Chemical effects on ices: studies with a chemo-dynamical model

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Jeong-Eun Lee Kyung Hee University University of Texas at Austin. Chemical effects on ices: studies with a chemo-dynamical model. Contents:. Very Low Luminosity Objects ( VeLLOs , L


Chemical Evolution of Very Low Luminosity Objects (VeLLOs)Chemical effects on ices:studies with a chemo-dynamical modelJeong-Eun LeeKyung Hee UniversityUniversity of Texas at AustinContents:Very Low Luminosity Objects (VeLLOs, L 50 KFormation of pure CO2 ice requires at least 20 K.Pure CO2 ice formation is an irreversible process.Pure CO2 Ice FormationLaboratory DataCO2:H2O mixture, CO:CO2 mixture (Ehrenfreund et al. 1997)Only the pure CO2 ice (van Broekhuizen et al. 2006) component has double peak.Laboratory data from Leiden Observatory data base.Pure CO2 iceDust Temperature is Too LowThe envelope around low luminosity protostars with 0.6 L does NOT have a dust temperature higher than 20 K to form the pure CO2 ice.If we can detect the pure CO2 ice feature around low luminosity protostars, then it can be an evidence of the past high accretion rate!Radius (AU) Dust Temperature (K)CO evaporation temperatureObservationCO2 ice with Spitzer/IRS SH mode (R=600)19 low luminosity protostars with Lint < 0.7 L (PI: M. Dunham)18 of them have Lint < 0.6 L.3 of them have Lint < 0.1 L. 50 higher luminosity protostars with Lint > 1 L (c2d: Pontoppidan et al. 2008)C18O (J = 21; 219.560352 GHz) toward 11 low luminosity protostars at CSO.Kim et al., 2012Pure CO2 Ice Detections at Low Luminosity ProtostarsSix low luminosity embedded protostars show significant double peaks caused by the pure CO2 ice . Three more sources show evidence of pure CO2 ice.Column Density is calculated CB68SSTc2d J125342.9-771511.5 CB130-1SSTc2d J032845.3+310542.0SSTc2d J032923.5+313329.50.15 L0.54 L0.14 L0.26 L0.20 LComponent Analysis with Laboratory DataPure CO2 iceWater-rich CO2 iceCO-CO2 mixtureInternal luminosity of IRAM 04191+1522 is 0.08 L, but it has the pure CO2 ice component. The source had higher temperatures than the dust temperature derived from the current SED.Double peak comes from the pure CO2 ice componentTotal CO2 iceIRAM 04191+1522Tests with Chemo-dynamical ModelsChemo-dynamical modelsContinuous accretion + chemical network without surface chemistryContinuous accretion + CO to CO2 ice conversionEpisodic accretion + chemical network without surface chemistryEpisodic accretion + CO to CO2 ice conversionKim et al., 2012Result: C18O gasKim et al., 2012Result: CO2 iceKim et al., 2012Best FitCaveat; No explicit surface chemistryInclusion of surface chemistry explicitly using rate equationsWillacy et al. (2006), Garrod and Herbst (2006), Dodson-Robinson et al. (2009), Yu et al. (in prep.)ad hoc approximation vs. explicit surface chemistryad hoc approximationExplicit surface chemistryBranching ratio between CO ice and CO2 ice = 0.5 : 0.5CO + grain gCO (50%) or gCO2 (50%)COCO2H2OAKARI spectrum of a low luminosity sourceJ034351.02+320307.9 (L=0.33 L, Dunham et al. 2008)COCO2H2OICESContinuous accretionEpisodic accretionFurther constraints forepisodic accretionALMA observations for the distribution of gaseous moleculesOther ices observed with Spitzer/IRS and AKARIe.g. Boogert et al. (2011)e.g. Noble et al. (2013), Lee et al. (in prep.) SummaryEpisodic Accretion Model can explainpresence of pure CO2 ice in low luminosity protostarslow luminosity itself, strength of molecular lines, and total CO2 ice column density with the ad hoc ice conversion of CO to CO2Surface chemistry must be included more explicitly.Chemo-Dynamical model for the episodic accretion model could be constrained better by existing IR ice spectra and future ALMA observations.Thank you.Boogert et al., 2011Episodic accretion modelwith/without surface chemistryNo surface chemistryWith surface chemistryCO and N2H+ abundancesSo we included the The absolute amount of CO changed, but the relative distribution with radius is the same. Therefore, the ALMA observations of emission distribution of CO gas is still useful to pin down the dynamical process associated with VeLLOs.GO + GCO GCO2 GO + GHCO GCO2 + GHGOH + GCO GCO2 + GHAssume ONLY GH, GC, GN, GO, GS, GH2, GCH, GOH, and GNH are mobile.Grain surface reaction For exothermic reaction without an activation energy : P =1With an activation energy (Ea)b = 1 , r = reduced mass


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