition, location and radii of the planets. 2. Cosmic elemental abundances. 3. Condensation temperatures of material. o Given % of material that condenses, can calculate minimum mass of original nebula from which the planets formed. • Figure from Page 115 of “Physics & Chemistry of the Solar System” by Lewis o Steps 1-8: metals & rock, steps 9-13: ices PY4A01 Solar System Science Nebula composition o Assume solar/cosmic abundances: Representative Main nebular Fraction of elements Low-T material nebular mass H, He Gas 98.4 % H2, He C, N, O Volatiles (ices) 1.2 % H2O, CH4, NH3 Si, Mg, Fe Refractories 0.3 % (metals, silicates) PY4A01 Solar System Science Minimum mass for terrestrial planets o Mercury:~5.43 g cm-3 => complete condensation of Fe (~0.285% Mnebula). 0.285% Mnebula = 100 % Mmercury => Mnebula = (100/ 0.285) Mmercury = 350 Mmercury o Venus: ~5.24 g cm-3 => condensation from Fe and silicates (~0.37% Mnebula). =>(100% / 0.37% ) Mvenus = 270 Mvenus o Earth/Mars: 0.43% of material condensed at cooler temperatures. -
Planet Formation
3. Planet form ation Frontiers of A stronom y W orkshop/S chool Bibliotheca A lexandrina M arch-A pril 2006 Properties of planetary system s • all giant planets in the solar system have a > 5 A U w hile extrasolar giant planets have semi-major axes as small as a = 0.02 A U • planetary orbital angular momentum is close to direction of S un’s spin angular momentum (w ithin 7o) • 3 of 4 terrestrial planets and 3 of 4 giant planets have obliquities (angle betw een spin and orbital angular momentum) < 30o • interplanetary space is virtually empty, except for the asteroid belt and the Kuiper belt • planets account for < 0.2% of mass of solar system but > 98% of angular momentum Properties of planetary system s • orbits of major planets in solar system are nearly circular (eMercury=0.206, ePluto=0.250); orbits of extrasolar planets are not (emedian=0.28) • probability of finding a planet is proportional to mass of metals in the star Properties of planetary system s • planets suffer no close encounters and are spaced fairly n regularly (Bode’s law : an=0.4 + 0.3×2 ) planet semimajor axis (A U ) n an (A U ) Mercury 0.39 −∞ 0.4 V enus 0.72 0 0.7 Earth 1.00 1 1.0 Mars 1.52 2 1.6 asteroids 2.77 (Ceres) 3 2.8 Jupiter 5.20 4 5.2 S aturn 9.56 5 10.0 U ranus 19.29 6 19.6 N eptune 30.27 7 38.8 Pluto 39.68 8 77.2 Properties of planetary system s • planets suffer no close encounters and are spaced fairly n regularly (Bode’s law : an=0.4 + 0.3×2 ) planet semimajor axis (A U ) n an (A U ) Mercury+ 0.39 −∞ 0.4 V enus 0.72 0 0.7 Earth 1.00 1 1.0 *predicted -
Planets of the Solar System
Chapter Planets of the 27 Solar System Chapter OutlineOutline 1 ● Formation of the Solar System The Nebular Hypothesis Formation of the Planets Formation of Solid Earth Formation of Earth’s Atmosphere Formation of Earth’s Oceans 2 ● Models of the Solar System Early Models Kepler’s Laws Newton’s Explanation of Kepler’s Laws 3 ● The Inner Planets Mercury Venus Earth Mars 4 ● The Outer Planets Gas Giants Jupiter Saturn Uranus Neptune Objects Beyond Neptune Why It Matters Exoplanets UnderstandingU d t di theth formationf ti and the characteristics of our solar system and its planets can help scientists plan missions to study planets and solar systems around other stars in the universe. 746 Chapter 27 hhq10sena_psscho.inddq10sena_psscho.indd 774646 PDF 88/15/08/15/08 88:43:46:43:46 AAMM Inquiry Lab Planetary Distances 20 min Turn to Appendix E and find the table entitled Question to Get You Started “Solar System Data.” Use the data from the How would the distance of a planet from the sun “semimajor axis” row of planetary distances to affect the time it takes for the planet to complete devise an appropriate scale to model the distances one orbit? between planets. Then find an indoor or outdoor space that will accommodate the farthest distance. Mark some index cards with the name of each planet, use a measuring tape to measure the distances according to your scale, and place each index card at its correct location. 747 hhq10sena_psscho.inddq10sena_psscho.indd 774747 22/26/09/26/09 111:42:301:42:30 AAMM These reading tools will help you learn the material in this chapter. -
Meteorites and the Origin of the Solar System
Meteorites and the origin of the solar system STEPHEN G. BRUSH University of Maryland, College Park, MD 20742, USA (e-mail: [email protected]) Abstract: During the past two centuries, theories of the origin of the solar system have been strongly influenced by observations and theories about meteorites. I review this history up to about 1985. During the 19th century the hypothesis that planets formed by accretion of small solid particles ('the meteoritic hypothesis') competed with the alternative 'nebular hypothesis' of Laplace, based on condensation from a hot gas. At the beginning of the 20th century Chamberlin and Moulton revived the meteoritic hypothesis as the 'planetesimal hypothesis' and joined it to the assumption that the solar system evolved from the encounter of the Sun with a passing star. Later, the encounter hypothesis was rejected and the planetesimal hypothesis was incorporated into new versions of the nebular hypothesis. In the 1950s, meteorites provided essential data for the establishment by Patterson and others of the pre- sently accepted 4500 Ma age of the Earth and the solar system. Analysis of the Allende meteorite, which fell in 1969, inspired the 'supernova trigger' theory of the origin of the solar system, and furnished useful constraints on theories of planetary formation developed by Urey, Ringwood, Anders and others. Many of these theories assumed condensation from a homogeneous hot gas, an assumption that was challenged by astrophysical calculations. The meteoritic-planetesimal theory of planet formation was developed in Russia by Schmidt and later by Safronov. Wetherill, in the United States, established it as the preferred theory for formation of terrestrial planets. -
Protoplanetary Disks, Jets, and the Birth of the Stars
Spanish SKA White Book, 2015 Anglada et al. 169 Protoplanetary disks, jets, and the birth of the stars G. Anglada1, M. Tafalla2, C. Carrasco-Gonz´alez3, I. de Gregorio-Monsalvo4, R. Estalella5, N. Hu´elamo6, O.´ Morata7, M. Osorio1, A. Palau3, and J.M. Torrelles8 1 Instituto de Astrof´ısica de Andaluc´ıa,CSIC, E-18008 Granada, Spain 2 Observatorio Astron´omicoNacional-IGN, E-28014 Madrid, Spain 3 Centro de Radioastronom´ıay Astrof´ısica,UNAM, 58090 Morelia, Michoac´an,Mexico 4 Joint ALMA Observatory, Santiago de Chile, Chile 5 Departament d'Astronomia i Meteorologia, Univ. de Barcelona, E-08028 Barcelona, Spain 6 Centro de Astrobiolog´ıa(INTA-CSIC), E-28691 Villanueva de la Ca~nada,Spain 7 Institute of Astronomy and Astrophysics, Academia Sinica, Taipei 106, Taiwan 8 Instituto de Ciencias del Espacio (CSIC)-UB/IEEC, E-08028 Barcelona, Spain Abstract Stars form as a result of the collapse of dense cores of molecular gas and dust, which arise from the fragmentation of interstellar (parsec-scale) molecular clouds. Because of the initial rotation of the core, matter does not fall directly onto the central (proto)star but through a circumstellar accretion disk. Eventually, as a result of the evolution of this disk, a planetary system will be formed. A fraction of the infalling matter is ejected in the polar direction as a collimated jet that removes the excess of mass and angular momentum, and allows the star to reach its final mass. Thus, the star formation process is intimately related to the development of disks and jets. Radio emission from jets is useful to trace accurately the position of the most embedded objects, from massive protostars to proto-brown dwarfs. -
Terrestrial Planets in High-Mass Disks Without Gas Giants
A&A 557, A42 (2013) Astronomy DOI: 10.1051/0004-6361/201321304 & c ESO 2013 Astrophysics Terrestrial planets in high-mass disks without gas giants G. C. de Elía, O. M. Guilera, and A. Brunini Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata and Instituto de Astrofísica de La Plata, CCT La Plata-CONICET-UNLP, Paseo del Bosque S/N, 1900 La Plata, Argentina e-mail: [email protected] Received 15 February 2013 / Accepted 24 May 2013 ABSTRACT Context. Observational and theoretical studies suggest that planetary systems consisting only of rocky planets are probably the most common in the Universe. Aims. We study the potential habitability of planets formed in high-mass disks without gas giants around solar-type stars. These systems are interesting because they are likely to harbor super-Earths or Neptune-mass planets on wide orbits, which one should be able to detect with the microlensing technique. Methods. First, a semi-analytical model was used to define the mass of the protoplanetary disks that produce Earth-like planets, super- Earths, or mini-Neptunes, but not gas giants. Using mean values for the parameters that describe a disk and its evolution, we infer that disks with masses lower than 0.15 M are unable to form gas giants. Then, that semi-analytical model was used to describe the evolution of embryos and planetesimals during the gaseous phase for a given disk. Thus, initial conditions were obtained to perform N-body simulations of planetary accretion. We studied disks of 0.1, 0.125, and 0.15 M. -
Volatiles in Protoplanetary Disks
Volatiles in Protoplanetary Disks Thesis by Ke Zhang In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy California Institute of Technology Pasadena, California 2015 (Defended May 15, 2015) ii c 2015 Ke Zhang All Rights Reserved iii Acknowledgements First and foremost, I would like to thank my advisor, Geoffrey Blake, for his patience, guidance, support, and inspiration that made this thesis possible. In retrospect, I am so grateful to have chosen Geoff as my mentor. He is a very special kind of advisor, so rare in the fast-paced world, who can be incredibly patient, waiting for a student to find her passion. But once the student has made up her mind, and starts to ask for resources, opportunities, and attention, he is so supportive and resourceful that the only limitation for the student is herself. It was a great privilege working with Geoff, who is ingeniously creative and vastly knowledgeable. Thank you for all the lessons, support, and, most importantly, for believing in and encouraging me. I'm also thankful for John Carpenter who opened for me the wonderful door of (sub)mm-wave interferometry and gave me a very first opportunity to work with ALMA data. John, you are my role model as a rigorous scientist who understands his field profoundly and is dedicated to getting things right. I would also like to thank Colette Salyk for being such a great mentor and a supportive friend during my years in graduate school. Thanks for taking me to the summit of Mauna Kea and beautiful Charlottesville. -
Allowed Planetary Orbits
RELATIONSHIPS OF PARAMETERS OF PLANETARY ORBITS IN SOLAR---TYPE-TYPE SYSTEMS FACULTY OF SCIENCE, PALACKÝ UNIVERSITY, OLOMOUC RELATIONSHIPS OF PARAMETERS OF PLANETARY ORBITS IN SOLAR-TYPE SYSTEMS DOCTORAL THESIS PAVEL PINTR OLOMOUC 2013 VYJÁD ŘENÍ O PODÍLNICTVÍ Prohlašuji, že všichni auto ři se podíleli stejným dílem na níže uvedených článcích: Pintr P., Pe řinová V.: The Solar System from the quantization viewpoint. Acta Universitatis Palackianae, Physica, 42 - 43 , 2003 - 2004, 195 - 209. Pe řinová V., Lukš A., Pintr P.: Distribution of distances in the Solar System. Chaos, Solitons and Fractals 34 , 2007, 669 - 676. Pintr P., Pe řinová V., Lukš A.: Allowed planetary orbits. Chaos, Solitons and Fractals 36 , 2008, 1273 - 1282. Pe řinová V., Lukš A., Pintr P.: Regularities in systems of planets and moons. In: Solar System: Structure, Formation and Exploration . Editor: Matteo de Rossi, Nova Science Publishers, USA (2012), pp. 153-199. ISBN: 978-1-62100-057-0. Pintr P.: Závislost fotometrických parametr ů hv ězd na orbitálních parametrech exoplanet. Jemná Mechanika a Optika 11 - 12 , 2012, 317 - 319. Pintr P., Pe řinová V., Lukš A.: Areal velocities of planets and their comparison. In : Quantization and Discretization at Large Scales . Editors: Smarandache F., Christianto V., Pintr P., ZIP Publishing, Ohio, USA (2012), pp. 15 - 26. ISBN: 9781599732275. Pintr P., Pe řinová V., Lukš A., Pathak A.: Statistical and regression analyses of detected extrasolar systems. Planetary and Space Science 75 , 2013, 37 - 45. Pintr P., Pe řinová V., Lukš A., Pathak A.: Exoplanet habitability for stellar spectral classes F, G, K and M. 2013, v p říprav ě. -
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. -
Formation and Evolution of Exoplanets
Formation and Evolution of Exoplanets Edited by Rory Barnes Astronomy Department University of Washington Box 351580 Seattle, WA 98195-1850, USA Chapter 1 { Exoplanet Observations, Jacob L. Bean Chapter 2 { Pinpointing Planets in Circumstellar Disks, Alice C. Quillen Chapter 3 { Planet-Planet Interactions, Rory Barnes Chapter 4 { Formation Via Disk Instability, Lucio Mayer Chapter 5 { Core Accretion Model, Olenka Hubickyj Chapter 6 { Formation of Terrestrial Planets, Sean N. Raymond Chapter 7 { Brown Dwarfs, Kevin Luhman Chapter 8 { Exoplanet Chemistry, Katharina Lodders Chapter 9 { Migration and Multiplicity E ects During Giant Planet Formation, Edward W. Thommes Chapter 10 { Planets in Mean Motion Resonance, Wilhelm Kley Chapter 11 { Planet{Planet Gravitational Scattering, Francesco Marzari Chapter 12 { Tides and Exoplanets, Brian Jackson, Rory Barnes & Richard Greenberg Chapter 1 { Exoplanet Observations Jacob L. Bean Institut furAstrophysik Friedrich-Hund-Platz 1 37077 Gottingen Germany The discovery and characterization of planets around other stars has revolutionized our view of planetary system formation and evolution. In this chapter, we summarize the main results from the observational study of exoplanetary systems in the context of how they constrain theory. We focus on the robust ndings that have emerged from examining the orbital, physical, and host star properties of large samples of detected exoplanets. We also describe the limitations and biases of current observational methods and potential overinterpretations of the data that should be avoided. In addition, we discuss compelling individual results that o er views beyond the well explored parameter spaces. Chapter 2 { Pinpointing Planets in Circumstellar Disks Alice C. Quillen Dept. of Physics and Astronomy University of Rochester Rochester, NY 14627 USA Recent observations of circumstellar disks have revealed a variety of interesting morphology: clearings, pu ed up disk edges, gaps, spiral-like features, warps, clumps, and lopsidedness. -
Formation and Evolution of Planetary Systems
Specialist Topics in Astrophysics: Lecture 2 Formation and Evolution of Planetary Systems Ken Rice ([email protected]) FormationFormation ofof PlanetaryPlanetary SystemsSystems Lecture 2: Main topics • Solar System characteristics • Origin of the Solar System • Building the planets Most theories of planet formation have been carried out in the context of explaining our Solar System • Any theory must first explain the data/observables OriginOrigin ofof ourour SolarSolar SystemSystem To have a successful theory we must explain the following: • Planets revolve in mostly circular orbits in same direction as the Sun spins OriginOrigin ofof ourour SolarSolar SystemSystem • Planetary orbits nearly lie in a single plane (except Pluto [no longer a planet!!] and Mercury), close to the Sun’s equator • Planets are well spaced, and their orbits do not cross or come close to crossing (except Neptune/Pluto) OriginOrigin ofof ourour SolarSolar SystemSystem • All planets (probably) formed at roughly the same time • Meteorites suggest inner portions of the Solar System were heated to ~1500 K during meteorite/planet formation period OriginOrigin ofof ourour SolarSolar SystemSystem • Planet composition varies in a systematic way throughout the Solar System Terrestrial planets are rocky Outer planets are gaseous OriginOrigin ofof ourour SolarSolar SystemSystem • Jupiter/Saturn are dominated by H and He; Neptune/ Uranus have much less H and He (mainly ices, methane, carbon dioxide and ammonia) OriginOrigin ofof OurOur SolarSolar SystemSystem • Planetary satellites -
How Do You Find an Exoplanet?
October 27, 2015 Time: 09:41am chapter1.tex © Copyright, Princeton University Press. No part of this book may be distributed, posted, or reproduced in any form by digital or mechanical means without prior written permission of the publisher. 1 INTRODUCTION For as long as there been humans we have searched for our place in the cosmos. — Carl Sagan, 1980 1.1 My Brief History I am an astronomer, and as such my professional interest is focused on the study of light emitted by objects in the sky. However, unlike many astronomers, my interest in the night sky didn’t begin until later in my life, well into my college education. I don’t have childhood memories of stargazing, I never thought to ask for a telescope for Christmas, I didn’t have a moon-phase calendar on my wall, and I never owned a single book about astronomy until I was twenty-one years old. As a child, my closest approach to the subject of astronomy was a poster of the Space Shuttle that hung next to my bed, but my interest was piqued more by the intricate mechanical details of the spacecraft rather than where it traveled. Looking back, I suppose the primary reason for my ignorance of astronomy was because I grew up in a metropolitan area, in the North County of St. Louis, Missouri. The skies are often cloudy in the winter when the nights are longest, the evenings are bright with light For general queries, contact [email protected] October 27, 2015 Time: 09:41am chapter1.tex © Copyright, Princeton University Press.