DUST2016, Garching, Sept 2016
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1 Emmanuel Dartois, IAS, Orsay, France Ivan Alata, Markus Bender, Karine Beroff, Marin Chabot, Gustavo A. Cruz- Diaz, Marie Godard, Aurélie Jallat, Rafael Martín-Doménech, Guillermo M. Muñoz Caro, Thomas Pino, Daniel Severin, Christina Trautmann DUST2016, Garching, Sept 2016
2 Outline( Context VUV Hydrocarbons production from a-ch dust Application to DISM Modeling of a PDR CRs SHI of ISM carbonaceous dust grain analogues Lupus 3 dark cloud ESO/F. Comeron(
3 Some carbonaceous solids observed in the ISM (Nano1)( Diamond( Fullerenes( AIBs1PAHs(:(( Class(A(to(C( Amorphous(( carbon( Hydrogenated(( amorphous(carbon( + organic matter Ice(mantles(( residues(
4 Hydrogenated amorphous carbons (a-c:h or HAC) DISM CH stretch abs. observed against IR bkgd sources Viehmann et al. A&A 2004 Pendleton(&(Allamandola(ApJ(2002( Pendleton et al Sun( UGC12158((Credit(NASA/ESA( Dartois,(Geballe,(Pino(et(al.(2007(
5 ISM (ext. galaxies) ***Arom.*CH*UPPER*LIMIT* OBSERVED* IRAS* * OLEF.* OLEF./AROM.* BACKBONE* Dartois,(Geballe,(Pino(et(al.(2007( Precursor Substrate
6 Hydrogenated amorphous carbons (a-c:h or HAC) CH stretch abs. Galactic ISM CH bendings abs. extragalactic DISM Godard et al. 2013, Sandford et al e.g. Sandford et al. 1995, Pendleton et al. ApJ 1994; Duley et al. ApJ 1994, 1998; Dartois et al 1997 τ (3.4)(:( 2.6%(to(35%((lab(HAC)(of(cosmic(C(( Dartois & Munoz Caro 2007 e.g. Risaliti et al. 2006, Imanishi et al. 2006; Mason et al. 2004, 1998; Pendelton et al 1994 τ(6.85)(~(0.12(τ(silicates)( 15%(+17%(of(the((cosmic( carbon( Up(to(40%(in(extreme(cases(?(
7 VUV Hydrocarbons molecules detections C 2, C 3, C 2 H 2, CCH, c-c 3 H 2, C 4 H. PDR: Photon Dominated Regions Top-down chemistry? Dense, cold molecular gas C 2 H C 3 H 2 C 3 H + Pety(et(al.(2005( One-dimensional Photo-Dissociation Region, The Horsehead (PDR) Guzman(et(al.(2015(
8 Objectives Study the evolution of a-c:h under simulated ISM conditions Interaction with VUV photons & Cosmic rays MgF 2( Cutoff( 115nm( Lyman-alpha nm LABORATORY* < E photon > = 8.6 ev/photon Ф= 2.7 x photon.cm -2.s -1 Madrid(2013( G.(Adolfo,(G.(M.(Munoz(Caro( ASTRO*MODEL* Chen(et(al.(2014;(Cruz1Diaz(et(al.(2014( Gredel(et(al.(1989( Test astrophysical models with the photoproducts H 2 formation Formation of hydrocarbons in PDRs regions. Astrophysical timescales
9 a-c:h Vacuum*chamber* Experiments T~10K* 45 * IR*Beam** IR*detector* VUV* Diaphragm** Beam*spliUer* RF*cavity* H2* VUV*source* P H2 =*0.75*mbar* I. Alata Bunch*of*ions* Irradiation at T=10 K TPD 5K/min QMS* Quadrupole*Mass* *Spectrometer* P ~ 2x10-8 mbar P ~ mbar
10 To enhance detection limits, both a-c:h and a-c:d analogues Optical depth a- C:D a-c:d a-c:h Number of N (C-H) & N (C-D) a-c:d a-c:h Wavenumber destruction cross-section σ CH (VUV) = 3 ± cm 2 Mennella(et(al.(1999,(2001( Alata(et(al.(2014( Gadallah(et(al.(2011,2013( σ CH (VUV) = 1(to(5( (10 19( cm 2( σ CH (VUV) similar (
11 Mean VUV penetration depth ( nm) measured ~ 80 nm (SOLEIL Synchrotron DISCO Beam line). Formation on the surface & in the volume UV-VUV Post irradiation TPD 5h irradiation then TPD 5K/min D2 Blank exp.
12 Photolytic H 2 formation rate CH abundance( extinction( Yield( Destruction cross-section( VUV photons flux( VUV Rate coefficient
13 VUV H 2 Rate coefficient With 5-10% C locked into a-c:h & PDR: χ/n(h) up to 0.25 R c up to cm 3 s -1 This(mechanism(can( provide(high(h 2 ( formadon(rates(at(low( to(high(grain(t( Habart(et(al.(2004(
14 Other photolytic products: CD 4 C 2 D y C 3 D y C 4 D y a-c:d Alata(et(al.(2015;(Jallat(2015(
15 CH 4 C 2 H y C 3 H y C 4 H y a-c:h Alata(et(al.(2015;(Jallat(2015(
16 Model(implementadon:( a1c:h(+(vuv(photon(!(a1c:h(+(c x H y (( Photoproduced ( ( (Yield( ( ( ((((Photolydc(rate( species ( ( ( ( ((%) ( ( ( ( ((10 14 s 1 )(( ( H 2 ( ( ( ( ( ( (96.5(((±3.0)( ( ( (2.79( (10 3 (( } CH 4 ( ( ( ( ( (3.0((((±1.0)( ( ( (86( Model(I( C 2 H 2 ( ( ( ( ( (0.081((((±0.060) ( (2.3(( C 2 H 4 ( ( ( ( ( (0.195((((±0.072) ( (5.6(( C 2 H 6 ( ( ( ( ( (0.246((((±0.063) ( (7.1(( } Model(II( C 3 H 4 ( ( ( ( ( (0.042((((±0.036) ( (1.2(( C 3 H 6 ( ( ( ( ( (0.114((((±0.057) ( (3.3(( C 3 H 8 ( ( ( ( ( (0.075((((±0.060) ( (2.2(( C 4 H 4 ( ( ( ( ( (0.009( ( ( ( (1( C 4 H 6 ( ( ( ( ( (0.027( ( ( ( (1(( C 4 H 8 ( ( ( ( ( (0.027( ( ( ( (1( C 4 H 8 ( ( ( ( ( (0.027( ( ( ( (1( } Model(III( Alata(et(al.(2015;(Jallat(2015(
17 1st step Meudon Code: Le(Pedt(et(al.(2006( Radiative transfer + Chemical reactions + Thermal balance A. Jallat Horsehead(nebula( T( (100(K(( n H ( ( (cm3(( χ( (60(Draine(units(( ζ(=( (s 11 ( [S]/n H (=(3.5x10 16 (( N H (cm -3 )* Distance to the star*
18 2nd step Nahoon Code: Wakelam(2006( Time dependence of a-ch perturbation Abundance / N H* C 4 H* +a-c:h photolysis* Initial* Abundance ratio* Distance to the star*
19 Abundance( Abundance ratio( CCH( c-c 3 H( C 4 H( c-c 3 H 2( PDR advection front velocity: ~ 1 km/s Alata(et(al.(2015;(Jallat(2015( d(0.5a V ) ~ cm, equivalent to yrs
20 Take home message VUV Bulk of the interstellar grains as important as surface a-c:h (& polyaromatic dust of AIBs-PAHs) photolytic reactions! formation of H 2 & hydrocarbons in the ISM Reduce gap between observed and modeled hydrocarbons abundances in PDRs Destruction timescale! in line with PDR advection front velocity (1 km/s) Models chemical network! include highly hydrogenated hydrocarbon species.
21 CRs(in(Diffuse(ISM(&(clouds:( ( (( ( ( (SHI(of(ISM(carbonaceous(dust((grain(analogues( Top-down chemistry? Dense, cold molecular gas C 2 H C 3 H 2 C 3 H + Pety(et(al.(2005( One-dimensional Photo-Dissociation Region, The Horsehead (PDR) Guzman(et(al.(2015(
22 GSI (Darmstadt) QMS* Quadrupole*Mass* *Spectrometer* IR*detector* Ion*Beam** a[c:h* 45 * Ion*Beam** VUV* Vacuum*chamber* Mass spectrometer a-c:h sample Irradiation at T= K + TPD 5K/min FTIR a-c:h sample Ion Beam
23 IR monitoring cross section of the solid phase processing Xe 0.6 GeV
24 H 2 CH 4 C 2 H y C 3 H y C 4 H y a-c:h Dartois(et(al.(submived(to(A&A( Ion*Beam** Cosmic rays release carbonaceous species Feeds the ladder of large gaseous C species
25 GSI (Darmstadt) 300K QMS* Ion*Beam** Post Irradiation TPD 5K/min 100K 40K
26 Dartois(et(al.(2016(submived(to(A&A(
27 Xe 0.6 GeV
28 Dartois(et(al.(2016(submived(to(A&A(
29 Relative abundance f (Z) Atomic number Z Φ(Z,E) Φ(Z,E) MeV/nucleon
30 Se(Z,E) f (Z) σ(z,e)(=(σ(se(z,e))( + η(se) Φ(Z,E) R GCR( d [s 11 ]=( ( (σ(z,e) f(z)(φ(z,e) de( CR
31 R d GCR [s -1 ] 8x10-16 s -1 (for ζ = 3.5x10-16 s -1 ) n X n tot a few η(x) e τ d f[n(x)] Diffuse medium (τd << 1) CR insufficient to be significant high energy CR penetrates deep in dense regions Photodissociation e τd! secondary UV induced (10 3/10-4 at AV > 7) abundance increases to values closer to observations and models (Guzmán et al. 2015; Alata et al. 2015; Pety et al. 2012).
32 One(more(slide ( " SHI in CR, desp. low abundance, have a role to play " CRs less significant for a-c:h in DISM " CRs induce a top-down chemistry for refractory dust grains in dense clouds " CRs radiolysis participate to the erosion of icy grains see poster by C. Jäger Sabri(et(al.(2015( " CRs participate to the replenishing of the dense cloud gas phase by ice e- sputtering e.g(dartois(et(al.(2013;( Rothard(et(al.(2016( " Lab eval needed, many space processes are concomitant (CRs, surface, thermal, UV, shocks ) Fantasdc(4(
33 I.(Alata( L.(Gavilan( E.(Dartois(( A.(Jallat((( M.(Chabot( G.(M.(Muñoz(Caro( G.(A.(Cruz(Diaz( T.(Pino( K.(Beroff(( R.(Mar n1doménech( M.(Bender( D.(Severin( C.(Trautmann(( Thank you! M.(Godard(
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