Bringa, E

Tielens, A

vanBreugel, W

UNT Digital Library

UCRL-CONF-222778Galaxies, Black Holes & Laboratories:Studies of interstellar medium materials inenergetic environmentsW. vanBreugel, E. Bringa, A. TielensJuly 12, 2006Dust and gas in ULIRGs: Tracing Star Formation and BlackHole Growth at the Centers of the Ultraluminous InfraredGalaxiesIthaca, NY, United StatesJune 19, 2006 through June 22, 2006Disclaimer   This document was prepared as an account of work sponsored by an agency of the United States Government. Neither the United States Government nor the University of California nor any of their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or usefulness of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply its endorsement, recommendation, or favoring by the United States Government or the University of California. The views and opinions of authors expressed herein do not necessarily state or reflect those of the United States Government or the University of California, and shall not be used for advertising or product endorsement purposes.  Galaxies, Black Holes &Laboratories:Studies of interstellar medium materialsin energetic environmentsWil van BreugelPhysics and Advanced Technologies, LLNLandUniversity of California, Merced+E. Bringa, LLNLA. Tielens, NASA/Amesand many othersDust and gas in ULIRGs, Cornell Univ., June 20, 2006This work was performed under the auspices of the U.S. Department of Energy,National Nuclear Security Administration by the University of California,Lawrence Livermore National Laboratory under contract No. W -7405-Eng-48MotivationPlan• Two ISM dust types• Two energy regimes• Two dust grain morphologies• Study processes where LLNLcan uniquely contribute– Experimentally– NumericallyLLNL Assets• High energy experimental andcomputational facilities, “astro-materials” expertiseScience Case• Energetic feedback fromsupernovae & active black ingalaxies• Interstellar dust controlsformation of stars & planetsGalaxy Formation & Energetic Feedback• Galaxies grow through merging,triggering collapse of interstellarclouds, star formation, supernovae• Thermal pressure, and photon +particle (Cosmic Ray) densities 10– 1000 x Milky Way• Galaxy and central black holemasses fundamentally related• Energy input from active blackholes affects galaxy formationEnergetic feedback on interstellar medium (pressure, radiation & Cosmic Rays)key to understanding evolution of galaxiesStar formation in merging galaxy Galaxy massBlackholemassHST image•  ISM materials condense out in stellar outflows & ejecta of superovae•  Mix silicate / carbon depends on type of star and evolutionary stageTwo types of ISM dustSilicates  ->  Rocks• Olivine!s, incl. Mg2SiO4 (forsterite)• Other common minerals in the ISM,Interplanetary Dust Particles,Comets, EarthCarbonaceous  ->  Life• Graphite, nano-diamonds• Hydrogenated Amorphous Carbon• Basis for more complex organicmolecules, LifeTwo energy regimes & morphologies• Amorphization: Irradiate crystallinematerials (silicates and carbonaceous) athigh energies to see if caused by CosmicRays (E. Bringa - this meeting)• Cover both nuclear (low) and electronic(high) energy regimes– Astrophysical shocks (100 km/s : 100eV - 10 keV)– Cosmic Rays (low en. mostabundant: 0.1 - 5 GeV)– Effects will be different: bondbreaking vs. re-ordering (C-rings)HSTMol. Dyn. sim.10-310-210-110010110210310410510610-210-1100101Nuclear Collisions Electronic ExcitationsCosmic RaysOther Plasmas  Incident Energy (keV)Deposited Energy=dE/dx (eV/nm) Electronic NuclearShocksChemistryTwo energy deposition regimesTwo astrophysical regimesThermal: ShocksNon-thermal: Cosmic RaysBoth occur in supernovae and jetsGraphite Anthracite-CoalTwo morphologiesCan Cosmic Rays amorphizeISM silicate dust? E. Bringa - this meeting2006 - LBNL 88” Cyclotron LLNLIon Beam LBNLHeavy  Ion Acc.ElectronicNuclear• LBNL experiments (Feb 2006)• 500 MeV Fe-ions• Galactic Cosmic Ray fluence• Results currently being analyzed2005 - LLNL Ion Beam ObservationBradley et al 1984ExperimentBringa et al 2006 Amorphous Ion Tracks Crystalline Xe3+TEM image• ISM silicate dust grains, observed• Crystalline in stellar outflows• Amorphous in dense ISM clouds• Possible reason: Cosmic rays• LLNL experiments:• 10 MeV ions (Xe+++) amorphize fosterite• dE/dx models then suggest lowenergy (100 - 500 MeV) Cosmic Ray Fe-ions will do this also, at fluencesrepresentative for our Galaxy• Hydrocarbons and organicmolecules form in stellaroutflows, ISM gas, and on ISMdust grains• Become integrated in SolarSystem and (pre-biotic) EarthLifecycles of hydrocarbons (CmHn), PAHs, andorganic (H, C, N, O, S, P) moleculesPossible Processes?• Gas phase chemistry• Big supply available• Energy source, efficiency?• Chemistry changes induced ingrains by energetic ions• Hot gas in shocks (keV ions)• Cosmic Rays (0.1 - 1 GeV mostabundant)• Regeneration due to grain-graincollisions in shocks• Supernovae• Active black holes• Colliding galaxiesISM cloud: dust and gas• Polycyclic Aromatic Hydrocarbons• Ubiquitous around clouds• Easily destroyed by UV light• Must be replenished inside cloudsSpitzer Space TelescopePAH!s• Graphite - Tokamak wall studies• radiation damage, erosion• hydrocarbon contamination• high flux & not much on chemistry• overlap with LLNL interests• PAHs - NASA / Ames Astrobiology Inst.• Formation & destruction of largenumer of PAHs at low energies• IR spectroscopy of individual PAHs(large data base)• excellent resource for predictingastronomical spectra• Hydrogenated Amorphous Carbon• low energy He+ Cosmic Rays (Strazullaet al 2005)• no detailed chemistry (only IR spectr.)• apply new LLNL technology(Superconducting Tunnel Junction X-raySpectrometer at the Advanced Light Source)Surface physics in TokamaksBringa et al 2004wall material atomwall material ionD,T neutralsD,T ionselectronsblisteringpermeation radiation damage(vacancy and interstitial clusters)chemicalsputteringre-emissiondissociationionizationrecycling(redeposition)implantationelectronemissionreflectionionizationphysicalsputteringcore plasmacontaminationdiffusion diffusionLaboratory IR spectra of PAHsNASA / Ames Astrochemistry LabNaphtalenehttp://web99.arc.nasa.gov/~astrochm/pahdata/index.html3.3 micronPrevious and ongoing workon carbonaceous materialshttp://www.astro.ucla.edu/~wright/dust/Fractal dust grain Interstellar shocks accelerate dust grains tovery large velocities (100 km/s) Use lasersto simulate high velocity impactsDetermine how grain properties and sizedistribution changeNIF Target ChamberLaser beamsCollisions compress, break up, melt dust grains:`nano-diamonds! & `black diamonds!www.pbs.org/wgbh/nova/diamonds/sky.htmlCarbonados (Black diamonds)Laser dust dynamics experiments (?)Astrophysics & Space TechnologyLaser dust dynamics experiments (?)Astrophysics & Space Technology J. Hansen et al, LLNLSmall Dust GrainLarge Dust GrainAstrophysics:Grain-grain collisionsSpace Technology:Micrometeorite impactsLaser experiments& debris analysis• Shocks accelerate grainsto typical ~ 100 km/s• Size distribution,structural changes (nano-diamonds ?)• Hypervelocity (> 1km/s) impacts affectspace hardware• Cratering (impactors)not understood HST solar panelsNo craters < 10 micron ?Graham 2001• Mbar pressures, picosectime, sub-micron particles• Accelerate grains infoam (10 km/s possible)• Catch in foam reservoirPotentially new LLNL capability in extreme astro-materials scienceLeverages LLNL expertise in lasers, debris analysis, simulationsConclusion• Compelling, broad scientific interest– ISM dust, formation stars/planets/galaxies,energetic feedback• Spitzer, future IR telescopes– ISM dust = new diagnostic• Advanced technologies– Synergy between astrophysics & materialsscience (!astro-materials science")STJ + Advanced Light Source:New application to ISM astro-materials science• Measuring small energy shifts allowscharacterization of chemical changesin materials after irradiation• Has already been shown to work forgraphite like material MgB2• New application for ISM !astro-materials" science: measure CSuperconducting Tunnel JunctionX-ray Spectrometer at the Advanced Light Source00.511.522.533.5180 185 190 195 200ab-plane excitationc-axis excitationBoron absorption [a.u.]Energy [eV]B2O3! bonding" bonding"* anti-bonding!* anti-bondingab-planec-axisMgB• New LLNL developed technology• More sensitive and  higher spectralresolution (10 - 15 eV) thancompeting detectors• Direct access to Advanced LightSource at LBNL (S. Friedrich- LLNL) MgB2

Galaxies, Black Holes & Laboratories: Studies of interstellar medium materials in energetic environments

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Galaxies, Black Holes & Laboratories: Studies of interstellar medium materials in energetic environments

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