Supplementary Bibliography of Kinetic Data on Gas Phase Reactions of Nitrogen, Oxygen, and Nitrogen Oxides (1972 - 1973)

Total Page:16

File Type:pdf, Size:1020Kb

Supplementary Bibliography of Kinetic Data on Gas Phase Reactions of Nitrogen, Oxygen, and Nitrogen Oxides (1972 - 1973) REFERENCE REFERENCE NAT'L INST. OF STAND & TECH Z NBS SPECIAL PUBLICATION 371 AlllDb 3bQSM7 NBS Publi- cations U.S. DEPARTMENT OF COMMERCE / National Bureau of Standards Supplementari Bibliography of Kinetic Dati» on Gas Phase Reactions oi Nitrogen, Oxygen, Nitrogen Oxidei : NATIONAL BUREAU OF STANDARDS The National Bureau of Standards' was established by an act of Congress March 3, 1901. The Bureau's overall goal is to strengthen and advance the Nation's science and technology and facilitate their effective application for public benefit. To this end, the Bureau conducts research and provides: (1) a basis for the Nation's physical measurement system, (2) scientific and technological services for industry and government, (3) a technical basis for equity in trade, and (4) technical services to promote public safety. The Bureau consists of the Institute for Basic Standards, the Institute for Materials Research, the Institute for Applied Technology, the Institute for Computer Sciences and Technology, and the Office for Information Programs. THE INSTITUTE FOR BASIC STANDARDS provides the central basis within the United States of a complete and consistent system of physical measurement; coordinates that system with measurement systems of other nations; and furnishes essential services leading to accurate and uniform physical measurements throughout the Nation's scientific community, industry, and commerce. The Institute consists of a Center for Radiation Research, an Office of Meas- urement Services and the following divisions: Applied Mathematics — Electricity — Mechanics — Heat — Optical Physics — Nuclear Sciences - — Applied Radiation " — Quantum Electronics — Electromagnetics " — Time " and Frequency — Laboratory Astrophysics " — Cryogenics ". THE INSTITUTE FOR MATERIALS RESEARCH conducts materials research leading to improved methods of measurement, standards, and data on the properties of well-characterized materials needed by industry, commerce, educational institutions, and Government; provides advisory and research services to other Government agencies; and develops, produces, and distributes standard reference materials. The Institute consists of the Office of Standard Reference Materials and the following divisions: Analytical Chemistry — Polymers — Metallurgy — Inorganic Materials — Reactor Radiation — Physical Chemistry. THE INSTITUTE FOR APPLIED TECHNOLOGY provides technical services to promote the use of available technology and to facilitate technological innovation in industry and Government; cooperates with public and private organizations leading to the development of technological standards (including mandatory safety standards), codes and methods of test; and provides technical advice and services to Government agencies upon request. The Institute consists of a Center for Building Technology and the following divisions and offices: Engineering and Product Standards — Weights and Measures — Invention and Innova- tion — Product Evaluation Technology — Electronic Technology — Technical Analysis — Measurement Engineering — Structures, Materials, and Life Safety * — Building Environment* —• Technical Evaluation and Application* — Fire Technology. THE INSTITUTE FOR COMPUTER SCIENCES AND TECHNOLOGY conducts research and provides technical services designed to aid Government agencies in improving cost effec- tiveness in the conduct of their programs through the selection, acquisition, and effective utilization of automatic data processing equipment; and serves as the principal focus within the executive branch for the development of Federal standards for automatic data processing equipment, techniques, and computer languages. The Institute consists of the following divisions Computer Services — Systems and Software — Computer Systems Engineering — Informa- tion Technology. THE OFFICE FOR INFORMATION PROGRAMS promotes optimum dissemination and accessibility of scientific information generated within NBS and other agencies of the Federal Government; promotes the development of the National Standard Reference Data System and a system of information analysis centers dealing with the broader aspects of the National Measurement System; provides appropriate services to ensure that the NBS staff has optimum accessibility to the scientific information of the world. The Office consists of the following organizational units: Office of Standard Reference Data — Office of Information Activities — Office of Technical Publications — Library — Office of International Relations. ^ Headquarters and Laboratories at Gaithersburg, Maryland, unless otherwise noted; mailing address Washington, D.C. 20234. ' Part of the Center for Radiation Research. > Located at Boulder, Colorado 80302. * Part of the Center for Building Technology. BUREAU Of STAfMRDS jUN 1 3 1975 ^cjoo Supplementaiy Bibliography of Kinetic aj' 1 Data on Gas Pliase Reactions of Nitrogen, Oxygen, and Nitrogen Oxides (1972-1973) Francis Westley Chemical Kinetics Information Center Institute for Materials Research U'- National Bureau of Standards Washington, D.C. 20234 i This work was supported by the NBS Office of Standard Reference Data and The Naval Ordnance Systems Command Department of the Navy Washington, D.C. 20360 5^ / U.S. DEPARTMENT OF COMMERCE, Rogers C.B. Morton. Secretary NATIONAL BUREAU OF STANDARDS, Richard W. Roberts, D;rec/or Issued June 1975 Library of Congress Catalog Card Number: 726-00272 National Bureau of Standards Special Publication 371-1 Nat. Bur. Stand. (U.S.), Spec. Publ. 371-1, 88 pages (June 1975) CODEN: XNBSAV For sale by the Superintendent of Documents, U.S. Government Printing Office, Washington, D.C. 20402 (Order by SD Catalog No. C13.10 :371-I) . Price $1.4J cents (Add 25 percent additional for other than U.S. mailing). TABLE OF CONTENTS Introduction • l Guidelines for the user 2 Journal and report codens 6 Part I. Reactions Involving N (and O) species 11 N» -> N + hv 11 N + M -> N» + M 11 N + M* -> N» + M... 11 M» + M -> N + M 11 N + N -> N2» 11 N + N + M -> Ng + M * 11 N + N + M -> N^ + M* 11 N + N + M -> N^* + M 11 N + N + M -> Ng* + M* 12 N + N + M->N2 + M + hv 12 N + -> N + N2 (exchange) 12 N + -> Ng + NO 12 N* N^o -> N2 + NO 12 N + NO -> Ng + 0 12 N + NO -> N^ + 0* 12 N + NO -> Ng* + 0 12 N» + NO -> Ng + 0 12 NO M N + + -> N^o + M 12 N + 0 -> NO + hv 12 N + 0 + M -> NO + M 12 N + 0 + M -> NO + M* 12 N + 0 + M -> NO* + M 13 N + Og -> NO •»• 0 13 N + Og -> NO* + 0 13 ^ * °2* -> NO + 0 ' 13 O2 + "> + ° 13 iii N2 -> N + N 13 \* -> N2 + hv 13 Ng** -> N2» + hv 13 + M -> N + N + M \ + M» -> N + N + M 14 -> Ng* + M N + N + M , 14 ^2 + M -> N2* * M (electronic excitation) 14 + M -> + M (vibrational excitation) , 14 ^2 + M* -> N2» + M (electronic energy transfer) 15 ^2 + M* -> N2'^ + M (electronlc-vlbrational energy transfer) 15 -> + M''' + M (viljratlonal energy transfer) 15 "2 + M** -> N2'^ + M* (electronlc-vlbrational energy transfer) 16 \* M -> N2 •» M (electronic relaxation) 15 ^2* •*- M -> N2 + M (rotational relaxation) 16 ^2* + M -> N2 + M (trans la tlonal relaxation) 16 N^^ + M -> + M (vibrational relaxation) 16 ^2* + M -> N2 + M* (electronic energy transfer) 17 Ng* + M -> N2 + M'^ (electronlc-vlbrational energy transfer) 17 ^2^^ M -> + + M* (vlbrational-electronlc energy transfer) ..».• 13 + M -> N2 + M''' (vibrational energy transfer) • ig \* + M -> N2»* + M (electronic transition) 19 ^2* + M* -> N2 + M** (electronic energy transfer) 19 Ng** + M -> N2» + M (electronic transition) 19 N^** + M -> N2''' + (electronlc-vlbrational energy transfer) 19 ^2** + M -> N2* + M* (vibrational energy transfer) 19 ^2* + N2* -> N2 + N2** (electronic energy transfer) • 19 ^ + 0 -> N NO 19 N2 + 0* -> NgO* 20 > 0 + M -> N2O M 20 + 0» + M -> N2O + M 20 1^2 + O2 -> NO + NO 20 N2O -> Ng + 0 20 iv -> N2 )- 0« 20 NgO* -> N2 + 0 20 N2O* "> \0 + hv 20 N2O + hv -> N2 + 0* 20 NjO + M -> I/2N2 + NO + M (overall) 20 N2O + M -> N2 + 0 + M 21 ^20 + M» -> N2 + 0 + M 21 \0 + M* -> N2 + 0* + M 21 NgO M -> N2 + I/2O2 + M (overall) 21 \o + Vi^ ~> + M (vibrational energy transfer) .rt,.,,- ........ 21 NgO* + M -> N2O + M (electronic relaxation) 21 N2O* + M -> NgO + M (rotational relaxation) . • ,, 21 NgO* + M -> NgO ¥ M ( trans lational relaxation) ^t.... 21 U + M -> + M (vibrational relaxation) 22 N^o'^ + M -> NgO + (vibrational enerj^y transfer) 22 NgO + NO -> S2 + NO2 22 -> , >. \0 + 0 N2 + Og . 22 ^*20 + 0 -> N2 + O2* 22 NgO + 0* -> N2 + O2 o., -. 22 N2O 4- 0 -> NO -f m , 22 N2O + 0» -> 110 NO 23 N2O2 -> H2 + O2 23 N2O2 -> NgO + 0 , 23 N2O2 + M3 -> N2 + NO + O2 23 ^202 + NO -> N2O + NO2 23 N2O3 + N2O5 -> 4NO2 • 23 ^204 + M -> NOg + NO2 + M (a.t low and hi^ pressure)... , r..... 23 N2O5 + M -> NO2 + MO3 + M 23 N2O5 + N2O5 -> 4NO2 + O2 (overall) * 23 NO* -> NO + hv 23 N0«* -> NO* + hv , , 23 NO + hv -> K + 0 , 24 V NO + bv ~> ro* 24 NO + M -> N + 0 + M 24 -> 0» NO + M N + + M 24 NO + M -> M* + 0 + M , 24 NO + M* -> IJO* + M (electronic enepj^y traiisfer) , 24 NO + M* -> NO=t + M (electrijQic-vibratiorjal energy transfer) 24 Jfl' -> NO + N0+ + M (vibrational energy tr>ir=sfer) , 24 NO* + M -> I© + M (electronic relaxation) 24 NO* + M -> NO + M (rotational relaxation) 25 N0+ + M -> 10 + M (vibrational relaxation) ». , 25 NO* + M -> NO + M ( trans laticnal relaxation) 25 NO* + M -> NO + H* (electronic energy transfer)..., , , 25 N0+ + M -> NO + (vibrational energy transfer)....,. 25 NO** + M -> NO* + H (electronic transition) 25 N0+^ + M -> N0=^ + (vibration-vibration resonant exchange) 25 NO + NO -> N^ + O2 (overall) 25 NO + NO* -> Ng + O2 25 NO + NO -> NgO + 0 (first
Recommended publications
  • JOHN R. THORSTENSEN Address
    CURRICULUM VITAE: JOHN R. THORSTENSEN Address: Department of Physics and Astronomy Dartmouth College 6127 Wilder Laboratory Hanover, NH 03755-3528; (603)-646-2869 [email protected] Undergraduate Studies: Haverford College, B. A. 1974 Astronomy and Physics double major, High Honors in both. Graduate Studies: Ph. D., 1980, University of California, Berkeley Astronomy Department Dissertation : \Optical Studies of Faint Blue X-ray Stars" Graduate Advisor: Professor C. Stuart Bowyer Employment History: Department of Physics and Astronomy, Dartmouth College: { Professor, July 1991 { present { Associate Professor, July 1986 { July 1991 { Assistant Professor, September 1980 { June 1986 Research Assistant, Space Sciences Lab., U.C. Berkeley, 1975 { 1980. Summer Student, National Radio Astronomy Observatory, 1974. Summer Student, Bartol Research Foundation, 1973. Consultant, IBM Corporation, 1973. (STARMAP program). Honors and Awards: Phi Beta Kappa, 1974. National Science Foundation Graduate Fellow, 1974 { 1977. Dorothea Klumpke Roberts Award of the Berkeley Astronomy Dept., 1978. Professional Societies: American Astronomical Society Astronomical Society of the Pacific International Astronomical Union Lifetime Publication List * \Can Collapsed Stars Close the Universe?" Thorstensen, J. R., and Partridge, R. B. 1975, Ap. J., 200, 527. \Optical Identification of Nova Scuti 1975." Raff, M. I., and Thorstensen, J. 1975, P. A. S. P., 87, 593. \Photometry of Slow X-ray Pulsars II: The 13.9 Minute Period of X Persei." Margon, B., Thorstensen, J., Bowyer, S., Mason, K. O., White, N. E., Sanford, P. W., Parkes, G., Stone, R. P. S., and Bailey, J. 1977, Ap. J., 218, 504. \A Spectrophotometric Survey of the A 0535+26 Field." Margon, B., Thorstensen, J., Nelson, J., Chanan, G., and Bowyer, S.
    [Show full text]
  • Arxiv:2105.11583V2 [Astro-Ph.EP] 2 Jul 2021 Keck-HIRES, APF-Levy, and Lick-Hamilton Spectrographs
    Draft version July 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 The California Legacy Survey I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades Lee J. Rosenthal,1 Benjamin J. Fulton,1, 2 Lea A. Hirsch,3 Howard T. Isaacson,4 Andrew W. Howard,1 Cayla M. Dedrick,5, 6 Ilya A. Sherstyuk,1 Sarah C. Blunt,1, 7 Erik A. Petigura,8 Heather A. Knutson,9 Aida Behmard,9, 7 Ashley Chontos,10, 7 Justin R. Crepp,11 Ian J. M. Crossfield,12 Paul A. Dalba,13, 14 Debra A. Fischer,15 Gregory W. Henry,16 Stephen R. Kane,13 Molly Kosiarek,17, 7 Geoffrey W. Marcy,1, 7 Ryan A. Rubenzahl,1, 7 Lauren M. Weiss,10 and Jason T. Wright18, 19, 20 1Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 2IPAC-NASA Exoplanet Science Institute, Pasadena, CA 91125, USA 3Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 4Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA 5Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 6Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA 7NSF Graduate Research Fellow 8Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA 9Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 10Institute for Astronomy, University of Hawai`i,
    [Show full text]
  • UC Irvine UC Irvine Previously Published Works
    UC Irvine UC Irvine Previously Published Works Title Astrophysics in 2006 Permalink https://escholarship.org/uc/item/5760h9v8 Journal Space Science Reviews, 132(1) ISSN 0038-6308 Authors Trimble, V Aschwanden, MJ Hansen, CJ Publication Date 2007-09-01 DOI 10.1007/s11214-007-9224-0 License https://creativecommons.org/licenses/by/4.0/ 4.0 Peer reviewed eScholarship.org Powered by the California Digital Library University of California Space Sci Rev (2007) 132: 1–182 DOI 10.1007/s11214-007-9224-0 Astrophysics in 2006 Virginia Trimble · Markus J. Aschwanden · Carl J. Hansen Received: 11 May 2007 / Accepted: 24 May 2007 / Published online: 23 October 2007 © Springer Science+Business Media B.V. 2007 Abstract The fastest pulsar and the slowest nova; the oldest galaxies and the youngest stars; the weirdest life forms and the commonest dwarfs; the highest energy particles and the lowest energy photons. These were some of the extremes of Astrophysics 2006. We attempt also to bring you updates on things of which there is currently only one (habitable planets, the Sun, and the Universe) and others of which there are always many, like meteors and molecules, black holes and binaries. Keywords Cosmology: general · Galaxies: general · ISM: general · Stars: general · Sun: general · Planets and satellites: general · Astrobiology · Star clusters · Binary stars · Clusters of galaxies · Gamma-ray bursts · Milky Way · Earth · Active galaxies · Supernovae 1 Introduction Astrophysics in 2006 modifies a long tradition by moving to a new journal, which you hold in your (real or virtual) hands. The fifteen previous articles in the series are referenced oc- casionally as Ap91 to Ap05 below and appeared in volumes 104–118 of Publications of V.
    [Show full text]
  • A Disintegrating Minor Planet Transiting a White Dwarf!
    A Disintegrating Minor Planet Transiting a White Dwarf! Andrew Vanderburg1, John Asher Johnson1, Saul Rappaport2, Allyson Bieryla1, Jonathan Irwin1, John Arban Lewis1, David Kipping1,3, Warren R. Brown1, Patrick Dufour4, David R. Ciardi5, Ruth Angus1,6, Laura Schaefer1, David W. Latham1, David Charbonneau1, Charles Beichman5, Jason Eastman1, Nate McCrady7, Robert A. Wittenmyer8, & Jason T. Wright9,10. ! White dwarfs are the end state of most stars, including We initiated follow-up ground-based photometry to the Sun, after they exhaust their nuclear fuel. Between better time-resolve the transits seen in the K2 data (Figure 1/4 and 1/2 of white dwarfs have elements heavier than S1). We observed WD 1145+017 frequently over the course helium in their atmospheres1,2, even though these of about a month with the 1.2-meter telescope at the Fred L. elements should rapidly settle into the stellar interiors Whipple Observatory (FLWO) on Mt. Hopkins, Arizona; unless they are occasionally replenished3–5. The one of the 0.7-meter MINERVA telescopes, also at FLWO; abundance ratios of heavy elements in white dwarf and four of the eight 0.4-meter telescopes that compose the atmospheres are similar to rocky bodies in the Solar MEarth-South Array at Cerro Tololo Inter-American system6,7. This and the existence of warm dusty debris Observatory in Chile. Most of these data showed no disks8–13 around about 4% of white dwarfs14–16 suggest interesting or significant signals, but on two nights we that rocky debris from white dwarf progenitors’ observed deep (up to 40%), short-duration (5 minutes), planetary systems occasionally pollute the stars’ asymmetric transits separated by the dominant 4.5 hour atmospheres17.
    [Show full text]
  • Massive Fast Rotating Highly Magnetized White Dwarfs: Theory and Astrophysical Applications
    Massive Fast Rotating Highly Magnetized White Dwarfs: Theory and Astrophysical Applications Thesis Advisors Ph.D. Student Prof. Remo Ruffini Diego Leonardo Caceres Uribe* Dr. Jorge A. Rueda *D.L.C.U. acknowledges the financial support by the International Relativistic Astrophysics (IRAP) Ph.D. program. Academic Year 2016–2017 2 Contents General introduction 4 1 Anomalous X-ray pulsars and Soft Gamma-ray repeaters: A new class of pulsars 9 2 Structure and Stability of non-magnetic White Dwarfs 21 2.1 Introduction . 21 2.2 Structure and Stability of non-rotating non-magnetic white dwarfs 23 2.2.1 Inverse b-decay . 29 2.2.2 General Relativity instability . 31 2.2.3 Mass-radius and mass-central density relations . 32 2.3 Uniformly rotating white dwarfs . 37 2.3.1 The Mass-shedding limit . 38 2.3.2 Secular Instability in rotating and general relativistic con- figurations . 38 2.3.3 Pycnonuclear Reactions . 39 2.3.4 Mass-radius and mass-central density relations . 41 3 Magnetic white dwarfs: Stability and observations 47 3.1 Introduction . 47 3.2 Observations of magnetic white dwarfs . 49 3.2.1 Introduction . 49 3.2.2 Historical background . 51 3.2.3 Mass distribution of magnetic white dwarfs . 53 3.2.4 Spin periods of isolated magnetic white dwarfs . 53 3.2.5 The origin of the magnetic field . 55 3.2.6 Applications . 56 3.2.7 Conclusions . 57 3.3 Stability of Magnetic White Dwarfs . 59 3.3.1 Introduction . 59 3.3.2 Ultra-magnetic white dwarfs . 60 3.3.3 Equation of state and virial theorem violation .
    [Show full text]
  • Arxiv:2001.10147V1
    Magnetic fields in isolated and interacting white dwarfs Lilia Ferrario1 and Dayal Wickramasinghe2 Mathematical Sciences Institute, The Australian National University, Canberra, ACT 2601, Australia Adela Kawka3 International Centre for Radio Astronomy Research, Curtin University, Perth, WA 6102, Australia Abstract The magnetic white dwarfs (MWDs) are found either isolated or in inter- acting binaries. The isolated MWDs divide into two groups: a high field group (105 − 109 G) comprising some 13 ± 4% of all white dwarfs (WDs), and a low field group (B < 105 G) whose incidence is currently under investigation. The situation may be similar in magnetic binaries because the bright accretion discs in low field systems hide the photosphere of their WDs thus preventing the study of their magnetic fields’ strength and structure. Considerable research has been devoted to the vexed question on the origin of magnetic fields. One hypothesis is that WD magnetic fields are of fossil origin, that is, their progenitors are the magnetic main-sequence Ap/Bp stars and magnetic flux is conserved during their evolution. The other hypothesis is that magnetic fields arise from binary interaction, through differential rotation, during common envelope evolution. If the two stars merge the end product is a single high-field MWD. If close binaries survive and the primary develops a strong field, they may later evolve into the arXiv:2001.10147v1 [astro-ph.SR] 28 Jan 2020 magnetic cataclysmic variables (MCVs). The recently discovered population of hot, carbon-rich WDs exhibiting an incidence of magnetism of up to about 70% and a variability from a few minutes to a couple of days may support the [email protected] [email protected] [email protected] Preprint submitted to Journal of LATEX Templates January 29, 2020 merging binary hypothesis.
    [Show full text]
  • L119 a Dusty Disk Around Gd 362, a White Dwarf with A
    The Astrophysical Journal, 632:L119–L122, 2005 October 20 ᭧ 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. A DUSTY DISK AROUND GD 362, A WHITE DWARF WITH A UNIQUELY HIGH PHOTOSPHERIC METAL ABUNDANCE E. E. Becklin,1 J. Farihi,2 M. Jura,1 Inseok Song,2 A. J. Weinberger,3 and B. Zuckerman1 Received 2005 July 14; accepted 2005 September 9; published 2005 October 5 ABSTRACT Eighteen years after an infrared excess was discovered associated with the white dwarf G29-38, we report ground-based measurements (JHKs KLN ) with millijansky-level sensitivity of GD 362 that show it to be a second single white dwarf with an infrared excess. As a first approximation, the excess around GD 362, which amounts to ∼3% of the total stellar luminosity, can be explained by emission from a passive, flat, opaque dust disk that lies within the Roche radius of the white dwarf. The dust may have been produced by the tidal disruption of a large parent body such as an asteroid. Accretion from this circumstellar disk could account for the remarkably high abundance of metals in the star’s photosphere. Subject headings: circumstellar matter — minor planets, asteroids — white dwarfs Ϫ 1. INTRODUCTION of comets and asteroids with a rate of3 # 10 6 g s 1 (Fixsen & Dwek 2002), and analogous circumstellar dust debris pro- It is likely that many planetary systems survive a star’s evo- duced by the destruction of parent bodies is common around lution as a red giant and persist as the star becomes a white main-sequence stars (Zuckerman 2001).
    [Show full text]
  • Post-Main-Sequence Planetary System Evolution Rsos.Royalsocietypublishing.Org Dimitri Veras
    Post-main-sequence planetary system evolution rsos.royalsocietypublishing.org Dimitri Veras Department of Physics, University of Warwick, Coventry CV4 7AL, UK Review The fates of planetary systems provide unassailable insights Cite this article: Veras D. 2016 into their formation and represent rich cross-disciplinary Post-main-sequence planetary system dynamical laboratories. Mounting observations of post-main- evolution. R. Soc. open sci. 3: 150571. sequence planetary systems necessitate a complementary level http://dx.doi.org/10.1098/rsos.150571 of theoretical scrutiny. Here, I review the diverse dynamical processes which affect planets, asteroids, comets and pebbles as their parent stars evolve into giant branch, white dwarf and neutron stars. This reference provides a foundation for the Received: 23 October 2015 interpretation and modelling of currently known systems and Accepted: 20 January 2016 upcoming discoveries. 1. Introduction Subject Category: Decades of unsuccessful attempts to find planets around other Astronomy Sun-like stars preceded the unexpected 1992 discovery of planetary bodies orbiting a pulsar [1,2]. The three planets around Subject Areas: the millisecond pulsar PSR B1257+12 were the first confidently extrasolar planets/astrophysics/solar system reported extrasolar planets to withstand enduring scrutiny due to their well-constrained masses and orbits. However, a retrospective Keywords: historical analysis reveals even more surprises. We now know that dynamics, white dwarfs, giant branch stars, the eponymous celestial body that Adriaan van Maanen observed pulsars, asteroids, formation in the late 1910s [3,4]isanisolatedwhitedwarf(WD)witha metal-enriched atmosphere: direct evidence for the accretion of planetary remnants. These pioneering discoveries of planetary material around Author for correspondence: or in post-main-sequence (post-MS) stars, although exciting, Dimitri Veras represented a poor harbinger for how the field of exoplanetary e-mail: [email protected] science has since matured.
    [Show full text]
  • Survival of Exomoons Around Exoplanets 2
    Survival of exomoons around exoplanets V. Dobos1,2,3, S. Charnoz4,A.Pal´ 2, A. Roque-Bernard4 and Gy. M. Szabo´ 3,5 1 Kapteyn Astronomical Institute, University of Groningen, 9747 AD, Landleven 12, Groningen, The Netherlands 2 Konkoly Thege Mikl´os Astronomical Institute, Research Centre for Astronomy and Earth Sciences, E¨otv¨os Lor´and Research Network (ELKH), 1121, Konkoly Thege Mikl´os ´ut 15-17, Budapest, Hungary 3 MTA-ELTE Exoplanet Research Group, 9700, Szent Imre h. u. 112, Szombathely, Hungary 4 Universit´ede Paris, Institut de Physique du Globe de Paris, CNRS, F-75005 Paris, France 5 ELTE E¨otv¨os Lor´and University, Gothard Astrophysical Observatory, Szombathely, Szent Imre h. u. 112, Hungary E-mail: [email protected] January 2020 Abstract. Despite numerous attempts, no exomoon has firmly been confirmed to date. New missions like CHEOPS aim to characterize previously detected exoplanets, and potentially to discover exomoons. In order to optimize search strategies, we need to determine those planets which are the most likely to host moons. We investigate the tidal evolution of hypothetical moon orbits in systems consisting of a star, one planet and one test moon. We study a few specific cases with ten billion years integration time where the evolution of moon orbits follows one of these three scenarios: (1) “locking”, in which the moon has a stable orbit on a long time scale (& 109 years); (2) “escape scenario” where the moon leaves the planet’s gravitational domain; and (3) “disruption scenario”, in which the moon migrates inwards until it reaches the Roche lobe and becomes disrupted by strong tidal forces.
    [Show full text]
  • R E P O R T Not an Accident That She and Her Team Have Raised More Support for Faculty and Students in the College Than Ever Before in History
    Winter 2008 Volume Nine REPORT COLLEGE OF LETTERS AND SCIENCE A showcase of the people and progress in the UCLA College of Letters and Science 6 8 10 An Academic Gem Returns A Master of Narrating Something Dramatic the Incomprehensible and Violent After two years under wraps, the renowned collections of the William Historian Saul Friedlander brings to Astronomers in the College have Andrews Clark Memorial Library are a close his work on Nazi Germany identified clues in a cosmic catastro- once again open to the public and to and the genocide of the Jews with phe which may show evidence of the the scholars of the world. an award-winning volume. formation of planets like Earth. Exploring the Struggle for Computing the Explosion in Success Stories Social Justice Genetic Information Four UCLA students talk about Ruth Milkman explores the evolving Matteo Pellegrini is using computer how the university’s Academic trends that make Los Angeles a technology to help biological scientists Advancement Program, the catalyst for change in the American expand the possibilities for genetic nation’s largest student diversity labor movement. research. program, supported them in their challenges—and triumphs. 12 14 16 On the cover: The Mildred E. Mathias Botanical Garden at UCLA is a haven for research, teaching—or for peaceful reflection on a busy campus day. The seven-acre Mathias Garden, located on Snapshots the east border of the UCLA campus, is a living museum that maintains one of America’s largest outdoor collections of tropical and sub-tropical plants. The garden also offers public education programs, and serves as an outdoor classroom for undergraduate College News Great Futures courses and graduate training in several UCLA departments.
    [Show full text]
  • Joint Meeting of the American Astronomical Society & The
    American Association of Physics Teachers Joint Meeting of the American Astronomical Society & Joint Meeting of the American Astronomical Society & the 5-10 January 2007 / Seattle, Washington Final Program FIRST CLASS US POSTAGE PAID PERMIT NO 1725 WASHINGTON DC 2000 Florida Ave., NW Suite 400 Washington, DC 20009-1231 MEETING PROGRAM 2007 AAS/AAPT Joint Meeting 5-10 January 2007 Washington State Convention and Trade Center Seattle, WA IN GRATITUDE .....2 Th e 209th Meeting of the American Astronomical Society and the 2007 FOR FURTHER Winter Meeting of the American INFORMATION ..... 5 Association of Physics Teachers are being held jointly at Washington State PLEASE NOTE ....... 6 Convention and Trade Center, 5-10 January 2007, Seattle, Washington. EXHIBITS .............. 8 Th e AAS Historical Astronomy Divi- MEETING sion and the AAS High Energy Astro- REGISTRATION .. 11 physics Division are also meeting in LOCATION AND conjuction with the AAS/AAPT. LODGING ............ 12 Washington State Convention and FRIDAY ................ 44 Trade Center 7th and Pike Streets SATURDAY .......... 52 Seattle, WA AV EQUIPMENT . 58 SUNDAY ............... 67 AAS MONDAY ........... 144 2000 Florida Ave., NW, Suite 400, Washington, DC 20009-1231 TUESDAY ........... 241 202-328-2010, fax: 202-234-2560, [email protected], www.aas.org WEDNESDAY..... 321 AAPT AUTHOR One Physics Ellipse INDEX ................ 366 College Park, MD 20740-3845 301-209-3300, fax: 301-209-0845 [email protected], www.aapt.org Acknowledgements Acknowledgements IN GRATITUDE AAS Council Sponsors Craig Wheeler U. Texas President (6/2006-6/2008) Ball Aerospace Bob Kirshner CfA Past-President John Wiley and Sons, Inc. (6/2006-6/2007) Wallace Sargent Caltech Vice-President National Academies (6/2004-6/2007) Northrup Grumman Paul Vanden Bout NRAO Vice-President (6/2005-6/2008) PASCO Robert W.
    [Show full text]
  • Aspects of Planetary Systems Around White Dwarfs
    Planetary Systems Around White Dwarfs Dimitri Veras1;2 (1) Centre for Exoplanets and Habitability, University of Warwick, Coventry CV4 7AL, United Kingdom (2) Department of Physics, University of Warwick, Coventry CV4 7AL, United Kingdom ABSTRACT White dwarf planetary science is a rapidly growing field of research featuring a diverse set of observations and theoretical explorations. Giant planets, minor planets, and debris discs have all been detected orbiting white dwarfs. The innards of broken-up minor planets are measured on an element-by-element basis, providing a unique probe of exoplanetary chemistry. Numerical simulations and analytical investigations trace the violent physical and dynamical history of these systems from au-scale distances to the immediate vicinity of the white dwarf, where minor planets are broken down into dust and gas and are accreted onto the white dwarf photosphere. Current and upcoming ground-based and space- based instruments are likely to further accelerate the pace of discoveries. Subject headings: Asteroids, Planets, White Dwarfs, Discs, Geochemistry, Plan- etary Interiors, Planet Formation, Celestial Mechanics, Tides, Evolved Stars 1. Introduction White dwarf exoplanetary systems provide windows into composition, physical processes and minor planets (asteroids, comets, moons, and interior fragments of larger planets) which are unavailable in main-sequence investigations. Almost every known exoplanet orbits a star that will become a white dwarf, and these exoplanets will either survive or be destroyed throughout the stellar transformation. En route, the exoplanets' perturbations on smaller bodies contribute to the latter's physical and dynamical evolution, allowing them to approach and be destroyed by the white dwarf. The resulting remnants are ubiquitously observable, such that the occurrence rate of white dwarf planetary systems is comparable to that of main-sequence exoplanetary systems.
    [Show full text]