Astrochemistry Lecture 2 Basic Processes (cont d)
|
|
- Junior McGee
- 6 years ago
- Views:
Transcription
1 Astrochemistry Lecture 2 Basic Processes (cont d) Ewine F. van Dishoeck Leiden Observatory Spring 2008
2 Types of chemical reactions Formation of bonds Radiative association: X + + Y XY + + hν Associative detachment X - + Y Æ XY + e Grain surface: X + Y:g XY + g Destruction of bonds Photo-dissociation: XY + hν X + Y Dissociative recombination: XY + + e X + Y Collisional dissociation: XY + M X + Y + M Rearrangement of bonds Ion-molecule reactions: X + + YZ XY + + Z Charge-transfer reactions: X + + YZ X + YZ + Neutral-neutral reactions: X + YZ XY + Z
3 2.1 Ion-molecule reactions Ion induces dipole moment in molecule when it approaches it => long-range attraction which goes as μ1/r 4 Reaction is rapid even at low T if the reaction is exothermic; rate can be readily computed by classical capture theory developed by Langevin 1905 Energy X + + YZ XY + + Z XYZ + Reaction path
4 Classical capture theory X + b c YZ - Reaction only occurs if impact parameter b small enough that X + is captured, i.e., spends enough time near YZ for reaction to take place
5 Langevin rate Langevin rate Interaction potential (induced dipole + centrifugal barrier): V ( e b eff R )= α μ v V eff has maximum value: Critical impact parameter: 1 2 2R 2R ( μb v ) /(8 αe ) F > v = H G I / ( b ) /(8 e ) b 2 K J crit μv μ α Centrifugal barrier 4αe μv Rate coefficient is independent of T: α=polarizability b=impact parameter v=velocity k e = σ πb = π α 2 9 v = critv 2 10 cm s μ 2 3 1
6 Ion-molecule processes X + + YZ Æ XY + + Z exchange Æ X + YZ + charge transfer Many experiments performed at room T, some at low T. Most reactions (>90%) indeed proceed at Langevin rate, but some exceptions known NH 3+ + H 2 Æ NH 4+ + H
7 Experiments M. Smith Rate coefficients for ion-polar reactions may be factors of larger than Langevin values at low T, because V(R)μR -2 Example: C + + OH Æ CO + + H
8 Unusual case: N + + H 2 -Potentially initiates much of nitrogen chemistry -Rate decreases rapidly at low T, however, because reaction slightly endothermic at T<100 K
9 2.2 Neutral-neutral reactions Long-range attraction weak: van der Waals interaction μ 1/R 6 Potential barriers may occur in entrance and exit channels => reactions thought to be slow at low T Experiments: reactions can be fast at low T! Energy X + YZ XY + Z entrance XYZ exit Reaction path
10 CN + C 2 H 6 : or why extrapolation is unreliable k / cm 3 molec -1 sec -1 T/K /(T/K) I. Sims et al. Rennes/Birmingham
11 CN + C 2 H 6 : or why extrapolation is unreliable T/K k / cm 3 molec -1 sec T/K k / cm 3 molec -1 sec T/K 10 3 / (T/K) k / cm 3 molec -1 sec /(T/K) / (T/K)
12 CN + C 2 H 6 : or why extrapolation is unreliable T/K k / cm 3 molec -1 sec T/K k / cm 3 molec -1 sec T/K 10 3 / (T/K) k / cm 3 molec -1 sec /(T/K) / (T/K)
13 CN + C 2 H 6 : reaction stays rapid at low T! k / cm 3 molec -1 sec T/K I. R. Sims, J. L. Queffelec, D. Travers, B. R. Rowe, L. B. Herbert, J. Karthäuser, and I. W. M. Smith, Chem. Phys. Lett. 211 (4-5), 461 (1993) / (T/K)
14 Isentropic expansion CRESU technique and slm carrier gas (He, Ar or N 2 ) + precursor + reagent uniform supersonic flow axisymmetric Laval nozzle boundary layer sets scale of apparatus nozzle throat diameter 3 mm 5 cm uniform supersonic flow T = K ρ = cm 3 Laval nozzle and isentropic flow chamber pressure mbar pumping speed m 3 hr -1
15 Laval nozzles on rockets
16 Types of neutral-neutral reactions E A /k V(R) Molecule-molecule >10 4 K E.g., H 2 +D 2 Æ 2HD Radical-saturated mol ~2000 E.g., OH + H 2 Æ H 2 O + H Radical-unsaturated mol ~0 E.g., OH + CO Æ CO 2 + H Radical-radical -100 E.g., O + OH Æ O 2 + H
17 Rate coefficient V Blow-up entrance channel J>0 J=0 V = V ( R) + J / 2μR eff A 2 2 R c R - Determined by shape entrance potential - Low energy collisions: R c large
18 Adiabatic capture approximation If collision energy < V eff (R c ): reaction probability=0 If collision energy > V eff (R c ): reaction probability=1 This implies that one needs to know the potential surface in the entrance channel very well! Advantages Analytical formulae for rate constants for easy use in chemical networks Disadvantages Ignores angular dependence potential Ignores short range forces Ignores quantum effects (e.g., tunneling) Assumes no activation energy D. Clary 1993
19 Adiabatic capture theory Rate coefficient kt T n 2 ( ) as T Æ 0 for potentials of the form R -n Interaction Potential Low T dep. Charge-induced dipole R -4 T 0 Charge-dipole R -2 T -1/2 Charge-quadrupole R -3 T -1/6 Dipole-dipole R -3 T -1/6 Dipole-quadrupole R -4 T 0 Dispersion R -6 T 1/6
20 Experiments: examples -Some reactions are faster at low T than at high T - These neutral-neutral reactions are typically only a factor of 5 slower than ion-molecule reactions at low T => cannot be neglected in networks!
21 -Reactions with O( 3 P 2 ), S( 3 P 2 ), (non-zero J lowest fine-structure level) are fast, but with C( 3 P 0 ), Si( 3 P 0 ),. (J=0 lowest fine-structure level) are slow? Radical-atom reactions Importance of fine-structure excitation N + OH ÆNO + H O(J=2) O + OH ÆO 2 + H Exp Rate at low T controversial!
22 2.3 Gas-grain chemistry: H 2 Evidence for gas-grain chemistry H 2 in interstellar clouds NH in diffuse clouds Abundances H 2 O, CO 2, CH 3 OH, in ices higher than expected from freeze-out of gas phase
23 Formation mechanisms Diffusive mechanism (Langmuir-Hinshelwood) X + g:y Æ X:g:Y Æ X-Y:g Æ XY + g sticking diffusion + desorption molecule formation Direct mechanism (Eley-Rideal) X + Y:g Æ X-Y:g ÆXY + g direct reaction desorption Surface can be silicates, carbonaceous, ice,
24 Grain surface processes diffusive vs. direct
25 Diffusive mechanism X + g: Y X: g: Y X Y: g XY + g sticking diffusion+ desorption mol.form Process proceeds in several steps: 1. H atom must collide with grain: H + g 2. Colliding atom must stick to surface: H + g H : g 3. H atom must be retained until another atom gets absorbed: H : g H : g : H 4. H atoms must be mobile to find each other and form bond: H : g : H H H : g 5. H 2 must be ejected from surface: H H : g H 2 + g Probabilities of 2, 3+4 and 5 are η S, η r, η d
26 H 2 formation on grains
27 1. Collision rate with grain Collision rate: rc = πa 2 vh ngn( H) where πa 2 =geometrical cross section v H =10 4 T 1/2 cm s -1 ~10 5 at 100 K n g =number density of grains Observations of extinction: πa n 3 10 rc nhn( H) 2 22 g Compare with required H 2 formation rate (from obs) R = nhn( H)η η η f S r d => all probabilities must be nearly unity n H
28 2. Adsorption time Classical expression: t = 1 E kt ν exp( / ) a d With E d =binding energy; ν=e d /k~10 12 s -1 Physical adsorption: E d ~400 K => t a =3x10 5 s at T=10 K t a =2x10-8 s at T=40 K Chemisorption: E d ~20000 K => t a = at 100 K => H atoms will evaporate above 40 K before forming H 2, unless the grain has strong binding sites
29 3. Arrival of second H atom Consider t a of first H atom with time for collision of second H atom with grain t C 1 = = s for n(h) = 1 rn( H) C = 3 10 s for n(h) = 100 cm 2 3 t C <t a if T<15 K for physical absorption At higher temperatures, need chemisorption to retain first H
30 4. Surface hopping In diffuse clouds: T>15 K, T d >15 K => need chemisorption to retain H Assume second H atom is physically adsorbed Hopping time second H atom: t h ~10-9 s For random 2D walk: where r=distance between sites ~1.5 Å 2 => t M <t a for T<20 K with Second H atom can find first H atom before evaporation t M π( a / 2) = th 10 2 r 3 s
31 5. Ejection Since there are no strong H 2 -grain bonds, H 2 is now physically adsorbed and will be rapidly ejected From 1-5 it is plausible that η S η r η d ª1, provided the dust temperature is not too high
32 Eley-Rideal mechanism X + Y: g X Y: g XY + g direct reaction desorption If there are enough chemisorption sites so that grain is saturated with H atoms, formation rate of H 2 is controlled by rate of arrival of H atoms at surface It is assumed that H 2 is formed at every encounter, and rapidly ejected back into gas phase This process is important especially at higher T
33 Simulations diffuse mechanism Takahashi et al. 1998
34 Simulation Eley-Rideal mechanism
35 H 2 formation Recent flurry of experiments and theory Experiments provide constraints on mobility of adsorbed H and on binding and diffusion energies on various materials: silicates, carbonaceous material (graphite), ices Modeling of experimental data somewhat controversial Roughness/irregularity of surface and temperature fluctuations play a role as well Pironello et al Biham et al Cazaux & Tielens 2004 Hornekaer et al Vidali et al Cuppen & Herbst 2007
36 2.4 Gas-grain chemistry: other species Only diffusive mechanisms considered Typical day in the life on the surface of a grain in a dense cloud A few molecules or atoms land on the icy surface All species except He stick with η S =1 If sufficiently light, the particle can migrate over the surface by tunneling or thermal hopping Migrating species: H, O, C, N Perhaps: CH, NH, OH, NH 2, CH 2, CH 3 Reactions may occur if activation barriers sufficiently low
37 Relevant time scales See Sect. 2.3 for formulae adsorption (=residence) and migration (=thermal hopping) times Tunneling only important for H, H 2 Limiting activation barriers of reactions at T d =10 K H 3500 K H 4500 K 2 O,C,N 450 K
38 Types of surface reactions 1. Atom-atom reactions, e.g., N + O Æ NO 2. Radical- atom reactions, e.g., H + NOÆ HNO 3. Radical-radical reactions, e.g., CH 3 + OH Æ CH 3 OH 4. Radical-H 2 reactions, e.g., OH + H 2 Æ H 2 O + H 5. Molecule atom reactions, e.g., CO + O Æ CO 2 6. Hydrogen abstraction reactions, e.g., H 2 CO + H Æ HCO + H 2 Type 1,2,3: No activation barrier (typically) Type 4,5,6: Activation barrier
39 Example: H 2 O formation Tielens & Hagen 1982
40 Example: CH 3 OH and HCOOH
41 Experimental simulation Condensation of ice (CO, O 2, N 2, ) in UHV chamber Bombardment by cooled atomic beam (H,O) produced in microwave or DC discharge Analysis of products by Reflection Absorption InfraRed Spectroscopy (RAIRS) and Mass Spectrometry Few groups around the world capable of these experiments, including Sackler laboratory in Leiden
42 Main QMS From FTIR Spectrometer To rotary stage Secondary QMS H 2 7:1 / 45:8 ellipsoidal mirror H 2 :18 off-axis parabolic mirror 100 K gas InSb / MCT l.n 2 cooled IR detector External link to FTIR Spectrometer Atomic Source To rotary stage Turbo Pump Turbo Pump To rotary stage
43 Some experimental results Hiraoka et al. 1994, 1995, 1998, 2002 H bombardment of activated N 2, CO, N 2 O ices (10-30 monolayers containing few % of N, C, O) 1% yield of NH 3, CH 4, H 2 O => Hydrogenation of N, C, O is efficient H can penetrate into apolar matrices H bombardment of CO ice ~0.01% yield of H 2 CO and CH 3 OH: low! Watanabe et al. 2002, 2003, 2005 H bombardment of CO-H2O and CO matrix ~10% yield of H2CO and CH3OH: high! Yield CH 3 OH is optimal at 15 K Fuchs et al H bombardment of CO-H 2 O and CO matrix Results consistent with both groups, depending on H flux CH 3 OH can be formed at low T!
44 CH 3 OH experiment IR spectroscopy to monitor products Max. CH 3 OH yield at 15 K Higher T => less sticking of H Watanabe et al.2003
45 2.5 Photochemistry in ices Ices in dark clouds can be irradiated by UV due to Penetration interstellar radiation: up to A V =5 mag Cosmic ray photons Internal sources (young stellar objects) => ~10 UV photons per molecule in 10 5 yr Many experiments in laboratories on different ice mixtures => rapid formation of CO 2, H 2 CO, in H 2 O:CO irradiated ices Experiments with UV and high-energy particle bombardment => large data base Interstellar applications need to take competition with reactions with H into account No strong observational evidence yet for UV photolysis of ices
46
47
48 Types of reactions 1. Photodissociation, e.g., H2O + hn Æ OH + H 2. Molecule - radical reactions, e.g., CO + OH Æ COOH 3. Radical-radical reactions, e.g., COOH + H Æ HCOOH CONH 2 + NH 2 Æ HNCO + NH 3 4. Acid-base reactions, e.g., HCOOH + NH3 Æ HCOO- + NH4+ 5. Thermal reactions, e.g., CO + O Æ CO 2 6. Hydrogen abstraction reactions, e.g., H 2 CO + H Æ HCO + H 2 Type 1,2,3: No activation barrier Type 4,5,6: Activation barrier
Astrochemistry the summary
Astrochemistry the summary Astro 736 Nienke van der Marel April 27th 2017 Astrochemistry When the first interstellar molecules were discovered, chemists were very surprised. Why? Conditions in space are
More information2- The chemistry in the. The formation of water : gas phase and grain surface formation. The present models. Observations of molecules in the ISM.
2- The chemistry in the ISM. The formation of water : gas phase and grain surface formation. The present models. Observations of molecules in the ISM. 1 Why studying the ISM chemistry? 1- The thermal balance,
More informationOUTLINE OF A GAS-GRAIN CHEMICAL CODE. Dima Semenov MPIA Heidelberg
OUTLINE OF A GAS-GRAIN CHEMICAL CODE Dima Semenov MPIA Heidelberg MOTTO OF ASTROCHEMISTRY CODE DEVELOPMENT We had 5 ODE solvers, 9 Jacobi matrix inversion routines, several approaches to calculate reaction
More informationLecture 6: Molecular Transitions (1) Astrochemistry
Lecture 6: Molecular Transitions (1) Astrochemistry Ehrenfreund & Charnley 2000, ARA&A, 38, 427 Outline Astrochemical processes: The formation of H2 H3 formation The chemistry initiated by H3 Formation
More informationGAS PHASE CHEMICAL KINETICS : EXPERIMENTAL ADVANCES AND PROSPECTS
GAS PHASE CHEMICAL KINETICS : EXPERIMENTAL ADVANCES AND PROSPECTS Sébastien Le Picard France Astrophysique de Laboratoire Institut de Physique de Rennes Université de Rennes 1 Gas phase chemistry in the
More informationHydrogenation of solid hydrogen cyanide HCN and methanimine CH 2 NH at low temperature
Hydrogenation of solid hydrogen cyanide HCN and methanimine CH 2 NH at low temperature P. Theule, F. Borget, F. Mispelaer, G. Danger, F. Duvernay, J. C. Guillemin, and T. Chiavassa 5 534,A64 (2011) By
More informationThe Interstellar Medium
The Interstellar Medium Fall 2014 Lecturer: Dr. Paul van der Werf Oortgebouw 565, ext 5883 pvdwerf@strw.leidenuniv.nl Assistant: Kirstin Doney Huygenslaboratorium 528 doney@strw.leidenuniv.nl Class Schedule
More information19. Interstellar Chemistry
19. Interstellar Chemistry 1. Introduction to Interstellar Chemistry 2. Chemical Processes & Models 3. Formation & Destruction of H 2 4. Formation & Destruction of CO References Duley & Williams, "Interstellar
More informationAstrochemistry and Molecular Astrophysics Paola Caselli
School of Physics and Astronomy FACULTY OF MATHEMATICS & PHYSICAL SCIENCES Astrochemistry and Molecular Astrophysics Paola Caselli Outline 1. The formation of H 2 2. The formation of H 3 + 3. The chemistry
More informationAstrochimistry Spring 2013
Astrochimistry Spring 2013 Lecture 3: H2 Formation NGC 7023 - HST Julien Montillaud 1st February 2013 Outline I. The most abundant molecule in the Universe (6 p.) I.1 Relative abundances I.2 Historical
More informationOxidation processes on cold surfaces, diffusion and reactivity
Marco Minissale Université de Cergy-Pontoise and Observatoire de Paris Oxidation processes on cold surfaces, diffusion and reactivity Leiden, 13th March 2013 What we know about oxygenation? Astrophysical
More information21. Introduction to Interstellar Chemistry
21. Introduction to Interstellar Chemistry 1. Background 2. Gas Phase Chemistry 3. Formation and Destruction of H 2 4. Formation and Destruction of CO 5. Other Simple Molecules References Tielens, Physics
More informationThe formation of stars and planets. Day 1, Topic 2: Radiation physics. Lecture by: C.P. Dullemond
The formation of stars and planets Day 1, Topic 2: Radiation physics Lecture by: C.P. Dullemond Astronomical Constants CGS units used throughout lecture (cm,erg,s...) AU = Astronomical Unit = distance
More informationInterstellar Dust and Extinction
University of Oxford, Astrophysics November 12, 2007 Outline Extinction Spectral Features Emission Scattering Polarization Grain Models & Evolution Conclusions What and Why? Dust covers a range of compound
More informationGas-grain chemistry in cold interstellar cloud cores with a microscopic Monte Carlo approach to surface chemistry ABSTRACT
A&A 469, 973 983 (2007) DOI: 05/0004-636:20077423 c ESO 2007 Astronomy & Astrophysics Gas-grain chemistry in cold interstellar cloud cores with a microscopic Monte Carlo approach to surface chemistry Q.
More informationLow Temperature Reactions: A Path to Interstellar Study Introduction:
Low Temperature Reactions: A Path to Interstellar Study Wade Eveland Advisor: Dr. Simon North 04/22/2013 Introduction: Initially, the big bang created mostly hydrogen and helium, yet the universe today
More informationCosmic Evolution, Part II. Heavy Elements to Molecules
Cosmic Evolution, Part II Heavy Elements to Molecules First a review of terminology: Element Atom Electro- magnetic Electrons Nucleus Electromagnetic Strong Nuclear Compound Molecule Protons Neutrons Neutral
More informationSecondary Ion Mass Spectrometry (SIMS)
CHEM53200: Lecture 10 Secondary Ion Mass Spectrometry (SIMS) Major reference: Surface Analysis Edited by J. C. Vickerman (1997). 1 Primary particles may be: Secondary particles can be e s, neutral species
More informationThe KInetic Database for Astrochemistry
The KInetic Database for Astrochemistry Valentine Wakelam and the KIDA team Laboratory astrophysics of Bordeaux France ICE Interstellar chemical models Compute species abundances as a function of time
More informationAstrochemical Models. Eric Herbst Departments of Chemistry and Astronomy University of Virginia
Astrochemical Models Eric Herbst Departments of Chemistry and Astronomy University of Virginia Chemical Models Gas-phase reactions 1000 s of reactions Grain-surface reactions Abundances, columns, spectra
More informationLecture 18 - Photon Dominated Regions
Lecture 18 - Photon Dominated Regions 1. What is a PDR? 2. Physical and Chemical Concepts 3. Molecules in Diffuse Clouds 4. Galactic and Extragalactic PDRs References Tielens, Ch. 9 Hollenbach & Tielens,
More informationLecture 10: "Chemistry in Dense Molecular Clouds"
Lecture 10: "Chemistry in Dense Molecular Clouds" Outline 1. Observations of molecular clouds 2. Physics of dense clouds 3. Chemistry of dense clouds: C-, O-, N-chemistry Types of molecular clouds Diffuse
More information" There's life Jim...but we don't KNOW it (yet): a journey through the chemically controlled cosmos from star birth to the formation of life"
" There's life Jim...but we don't KNOW it (yet): a journey through the chemically controlled cosmos from star birth to the formation of life" 30 th May 2007, Stockholm Observatory with support from the
More informationCosmic Evolution, Part II. Heavy Elements to Molecules
Cosmic Evolution, Part II Heavy Elements to Molecules Heavy elements molecules First a review of terminology: Electromagnetic Electrons Element Atom Nucleus Compound Molecule Electromagnetic Strong Nuclear
More informationMaster Equation for Hydrogen Recombination on Grain Surfaces
Syracuse University SURFACE Physics College of Arts and Sciences 12-12-2000 Master Equation for Hydrogen Recombination on Grain Surfaces Gianfranco Vidali Department of Physics, Syracuse University, Syracuse,
More informationAstrochemistry. Lecture 10, Primordial chemistry. Jorma Harju. Department of Physics. Friday, April 5, 2013, 12:15-13:45, Lecture room D117
Astrochemistry Lecture 10, Primordial chemistry Jorma Harju Department of Physics Friday, April 5, 2013, 12:15-13:45, Lecture room D117 The first atoms (1) SBBN (Standard Big Bang Nucleosynthesis): elements
More informationLecture 18 Long Wavelength Spectroscopy
Lecture 18 Long Wavelength Spectroscopy 1. Introduction. The Carriers of the Spectra 3. Molecular Structure 4. Emission and Absorption References Herzberg, Molecular Spectra & Molecular Structure (c. 1950,
More informationarxiv: v1 [astro-ph] 17 Sep 2007
Astronomy & Astrophysics manuscript no. 8210Hat c ESO 2008 February 1, 2008 H-atom bombardment of CO 2, HCOOH and CH 3 CHO containing ices S. E. Bisschop, G. W. Fuchs, E. F. van Dishoeck, and H. Linnartz
More informationPhysics and Chemistry of the Interstellar Medium
Physics and Chemistry of the Interstellar Medium Sun Kwok The University of Hong Kong UNIVERSITY SCIENCE BOOKS Sausalito, California * Preface xi The Interstellar Medium.1.1 States of Matter in the ISM
More informationSurface Chemistry and Reaction Dynamics of Electron Beam Induced Deposition Processes
Surface Chemistry and Reaction Dynamics of Electron Beam Induced Deposition Processes e -? 2 nd FEBIP Workshop Thun, Switzerland 2008 Howard Fairbrother Johns Hopkins University Baltimore, MD, USA Outline
More informationPhysics 224 The Interstellar Medium
Physics 224 The Interstellar Medium Lecture #11: Dust Composition, Photoelectric Heating, Neutral Gas Outline Part I: Dust Heating & Cooling continued Part III: Dust Emission & Photoelectric Heating Part
More informationInterstellar dust: The hidden protagonist. Stéphanie Cazaux Marco Spaans Vincent Cobut Paola Caselli Rowin Meijerink
Interstellar dust: The hidden protagonist Stéphanie Cazaux Marco Spaans Vincent Cobut Paola Caselli Rowin Meijerink th 15 February 2012 Overview Star form in clouds made of gas + dust Catalyst: Enrich
More informationChemical Reactions Induced by Ionizing and Electron-beam Irradiation in Freon/Water (Ice) Films
Chemical Reactions Induced by Ionizing and Electron-beam Irradiation in Freon/Water (Ice) Films Johns Hopkins University (founded in 1876) Dr. C.C. Perry Prof. D.H. Fairborther School of Arts & Sciences
More informationLaser Dissociation of Protonated PAHs
100 Chapter 5 Laser Dissociation of Protonated PAHs 5.1 Experiments The photodissociation experiments were performed with protonated PAHs using different laser sources. The calculations from Chapter 3
More informationPDR Modelling with KOSMA-τ
PDR Modelling with KOSMA-τ M. Röllig, V. Ossenkopf-Okada, C. Bruckmann; Y. Okada, N. Schneider, U. Graf, J. Stutzki I. Physikalisches Institut, Universität zu Köln The KOSMA-τ PDR Code 1-D, spherical geometry
More informationDissociative recombination reactions. Wolf D. Geppert ISSI workshop, Bern (CH) December 2008
Dissociative recombination reactions Wolf D. Geppert ISSI workshop, Bern (CH) December 2008 Important electron-ion processes A B - Resonant ion pair formation (high energies) AB hν Radiative recombination
More informationNew models of interstellar gas±grain chemistry ± I. Surface diffusion rates
Mon. Not. R. Astron. Soc. 319, 837±850 (2000) New models of interstellar gas±grain chemistry ± I. Surface diffusion rates Deborah P. Ruffle 1 and Eric Herbst 2w 1 Department of Physics, The Ohio State
More information6. Interstellar Medium. Emission nebulae are diffuse patches of emission surrounding hot O and
6-1 6. Interstellar Medium 6.1 Nebulae Emission nebulae are diffuse patches of emission surrounding hot O and early B-type stars. Gas is ionized and heated by radiation from the parent stars. In size,
More informationIonization Detectors
Ionization Detectors Basic operation Charged particle passes through a gas (argon, air, ) and ionizes it Electrons and ions are collected by the detector anode and cathode Often there is secondary ionization
More informationDust in the Diffuse Universe
Dust in the Diffuse Universe Obscuring Effects Chemical Effects Thermal Effects Dynamical Effects Diagnostic Power Evidence for Grains: Chemical Effects Catalyzes molecular hydrogen formation. Depletion
More information8: Composition and Physical state of Interstellar Dust
8: Composition and Physical state of Interstellar Dust James Graham UC, Berkeley 1 Reading Tielens, Interstellar Medium, Ch. 5 Mathis, J. S. 1990, AARA, 28, 37 Draine, B. T., 2003, AARA, 41, 241 2 Nature
More informationThermal Equilibrium in Nebulae 1. For an ionized nebula under steady conditions, heating and cooling processes that in
Thermal Equilibrium in Nebulae 1 For an ionized nebula under steady conditions, heating and cooling processes that in isolation would change the thermal energy content of the gas are in balance, such that
More informationLec 3. Radiative Processes and HII Regions
Lec 3. Radiative Processes and HII Regions 1. Photoionization 2. Recombination 3. Photoionization-Recombination Equilibrium 4. Heating & Cooling of HII Regions 5. Strömgren Theory (for Hydrogen) 6. The
More informationc re l 4. Controlling reagents and characterizing products Control of reagent orientation
4. Controlling reagents and characterizing products Reagent state selection in molecular beams Selection of velocity in a molecular beam. Achieved through the use of choppers, control of source pressure,
More informationAstronomy 106, Fall September 2015
Today in Astronomy 106: molecules to molecular clouds to stars Aromatic (benzene-ring) molecules in space Formation of molecules, on dust-grain surfaces and in the gas phase Interstellar molecular clouds
More informationSUPPLEMENTARY INFORMATION
Supplementary Discussion In this Supplementary Discussion, we give more detailed derivations of several of the results in our letter. First, we describe in detail our method of calculating the temperature
More informationHall, Milton Keynes MK7 6AA, UK Published online: 06 Jul 2015.
This article was downloaded by: [Universiteit Leiden / LUMC] On: 06 July 2015, At: 07:14 Publisher: Taylor & Francis Informa Ltd Registered in England and Wales Registered Number: 1072954 Registered office:
More informationIR Spectroscopy and physicochemical effects on astrophysical ices produced by energetic ions collisions
IR Spectroscopy and physicochemical effects on astrophysical ices produced by energetic ions collisions Ana Lucia de Barros Physics Department Centro Federal de Educação Tecnológica Celso Suckow da Fonseca
More informationPHYSICS OF THE SPACE ENVIRONMENT
PHYSICS OF THE SPACE ENVIRONMENT PHYS/EATS 380 Winter 006 Notes Set 6 Ionospheric Electron Densities The D, E, F1 and F Layers With the advent of radio communication in the early part of the last century
More informationPhotodissociation and ionisation of molecules due to stellar and cosmic-ray-induced radiation
Photodissociation and ionisation of molecules due to stellar and cosmic-ray-induced radiation A. N. Heays, A. D. Bosman, and E. F. van Dishoeck Leiden Observatory, The Netherlands Objective Update and
More informationChemistry on interstellar grains
Journal of Physics: Conference Series Chemistry on interstellar grains To cite this article: E Herbst et al 2005 J. Phys.: Conf. Ser. 6 18 View the article online for updates and enhancements. Related
More informationPlanetary Atmospheres
Planetary Atmospheres Structure Composition Meteorology Clouds Photochemistry Atmospheric Escape EAS 4803/8803 - CP 20:1 Cloud formation Saturated Vapor Pressure: Maximum amount of water vapor partial
More informationLECTURE NOTES. Ay/Ge 132 ATOMIC AND MOLECULAR PROCESSES IN ASTRONOMY AND PLANETARY SCIENCE. Geoffrey A. Blake. Fall term 2016 Caltech
LECTURE NOTES Ay/Ge 132 ATOMIC AND MOLECULAR PROCESSES IN ASTRONOMY AND PLANETARY SCIENCE Geoffrey A. Blake Fall term 2016 Caltech Acknowledgment Part of these notes are based on lecture notes from the
More informationNuclear spin temperatures of hydrogen and water molecules formed and trapped on ice. Naoki Watanabe
9 Jun 2014, Nuclear Spin Effects in Astrochemistry 2014, Göteborg Nuclear spin temperatures of hydrogen and water molecules formed and trapped on ice Naoki Watanabe Institute of Low Temperature Science,
More informationComponents of Galaxies Gas The Importance of Gas
Components of Galaxies Gas The Importance of Gas Fuel for star formation (H 2 ) Tracer of galaxy kinematics/mass (HI) Tracer of dynamical history of interaction between galaxies (HI) The Two-Level Atom
More informationChapter 4: Astrochemistry: Synthesis and Modelling
Chapter 4: Astrochemistry: Synthesis and Modelling Valentine Wakelam Univ. Bordeaux, LAB, UMR 5804, F-33270, Floirac, France CNRS, LAB, UMR 5804, F-33270, Floirac, France Herma M. Cuppen Theoretical Chemistry,
More informationAcidic Water Monolayer on Ruthenium(0001)
Acidic Water Monolayer on Ruthenium(0001) Youngsoon Kim, Eui-seong Moon, Sunghwan Shin, and Heon Kang Department of Chemistry, Seoul National University, 1 Gwanak-ro, Seoul 151-747, Republic of Korea.
More informationX-ray Radiation, Absorption, and Scattering
X-ray Radiation, Absorption, and Scattering What we can learn from data depend on our understanding of various X-ray emission, scattering, and absorption processes. We will discuss some basic processes:
More informationFormation of molecular hydrogen on analogues of interstellar dust grains: experiments and modelling
Journal of Physics: Conference Series Formation of molecular hydrogen on analogues of interstellar dust grains: experiments and modelling To cite this article: Gianfranco Vidali et al 2005 J. Phys.: Conf.
More informationAdsorption of gases on solids (focus on physisorption)
Adsorption of gases on solids (focus on physisorption) Adsorption Solid surfaces show strong affinity towards gas molecules that it comes in contact with and some amt of them are trapped on the surface
More informationLow temperature reactions between stored ions and condensable gases: formation of protonated methanol via radiative association
WDS 02 Proceedings of Contributed Papers, PART II, 294-300, 2002. ISBN 80-85863-88-X MATFYZPRESS Low temperature reactions between stored ions and condensable gases: formation of protonated methanol via
More informationAstrochemistry (2) Interstellar extinction. Measurement of the reddening
Measurement of the reddening The reddening of stellar colours casts light on the properties of interstellar dust Astrochemistry (2) Planets and Astrobiology (2016-2017) G. Vladilo The reddening is measured
More informationATM 507 Lecture 4. Text reading Chapters 3 and 4 Today s topics Chemistry, Radiation and Photochemistry review. Problem Set 1: due Sept.
ATM 507 Lecture 4 Text reading Chapters 3 and 4 Today s topics Chemistry, Radiation and Photochemistry review Problem Set 1: due Sept. 11 Temperature Dependence of Rate Constants Reaction rates change
More informationVictoria Louise Frankland. Heriot-Watt University. September 2011
Towards Understanding the Formation of Water on Interstellar Dust Grains Victoria Louise Frankland Submitted for the degree of Doctor of Philosophy Heriot-Watt University School of Engineering and Physical
More informationHerschel Constraints on Ice Formation and Destruction in Protoplanetary Disks
Herschel Constraints on Ice Formation and Destruction in Protoplanetary Disks Ilse Cleeves, University of Michigan Edwin Bergin, University of Michigan Karin Öberg, Harvard-Smithsonian CfA. Michiel Hogerheijde,
More informationIs plasma important? Influence molecule formation?
Is plasma important? Influence molecule formation? Plasma Structure (space & time) Influence? Daan Schram Eindhoven University of Technology d.c.schram@tue.nl http://www.tue.nl/en/employee/ep/e/d/ep-uid/19780797/?no_cache=1&chash=e23e831cf0c6bebeac6023f04dd3c4b6
More informationLecture 6 - spectroscopy
Lecture 6 - spectroscopy 1 Light Electromagnetic radiation can be thought of as either a wave or as a particle (particle/wave duality). For scattering of light by particles, air, and surfaces, wave theory
More informationModelling complex organic molecules in dense regions: Eley Rideal and complex induced reaction
doi:10.1093/mnras/stu2709 Modelling complex organic molecules in dense regions: Eley Rideal and complex induced reaction M. Ruaud, 1,2 J. C. Loison, 3,4 K. M. Hickson, 3,4 P. Gratier, 1,2 F. Hersant 1,2
More informationAdsorption, desorption, and diffusion on surfaces. Joachim Schnadt Divsion of Synchrotron Radiation Research Department of Physics
Adsorption, desorption, and diffusion on surfaces Joachim Schnadt Divsion of Synchrotron Radiation Research Department of Physics Adsorption and desorption Adsorption Desorption Chemisorption: formation
More informationThe Formation of Molecular Hydrogen in the Interstellar Medium
The Formation of Molecular Hydrogen in the Interstellar Medium FARAHJABEEN ISLAM Thesis submitted for the degree of Doctor of Philosophy University College London 2009 I, Farahjabeen Islam, confirm that
More informationWater formation at low temperatures by surface O 2 hydrogenation II: the reaction network
PAPER www.rsc.org/pccp Physical Chemistry Chemical Physics Water formation at low temperatures by surface O 2 hydrogenation II: the reaction network H. M. Cuppen,* ab S. Ioppolo, a C. Romanzinw a and H.
More informationThe chemistry of interstellar space
The chemistry of interstellar space Eric Herbst Departments of Physics and Astronomy, The Ohio State University, Columbus, Ohio 43210, USA Received 27th November 2000 First published as an Advance Article
More information7. Dust Grains & Interstellar Extinction. James R. Graham University of California, Berkeley
7. Dust Grains & Interstellar Extinction James R. Graham University of California, Berkeley Visual Extinction Presence of interstellar gas or nebulae has a long history Existence of absorbing interstellar
More informationAstr 2310 Thurs. March 23, 2017 Today s Topics
Astr 2310 Thurs. March 23, 2017 Today s Topics Chapter 16: The Interstellar Medium and Star Formation Interstellar Dust and Dark Nebulae Interstellar Dust Dark Nebulae Interstellar Reddening Interstellar
More informationLecture 7: Molecular Transitions (2) Line radiation from molecular clouds to derive physical parameters
Lecture 7: Molecular Transitions (2) Line radiation from molecular clouds to derive physical parameters H 2 CO (NH 3 ) See sections 5.1-5.3.1 and 6.1 of Stahler & Palla Column density Volume density (Gas
More informationPhysical Chemistry Chemical Physics
Physical Chemistry Chemical Physics www.rsc.org/pccp Volume 12 Number 23 21 June 2010 Pages 5929 6292 ISSN 1463-9076 COVER ARTICLE Brown et al. Ice in space: surface science investigations of the thermal
More informationSome HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines!
Some HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines Idealized 21cm spectra Example observed 21cm spectra HI densities
More informationA Far-ultraviolet Fluorescent Molecular Hydrogen Emission Map of the Milky Way Galaxy
A Far-ultraviolet Fluorescent Molecular Hydrogen Emission Map of the Milky Way Galaxy (The Astrophysical Journal Supplement Series, 231:21 (16pp), 2017 August) November 14, 2017 Young-Soo Jo Young-Soo
More informationElectronic Transition Spectra of Thiophenoxy and Phenoxy Radicals in Hollow cathode discharges
Electronic Transition Spectra of Thiophenoxy and Phenoxy Radicals in Hollow cathode discharges Tokyo Univ. Science Mitsunori ARAKI, Hiromichi WAKO, Kei NIWAYAMA and Koichi TSUKIYAMA 2014/06/16 2015/2/20
More informationResonances in Chemical Reactions : Theory and Experiment. Toshiyuki Takayanagi Saitama University Department of Chemistry
Resonances in Chemical Reactions : Theory and Experiment Toshiyuki Takayanagi Saitama University Department of Chemistry What is Chemical Reaction? Collision process between molecules (atoms) containing
More informationCosmic-ray induced diffusion, reactions and destruction of molecules in interstellar ices
Juris Kalvāns Engineering Research Institute «Ventspils International Radio Astronomy Center» of Ventspils University College, Inženieru 101, Ventspils, Latvia, LV-3601 (VIRAC) Cosmic-ray induced diffusion,
More informationa few more introductory subjects : equilib. vs non-equil. ISM sources and sinks : matter replenishment, and exhaustion Galactic Energetics
Today : a few more introductory subjects : equilib. vs non-equil. ISM sources and sinks : matter replenishment, and exhaustion Galactic Energetics photo-ionization of HII assoc. w/ OB stars ionization
More informationA resonant energy transfer toy model for CO ice
A resonant energy transfer toy model for CO ice Octavio Roncero Inst. Física Fundamental, CSIC Madrid (Spain) octavio.roncero@csic.es Outline Introduction 2 Förster Resonance Energy transfer 3 Reactivity
More informationThe Interstellar Medium
http://www.strw.leidenuniv.nl/~pvdwerf/teaching/ The Interstellar Medium Lecturer: Dr. Paul van der Werf Fall 2014 Oortgebouw 565, ext 5883 pvdwerf@strw.leidenuniv.nl Assistant: Kirstin Doney Huygenslaboratorium
More informationCatalysis Lectures W.H. Green 5.68J/10.652J Spring Handouts: Norskov et al., J. Catalysis Imbihl and Ertl, Chem. Rev. (partial) Homework
Catalysis Lectures W.H. Green 5.68J/10.652J Spring 2003 Handouts: Norskov et al., J. Catalysis Imbihl and Ertl, Chem. Rev. (partial) Homework Major points: 1) Why reactions have barriers, and how catalysts
More informationIR Spectrography - Absorption. Raman Spectrography - Scattering. n 0 n M - Raman n 0 - Rayleigh
RAMAN SPECTROSCOPY Scattering Mid-IR and NIR require absorption of radiation from a ground level to an excited state, requires matching of radiation from source with difference in energy states. Raman
More informationChapter 6. Summary and Conclusions
Chapter 6 Summary and Conclusions Plasma deposited amorphous hydrogenated carbon films (a-c:h) still attract a lot of interest due to their extraordinary properties. Depending on the deposition conditions
More informationInterstellar Medium and Star Birth
Interstellar Medium and Star Birth Interstellar dust Lagoon nebula: dust + gas Interstellar Dust Extinction and scattering responsible for localized patches of darkness (dark clouds), as well as widespread
More informationPhotochemistry and Astrochemistry: Photochemical Pathways to Interstellar Complex Organic Molecules
pubs.acs.org/cr Photochemistry and Astrochemistry: Photochemical Pathways to Interstellar Complex Organic Molecules Karin I. O berg* Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge,
More informationMaster course: Astrochemistry Basic principles and recent results
Master course: Astrochemistry Basic principles and recent results Ewine F. van Dishoeck Leiden Observatory Spring 2008 Outline of course Introduction; Basic molecular processes I Basic molecular processes
More informationChemistry Instrumental Analysis Lecture 34. Chem 4631
Chemistry 4631 Instrumental Analysis Lecture 34 From molecular to elemental analysis there are three major techniques used for elemental analysis: Optical spectrometry Mass spectrometry X-ray spectrometry
More informationCHM 5423 Atmospheric Chemistry Notes on kinetics (Chapter 4)
CHM 5423 Atmospheric Chemistry Notes on kinetics (Chapter 4) Introduction A mechanism is one or a series of elementary reactions that convert reactants into products or otherwise model the chemistry of
More informationThe Interstellar Medium (ch. 18)
The Interstellar Medium (ch. 18) The interstellar medium (ISM) is all the gas (and about 1% dust) that fills our Galaxy and others. It is the raw material from which stars form, and into which stars eject
More informationComplex organic molecules along the accretion flow in isolated and externally irradiated protoplanetary disks
Complex organic molecules along the accretion flow in isolated and externally irradiated protoplanetary disks Walsh, C., Herbst, E., Nomura, H., Millar, T. J., & Widicus Weaver, S. (214). Complex organic
More informationDiffuse Interstellar Medium
Diffuse Interstellar Medium Basics, velocity widths H I 21-cm radiation (emission) Interstellar absorption lines Radiative transfer Resolved Lines, column densities Unresolved lines, curve of growth Abundances,
More informationVibrational Spectroscopies. C-874 University of Delaware
Vibrational Spectroscopies C-874 University of Delaware Vibrational Spectroscopies..everything that living things do can be understood in terms of the jigglings and wigglings of atoms.. R. P. Feymann Vibrational
More informationAtmospheric escape. Volatile species on the terrestrial planets
Atmospheric escape MAVEN s Ultraviolet Views of Hydrogen s Escape from Mars Atomic hydrogen scattering sunlight in the upper atmosphere of Mars, as seen by the Imaging Ultraviolet Spectrograph on NASA's
More informationUpdate Log. ITYPE Reaction types in the gas-phase model
Update Log ITYPE Reaction types in the gas-phase model 0 Gas-grain interaction, Electron-grain recombination 1 Cosmic-ray ionization (direct process) #1, Cosmic-ray induced photoreactions (indirect process)
More informationThe Kinetic Monte Carlo Method as a Way To Solve the Master Equation for Interstellar Grain Chemistry
pubs.acs.org/cr Terms of Use The Kinetic Monte Carlo Method as a Way To Solve the Master Equation for Interstellar Grain Chemistry H. M. Cuppen,*, L. J. Karssemeijer, and T. Lamberts, Theoretical Chemistry,
More informationThe Dusty Universe. Joe Weingartner George Mason University Dept of Physics and Astronomy
The Dusty Universe Joe Weingartner George Mason University Dept of Physics and Astronomy To astronomers, dust means: sub micron solid grains (1 micron = 1 m = 10 6 m = one millionth of a meter) Typical
More information