%0 Journal Article %1 Zolotov2001 %A Zolotov, M. Y. %A Shock, E. L. %D 2001 %J Icarus %K imported %N 2 %P 323--337 %T Stability of condensed hydrocarbons in the solar nebula %V 150 %X Thermodynamic calculations of metastable equilibria in the H-C-O system are used to evaluate the stability of condensed polycyclic aromatic hydrocarbons (PAHs) and normal alkanes in the solar nebula. The effects of temperature, total pressure (governed by H-2), the abundances of gaseous CO and H2O, as well mass accretion rate into the Sun and viscous efficiency at the nebula midplane are explored. We show that the inhibited formation of graphite and methane permits metastable existence of hydrocarbons with respect to the inorganic gases H-2, CO, and H2O, Low temperatures, high pressures, high abundances of CO, low abundances of H2O, low accretion rates, and low viscous efficiencies favor stability of hydrocarbons. Condensed PAHs are stable relative to nominal abundances of the inorganic gases at temperatures below similar to 450 K depending on the physical parameters adopted for the nebula. Normal alkanes with carbon numbers > 10 are stable at temperatures 30-60 degrees lower, During the evolution of the nebula, hydrocarbons have a thermodynamic potential to form in a narrow zone, which moved toward the Sun as the accretion rate decreased. At radial distances of 2-4 AU, hydrocarbons had a potential to form at the time when the accretion rate was 10(-6.3)-10(-7.7) solar mass yr(-1), depending on the viscous efficiency. High temperature, low pressure, and a high CO/H2O ratio in the nebula increase the stability of PAHs compared with their alkylated versions and relative to their aliphatic counterparts with the same carbon number. The calculations reveal the thermodynamic possibility for nebular Fischer-Tropsch type (FTT) synthesis of condensed hydrocarbons on the surface of mineral grains from CO and H-2 in an H2O-depleted and/or CO-rich environment. (C) 2001 Academic Press.

@article{Zolotov2001, abstract = {Thermodynamic calculations of metastable equilibria in the H-C-O system are used to evaluate the stability of condensed polycyclic aromatic hydrocarbons (PAHs) and normal alkanes in the solar nebula. The effects of temperature, total pressure (governed by H-2), the abundances of gaseous CO and H2O, as well mass accretion rate into the Sun and viscous efficiency at the nebula midplane are explored. We show that the inhibited formation of graphite and methane permits metastable existence of hydrocarbons with respect to the inorganic gases H-2, CO, and H2O, Low temperatures, high pressures, high abundances of CO, low abundances of H2O, low accretion rates, and low viscous efficiencies favor stability of hydrocarbons. Condensed PAHs are stable relative to nominal abundances of the inorganic gases at temperatures below similar to 450 K depending on the physical parameters adopted for the nebula. Normal alkanes with carbon numbers > 10 are stable at temperatures 30-60 degrees lower, During the evolution of the nebula, hydrocarbons have a thermodynamic potential to form in a narrow zone, which moved toward the Sun as the accretion rate decreased. At radial distances of 2-4 AU, hydrocarbons had a potential to form at the time when the accretion rate was 10(-6.3)-10(-7.7) solar mass yr(-1), depending on the viscous efficiency. High temperature, low pressure, and a high CO/H2O ratio in the nebula increase the stability of PAHs compared with their alkylated versions and relative to their aliphatic counterparts with the same carbon number. The calculations reveal the thermodynamic possibility for nebular Fischer-Tropsch type (FTT) synthesis of condensed hydrocarbons on the surface of mineral grains from CO and H-2 in an H2O-depleted and/or CO-rich environment. (C) 2001 Academic Press.}, added-at = {2009-11-03T20:21:25.000+0100}, author = {Zolotov, M. Y. and Shock, E. L.}, biburl = {https://www.bibsonomy.org/bibtex/243165cc64aa77d4e64ab9a10870b9d1a/svance}, citedreferences = {AIKAWA Y, 1998, FARADAY DISCUSS, V109, P281 ; ALEXANDER CMO, 1998, METEORIT PLANET SCI, V33, P603 ; ALLAMANDOLA LJ, 1989, APJS, V71, P733 ; ANDERS E, 1973, Science, V182, P781 ; ANDERS E, 1974, ASTROPHYS J, V192, L101 ; BASILE BP, 1984, ORG GEOCHEM, V5, P211 ; BELL KR, 1997, ASTROPHYS J 1, V486, P372 ; BELL KR, 2000, PROTOSTARS PLANETS, V4, P1019 ; BOHME DK, 1992, CHEM REV, V92, P1487 ; BRADLEY JP, 1984, Science, V223, P56 ; BRADLEY JP, 1994, GEOCHIM COSMOCHIM AC, V58, P2123 ; BREARLEY AJ, 1990, GEOCHIM COSMOCHIM AC, V54, P831 ; CAMERON AGW, 1995, METEORITICS, V30, P133 ; CHANG S, 1978, LUNAR PLANET SCI, V9, P157 ; CHRISTOFFERSON R, 1984, LUN PLAN SCI 15, P152 ; CLEMETT SJ, 1993, Science, V262, P721 ; CRONIN JR, 1988, METEORITES EARLY SOL, P819 ; CRONIN JR, 1990, GEOCHIM COSMOCHIM AC, V54, P2859 ; CRONIN JR, 1993, CHEM LIFES ORIGINS, P209 ; CYR KE, 1998, Icarus, V135, P537 ; CYR KE, 1999, J GEOPHYS RES-PLANET, V104, P19003 ; DAYHOFF MO, 1964, Science, V146, P1461 ; DAYHOFF MO, 1967, NASA ; EBEL DS, 2000, GEOCHIM COSMOCHIM AC, V64, P339 ; EBERHARDT P, 1998, COSPAR C, V10 ; ECK RV, 1966, Science, V153, P628 ; ENGEL S, 1990, Icarus, V85, P380 ; FEGLEY B, 1988, WORKSH OR SOL SYST, P51 ; FEGLEY B, 1989, FORMATION EVOLUTION, P171 ; FEGLEY B, 1993, CHEM LIFES ORIGINS, P75 ; FERRANTE RF, 2000, Icarus, V145, P297 ; GALUSZKA J, 1992, J CATAL, V136, P96 ; GRADIE J, 1989, ASTEROIDS, V2, P316 ; GREVESSE N, 1993, ORIGIN EVOLUTION ELE, P15 ; GROSSMAN L, 1972, GEOCHIM COSMOCHIM AC, V36, P597 ; GROSSMAN L, 1974, REV GEOPHYS SPACE PH, V12, P71 ; GURVICH LV, 1989, THERMODYNAMIC PROPER ; HAHN JH, 1988, Science, V239, P1523 ; HARTMAN H, 1993, ORIGINS LIFE, V23, P221 ; HARTMANN L, 1993, PROTOSTARS PLANETS, V3, P497 ; HAYATSU R, 1977, GEOCHIM COSMOCHIM AC, V41, P1325 ; HAYATSU R, 1980, Science, V209, P1515 ; HAYATSU R, 1981, TOP CURR CHEM, V99, P1 ; HELGESON HC, 1993, GEOCHIM COSMOCHIM AC, V57, P3295 ; HELGESON HC, 1998, GEOCHIM COSMOCHIM AC, V62, P985 ; JOBLIN C, 1997, PLANET SPACE SCI, V45, P1539 ; JONES TD, 1988, THESIS U ARIZONA TUC ; KELLNER CS, 1981, J CATAL, V67, P175 ; KERRIDGE JF, 1983, EARTH PLANET SC LETT, V64, P186 ; KERRIDGE JF, 1987, GEOCHIM COSMOCHIM AC, V51, P2727 ; KOLODNY Y, 1980, EARTH PLANET SC LETT, V46, P149 ; KOVALENKO LJ, 1992, ANAL CHEM, V64, P682 ; KRESS M, 2000, ASTROCHEMISTRY MOL C, V197, P537 ; KRESS ME, 2001, METEORIT PLANET SCI, V36, P75 ; KRISHNAMURTHY RV, 1992, GEOCHIM COSMOCHIM AC, V56, P4045 ; KROT AN, 2000, PROTOSTARS PLANETS, V4, P1019 ; KUNG CC, 1979, EARTH PLANET SC LETT, V46, P141 ; LEWIS JS, 1974, Science, V186, P440 ; LEWIS JS, 1979, ASTROPHYS J, V234, P154 ; LEWIS JS, 1979, Icarus, V37, P190 ; LEWIS JS, 1980, ASTROPHYS J, V238, P357 ; LLORCA J, 1998, METEORIT PLANET SCI, V33, P243 ; LLORCA J, 2000, METEORIT PLANET SCI, V35, P841 ; LUQUE FJ, 1998, AM J SCI, V298, P471 ; MEIBOM A, 2000, Science, V288, P839 ; MENDYBAEV RA, 1986, GEOCHEM INT, V23, P105 ; MESSENGER S, 1998, ASTROPHYS J 1, V502, P284 ; MOREELS G, 1994, ASTRON ASTROPHYS, V282, P643 ; MOROZ LV, 1998, Icarus, V134, P253 ; ORO J, 1965, ORIGINS PREBIOLOGICA, P133 ; PERING KL, 1971, Science, V173, P237 ; PETAEV MI, 1998, METEORIT PLANET SCI, V33, P1123 ; PRINN RG, 1981, ASTROPHYS J, V249, P308 ; PRINN RG, 1989, ORIGIN EVOLUTION PLA, P78 ; RICHARD L, 1998, GEOCHIM COSMOCHIM AC, V62, P3591 ; SAGAN C, 1979, Nature, V277, P102 ; SAGAN C, 1993, ASTROPHYS J, V414, P399 ; SALAMA F, 1996, ASTROPHYS J 1, V458, P621 ; SCHULZE H, 1997, ASP C SER, V122, P397 ; SHOCK EL, 1988, Geology, V16, P886 ; SHOCK EL, 1989, Geology, V17, P572 ; SHOCK EL, 1990, Nature, V343, P728 ; SHOCK EL, 1992, ORIGINS LIFE, V22, P67 ; SHOCK EL, 1994, ORGANIC ACIDS GEOLOG, P270 ; SHOCK EL, 1998, J GEOPHYS RES-PLANET, V103, P28513 ; SIMONELLI DP, 1989, Icarus, V82, P1 ; STEIN SE, 1978, J PHYS CHEM-US, V82, P566 ; Stevenson DJ, 1988, Icarus, V75, P146 ; STUDIER MH, 1965, Science, V149, P1455 ; STUDIER MH, 1968, GEOCHIM COSMOCHIM AC, V32, P151 ; STUDIER MH, 1972, GEOCHIM COSMOCHIM AC, V36, P189 ; THOMAS KL, 1995, GEOCHIM COSMOCHIM AC, V59, P2797 ; TINGLE TN, 1991, METEORITICS, V26, P117 ; UREY HC, 1953, 13 INT C PUR APPL CH, P188 ; VANZEGGEREN F, 1970, COMPUTATION CHEM EQU ; WOOD JA, 1988, METEORITES EARLY SOL, P328 ; WOOD JA, 1996, METEORIT PLANET SCI, V31, P641 ; YANG J, 1983, GEOCHIM COSMOCHIM AC, V47, P2199 ; YUEN G, 1984, Nature, V307, P252 ; YUEN GU, 1990, LUNAR PLANET SCI, V21, P1367 ; ZEBONI RJM, 1992, GEOCHIM COSMOCHIM AC, V56, P2899 ; ZIEGENBEIN D, 1980, NEUES JB MINERALOGIE, V7, P289 ; ZOLENSKY M, 1988, METEORITES EARLY SOL, P114 ; ZOLOTOV M, 1999, J GEOPHYS RES-PLANET, V104, P14033 ; ZOLOTOV MY, 2000, J GEOPHYS RES-SOL EA, V105, P539 ; ZOLOTOV MY, 2000, METEORIT PLANET SCI, V35, P629}, interhash = {07ebea2b5e1cdbc1e9a12febcbb20495}, intrahash = {43165cc64aa77d4e64ab9a10870b9d1a}, journal = {Icarus}, keywords = {imported}, number = 2, owner = {svance}, pages = {323--337}, timestamp = {2009-11-03T20:22:21.000+0100}, title = {Stability of condensed hydrocarbons in the solar nebula}, volume = 150, year = 2001 }