SL?u4?u8 @@@ @@@@ BZsLx?u0 k?u< EN DB ?u@ :    & ./ h@ Xx    ;]  PW Z&H 7 N D o V [  $   v9 1 h HNVL6B. C. C. Porco1993,> Cruikshank1994l Fanale199797 Hubbard1993|g Lunine20030P Pointu19821D Sims19979Ocntl%$Pcntl :cntlDcntl Zcntl?PcntlVcntl)f cntlV`Acntl%0cntl*cntl/Wcntl>cntlj"Fcntli+cntlh@cntlg!YcntlfCcntle@cntl3Ґcntl@cntl0cntl/A cntl(cntl`cntl *cntl @cntl #]cntl &cntl vcntlhcntl*|pcntlŰcntl Pcntl$P`cntl.acce,@acce*!hacce)>acce6acce{acceacceacce!8acce!3} Singh1995 Singh1996 Sirdey1997rK Sisay2002 Sklarew1981a Slade1990u Sloan1996 Smilowitz1999 Smith1982 Smith1982i Smith1983 Smith1991 Smith19964 Smith1997< Smith1999 Smith1999 Smith1999 Smith1999 Smith2000& Smith2000 Smith2002 Smith2003 Smith2003 Smith2004 Smyth1981 Smythe19977 Soderblom2002 Somogyi2003 Speller1982 Speller1995 Speller1995 Spitzer2000 Spliker1997 Sromovsky1981 Stansberry1989za Stern2003U Sternberg1993 Sternberg1996 Sternberg1997 Sternberg2001 Stevenson19839 Stevenson1984 Stevenson1985 Stevenson1985 Stevenson1986Q Stevenson1987 Stevenson1992 Stief1989 Stoker1990 Stone1992 Strazzulla1993z  Strobel1974 Strobel1982 Strobel1982 Strobel1982! Strobel1985" Strobel1992> Strobel2004 Strong19929 Stumptner2001) Stumptner2001 Sugita20042 Suits1984" Summers1992# Svedhem2004Sweetnam1983p Swindle2002 Szopa2001$T. Fusco20010V T. Hidayat2002 T. Owen19815 T. Owen19976 T. Owen19982 T. Owen2003d T. R. Geballe19962 T. R. Geballe2003 T. Scattergood1988v T. Vo-Dinh19931= T.A. Callott1984 Takahashi2001 Takano20030. Tang19939 Tanguy1990# Taviani2001Teixeira19989! Th. de Graauw1998 Th. Encrenaz1993! Th. Encrenaz1998G Thinh1995 Thissen2004Thompson1984p$Thompson19840OThompson1984Thompson1985@%Thompson19850Thompson1989pThompson1991pThompson1991p&Thompson1991pThompson1992pThompson1992pThompson1992p'Thompson1992pThompson1993pThompson1994pThompson1994pThompson1994pThompson19959 Thouvenot1990 Tielens1998 Tipping1983 Tokano2001( Tokano2001) Tokano2001z Tolbert20002 Tolbert2004 Tomasko1982 Tomasko1989 Tomasko1992K Tomasko1993* Toon1980t+ Toon1988B Toon1992 Toon19922: Toon1993a Toon2000$ Toon20033% Toon200442 Toon20040,Toublanc1995pToublanc19999Toupance1975Toupance1982p Touzeau1999- Trafton1972. Trafton1974/ Trafton19750 Trafton19751 Trafton19782 Trainer2004 Tran2003h Tran200303 Tran20034 Traub20034 Travers1997# Trotta1999a Tse2001Tsuchiya19944c Tull1984k Tuminello1993 Tuminello1994 Turco1992* Turcon19805 Tyler1981 Tyler19836 Ulamec1992 Ushio2001 V. E. Suomi1981w V. G. Kunde1981x V. G. Kunde1983/ V. Vuitton2000U V.G. Kunde19811 Vacher19955 Vacher199557 Vacher19978 Vacher19999 Vacher2000 Valenca1998Valentin19879: Valero19838; Valero19838< Valero19838 Van Ghyseghem1988N Vann20040; Vanssay1995JVapillon20011:Varanasi19830;Varanasi1983p<Varanasi1983p:Varanasi19877= Velazquez1991J Veran2001 Vertes19988> Vervack2004 Vidal-Madjar1996@ Vidal-Madjar1997@ Vidal-Madjar20012 Volpi2001 Votaw1987 Vuitton2000? Vuitton2001r Vuitton2002h Vuitton2003@ Vuitton20037 W. Beisker1993oB W. C. Maguire1981x W. C. Maguire1983c W. D. Cochran1984W. K. Hartmann19919W. R. Thompson1987W. R. Thompson1992W. R. Thompson1992vW. R. Thompson1993W. T. Huntress1981 W. Thuillot19907 W. Thuillot1993 W.J.Borucki1989{ Wagener1991A Watson1963 Way2002 Welch2003 Welge1993 Wenkert1986 Werner20000 West1983 West1991 Western1993 Whited199695 Whitten1976 Whitten1983 Whitten1984K Wilhite2002L Wilhite2003Williams1984p Willingham1984 Wilson19999 Wilson19999B Wilson2000C Wilson2002 Wilson2003 Wilson20033 Wilson20044D Wilson2004E Wishnow2002 Wittemberg1997z Woeller1969J Woillez2001 Wong19808F Wong200265 Wood19818 Wood19838Q Woodman1978uWoodward199602 Worsnop2004( Wright19929V Y. Biraud2002x Y. L. Yung198317 Y. Nevo1993Yamamoto19944 Yamanashi2001Yanagawa19971 Yelle1991 Yelle1997 Yelle2002 Yelle2003GYomogida19950w Young1999 Young2002N Yu20040f Yung1980n Yung19800 Yung1983H Yung1984I Yung1988 Yung1999 Yung19999 Yung20008F Yung20020Z. Levin1987P Zabka2004 Zahnle2003 Zare19979 Zare20040(Zarnecki19920)Zarnecki1992p#Zarnecki20040a Zhang2003" Zhu1992' Zollweg1992J Zubrin1992 Zumberge1981p992 Zumberge1981pZumberge1981p Zumberge1981p Zumberge1981p992 Zumberge1981pZumberge1981p1992 Zumberge1981p992 Zumberge1981p992 Zumberge1981pZumberge1981pZumberge1981p992 Zumberge1981p Zumberge1981p Zumberge1981p1992 Zumberge1981pin1992 Zumberge1981p992 Zumberge1981p1992 Zumberge1981p Zumberge1981pZumberge1981p Zumberge1981p1992 Zumberge1981p Zumberge1981p Zumberge1981p Zumberge1981p Zumberge1981p Zumberge1981p Zumberge1981pZumberge1981p2 Zumberge1981p Zumberge1981p Zumberge1981p Zumberge1981p1992 Zumberge1981pZumberge1981p Zumberge1981p992 Zumberge1981pZumberge1981p Zumberge1981p Zumberge1981pZumberge1981pZumberge1981p Zumberge1981pZumberge1981p2 Zumberge1981p Zumberge1981pZumberge1981pZumberge1981pZumberge1981pZumberge1981p Zumberge1981p20007 W. Beisker1993oB W. C. Maguire1981x W. C. Maguire1983c W. D. Cochran1984W. K. Hartmann19919>W. R. Thompson1984W. R. Thompson1987W. R. Thompson1992W. R. Thompson1992vW. R. Thompson1993W. R. Thompson1993W. R. Thompson1994W. T. Huntress1981 W. Thuillot19907 W. Thuillot1993 W.J.Borucki1989 W.R. Thompson1991W W.R. Thompson1994) W.R.Thompson19951 Wagener1991 Welch2003 West1983 West1991 Whited199695 Whitten1976 Whitten1983 Whitten1984Williams1984pWilliams1984p Willingham1984 Wilson2003 Wilson20033 Wilson20044 Wittemberg1997z Woeller1969 Wong19808( Wright19929V Y. Biraud2002x Y. L. Yung198317 Y. Nevo1993 Yelle1991 Yelle1997 Young2002 Young2002 Yung1980tf Yung1980n Yung19800P Yung1983v Yung1984 Yung1999Z. Levin1987P Zabka2004 Zahnle2003 Zare19979 Zare20040(Zarnecki19920)Zarnecki1992p Zhu1992 Zumberge1981pYPV\NaOcXdeRfhijl[mnopqrst!7^u%vxy=_{~4L/< 6w29D 5TJIG+* "#-@F30'  ( !"#$%&'*+&,-SBHM/.1A)36795;<=>>@?ADFHJMCNQRST AuthorsIJournals zKeywords iG                               ?uH  L A. Brahic A. C. Aikin* A. Coustenis A. da Silva* A. J. Hollis A. Khelifi(* A. KlotzA. L. Broadfoot A. L. Cochran A. L. Lane(* A. L. Summers A. M. Altbuch A. Marten A. SalamaA. W. Grossman A.Coustenis*A.T. BasilevskyAbd Elkhalk, H.PAckerman, Thomas P.Adamkovics, MatePAdams, Nigel G.P Aflalaye, A. Aikin, A. C.Alcaraz, Christian Algatti, M. A.P Allan, R. Allen, M. Allen, Mark*Allison, M. D. Amsif, A.Anderson, C. M.PAnderson, J. D.PAnderson, John D. Anguel, S.(*Anicich, V. G.PAnicich, Vincent G. Arai, N.Arakawa, E. T.Arakawa, Edward T. Arie, E.$Aronowitz, Sheldon  Artemieva, N.Ashfold, M. N. R. Atreya, S. K.Atreya, Sushil K. Awal, M.Aylward, A. D.P B. A. Smith* B. Bezard B. J. Butler B. N. Khare* B. Nagy B. R. Sandel B. Rizk B. Schmitt(* B. Schulz B. Sicardy(* B.Khare B.N. Khare(* B.N.Khare B.NagyZBabcock, Lucia M. Badoz, J. Baillion, M.Baines, Kevin H.P Bakes, E. L.Bakes, E. L. O.Bakes, Emma L. O. Balucani, N.Banaszkiewicz, M. Bar-Nun, A.*Bar-Nun, AkivaPBarbieri, RobertoBarth, Erika L.P Bauer, S. J. Bauschlicher, Charles W., Jr.$Baushchlicher, Charles W., Jr.Beauchamp, J. L.PBeauchamp, Patricia M.(+L Bell, J. F.*Belmonte, S. A.P Benilan, Y.* Benilan, Yves Benitez, P.*Bennett, Chris J. Benson, R.(*Benson, RobertP Bergeat, A.*Bergstralh, Jay T. Bernard, J. M.P Bezard, B.(* Biemann, K.*Biller, Elinor D. Billiotte, M.Biondi, Manfred A. Birchley, P. N. W.  Bird, M. K.* Bjoraker, G. Blass, W. E. Blass, W.E.* Block, B. Boac, D. S.* Bockelee-Morvan, DominiqueBoering, Kristie A. Bohme, D. K. Bohn, R. B.* Bondar, A.(* Boon, J. J.*Borowski, Stanley K.Bortoleto, J. R. R.Borucki, W. J. Borucki, W.J.Borucki, William J. Borysow, A.*Borysow, Aleksandra Bossard, A.*Bossard, AlainP Boston, P. J.Bouchez, Antonin H. Boussin, C.*Bowyer, StuartP Brandner, W. Brault, James Brillet, J.*Broadfoot, A. L.PBrown, HarrisonPBrown, Lisa L.PBrown, Michael E.Brown, Robert Hamilton(+L Brull, C. Bruston, P.* Bruston, PaulBudil David, E.PBudil, David E.PBugaenko, L. A.PBurgdorf, M. J.P Buvet, R.C. A. Griffith C. Bittner(* C. Blanco C. Buil C. Buile C. C. Porco* C. Chyba C. de Bergh*C. Er C. Ferrari(* C. MeisseC. N. Matthews C. P. McKay* C. SaganC. W. Bauschlicher Jr.(+LC. W. Bauschlicher, Jr.+L C. W. Hord(* C.M. Anderson C.P. McKay(* C.P.McKay C.Sagan Cabane, M.(*Cabane, MichelP Calado, JorgeCaldwell, JohnPCallcott, T. A.PCameron, A. G. W. Canosa, A.(* Cao, Hong Capilla, P.* Capone, L. A. Capone, L.A.Carignan, G. R.P Carle, G. C.Carlson, R. W.PCartechini, L.PCasavecchia, Piero Casson, Joanna L.Cataldo, FrancoP Cernogora, G. Cess, R. D.*  5hbAbstracts of Papers, 220th ACS National Meeting, Washington, DC, United States, August 20-24, 2000/XhbAbstracts of Papers, 225th ACS National Meeting, New Orleans, LA, United States, March 23-27, 2003/XhdAbstracts of Papers, 228th ACS National Meeting, Philadelphia, PA, United States, August 22-26, 2004|Abstracts, 31st Northeast Regional Meeting of the American Chemical Society, Saratoga Springs, NY, United States, June 15-18Accounts Chem. Res. Accounts of Chemical ResearchAdv. Space Res.3Adv. Space. Res. Advances in Space ResearchDB\YAdvances in space research : official journal of the Committee on Space Research (COSPAR) AIP Conference ProceedingsDB American Journal of PhysicsDBAnalytical ChemistryAnn. GeophysicaeAnnales Geophysicae Ap. J.Applied Physics LettersP Astrobiology Astrometriya i AstrofizikaBBAstron. Astrophys. Astronom. J.Astronomical and Biochemical Origins and the Search for Life in the Universe, Proceedings of the International Conference on Bioastronomy, 5th, Capri, Italy, July 1-5, 1996l85Astronomical Society of the Pacific Conference Series Astronomy and AstrophysicsDB Astrophys. J.Astrophys. J. Supp.Astrophysical Journal,(Astrophysical Journal, Supplement Seriesp$Astrophysics and Space Science(U,&Astrophysics and Space Science Libraryp$Biochem. Biophys. Res. Commun.(ULFBook of Abstracts, 218th ACS National Meeting, New Orleans, Aug. 22-26PBull. Am. Astron. Soc. Can. J. Chem. Canadian Journal of Chemistry Canadian Journal of PhysicsDB Chemical & Engineering NewsBB0*Comments on Astrophysics and Space Physics (%Communications in Theoretical PhysicsDissociative Recombination: Theory, Experiment and Applications III, Proceedings of the Workshop, 3rd, Ein Gedi, Israel, May 29-June 2, 1995f Dojin News Doklady Akademii Nauk SSSRDB83European Space Agency, [Special Publication] ESA SP4/European Space Agency, [Special Publication] SP\p40European Space Agency, [Special Publication], SPľExobiology: Matter, Energy, and Information in the Origin and Evoluation of Life in the Universe, Proceedings of the Trieste Conference on Chemical Evolution, 5th, Trieste, Sept. 22-26, 1997First Steps in the Origin of Life in the Universe, Proceedings of the Trieste Conference on Chemical Evolution, 6th, Trieste, Italy, Sept. 18-22, 2000 Geology@Geophys. Res. Lett. Geophysical Research Letters"High Pressure ResearchP Icarus(%International Journal of Astrobiologyeir!!!vv====< 2 5J##-300'"#$$%%&&&&'&&HHHHHH9<>>@AAHRSbbdh@tBFIBT. J K" ((SDU>.%&_, -*& 9L@ 4xN++C0F   ? *Aerosols*Aerosols: AN, analysis*Aerosols: CH, chemistry *Ammonia*Ammonia: CH, chemistryis *AtmosphereH,*Atmosphere: AN, analysis *Atmosphere: CH, chemistry("*Bacteria, Aerobic: ME, metabolism pu($*Bacteria, Anaerobic: ME, metabolism  *BiogenesisAn*Carbon Monoxide*Cosmic Radiation *Electricity *Evolution, Chemicalm *ExobiologyCh*Exobiology: MT, methodsn *Extraterrestrial Environment *Free Radicals: CH, chemistry *Hydrocarbons: AN, analysist *Hydrocarbons: CH, chemistryy*Ice: AN, analysisrad *Jupiteri("*Mass Fragmentography: MT, methods *Methaner*Methane: CH, chemistryio*Models, Chemical *Nitrogen$!*Organic Chemicals: CH, chemistry*Polymers: AN, analysisca*Polymers: CH, chemistryo*Polymers: ME, metabolism *Saturnn:*Soil Microbiologyabo *Solar System *Space Flight *Waterers 0 (Aerosols)l 0 (Amines) Or0 (Amino Acids)ch 0 (Cyanides)R0 (Free Radicals)0 (Hydrocarbons)e 0 (Imines) Or 0 (Ions)o 0 (Nitriles)o0 (Organic Chemicals) 0 (Polymers)h1-dimensional photochem./3-dimensional solar radiative transfer modeling fails to account for the high-latitude HCN-HC3N-C2H2-CH4-N2 photochem. of the Titan atm.)|w15N+ + CD4 and O+ + 13CO2 state-selected ion-mol. reactions relevant to chem. of ionospheres of Titan, Mars, and Venus)85a computational study of the reaction of C2 with CH4)4/a coupled model of Titan's atm. and ionosphere)pa global time-dependent general circulation model for calcg. distribution of constituents in Titan's upper atm./thermosphere due to winds and mol. and eddy diffusion)(.XHEa two-dimensional multifluid MHD model of Titan's plasma environment)XSabiotic synthesis of bioorg. compds. in simulated primitive planetary environments)esAbsorption spectra (IR|vabsorption spectra and absorption coeffs. for methane in 750-940 nm region obtained by intracavity laser spectroscopy)oscD?absorption spectra coeff methane intracavity laser spectroscopy0  Absorptivityg,&abundance deuterated methane atm Titand iHCabundance in Titan's atm. as estd. by exptl. lab. simulation study)ccpmabundances of trace hydrocarbons, CO2, and H2O in Titan's atm. from IR Space Observatory mid-IR spectroscopy)Acetoacetic acid Benzidine Benzidine Carbamic acid Crotonamide Ethanol Hydantoic acid Naphthalene p-Crotonotoluidide (effect on sporulation of Monilinia fructicola)|ponmNHRannou, P., M. Cabane, E. Chassefiere, R. Botet, C. P. McKay, R. Courtin 1995NGTitan's Geometric Albedo: Role of the Fractal Structure of the Aerosolsr Icarus 118o355--3726/Rannou, P., M. Cabane, R. Botet, E. Chassefiere 1997JDA new interpretation of scattered light measurements at Titan's limbJ. Geophys. Res. 102 10997-11013B;Rannou, P., C. Ferrari, K. Rages, M. Roos-Serote, M. Cabaner 2000F@Characterization of Aerosols in the Detached Haze Layer of Titan Icarus 147D267--281*#Rannou, P., F. Hourdin, C. P. McKay  2002.(A wind origin for Titan's haze structure Nature 418853--856RKOrganic syntheses from methane-nitrogen atmospheres: implications for Titan AN 1983:48750A review and discussion with 36 refs. Numerous expts. have already been performed, simulating the evolution of gaseous mixts. contg. CH4 when submitted to energy flux. From their results, it appears that a variety of org. compds., including unsatd. hydrocarbons and nitriles such as HCN, can be synthesized into noticeable amts. from CH4-N2 mixts. After reviewing these expts., implications of the obtained results on the org. chem. at the periphery of Titan are discussed. [on SciFinder (R)]60Raulin, Francois Mourey, Didier Toupance, GerardOrigins of Lifeo123D 267-79 1982ztCAN 98:48750 6-0 General Biochemistry Lab. Phys. Chim. Environ.,Univ. Paris Val de Marne,Creteil,Fr. Journal; General Review 0302-1688 written in English. 7727-37-9 Role: BIOL (Biological study) (org. syntheses from atms. contg. methane and, Titan in relation to); 74-82-8 Role: BIOL (Biological study) (org. syntheses from atms. contg. nitrogen and, Titan in relation to)60Evolution (chem., of methane-nitrogen atm., Titan in relation to); Atmosphere (methane-nitrogen, org. syntheses in, Titan in relation to); Planets (Saturn, Titan satellite of, org. syntheses in atm. of); Synthesis (org., in atm. of Titan) methane nitrogen atm Titan review; review org synthesis atm Titans (Enceladus707d77d08/X `@#(* ^D(+L^DA(-l`(.X(-l(.X/X @#Ӏ0(\p/W^D԰ӰA(<HDsearch parameters for the remote detection of extraterrestrial life)08/X `@#(* ^D(+L^DA(-l`(.X(-l(.X/X @#Ӏ0(\p/W^D԰ӰA(<Satellites (Galileanr the remote detection of extraterrestrial life)08/X `@#(* HANear infrared spectra of potential solids at the surface of TitanAN 1993:172842xrIn the lab. the optical properties in the near IR (1-5 mm) of solid CH4, C2H6 and C2H4 and some of their mixts. were measured. With these data the spectra of three mixts. at a resoln. comparable to the one of the near IR spectrometer of the DISR instrument of the Huygens probe were simulated. At DISR's resoln. the best features to probe the compn. of solid surface on Titan are near 6000, 7500 and 8600 cm-1 for methane, near 7900, 7200 and 8400 cm-1 for ethane and near 6100 cm-1 for ethylene. In some cases concns. lower than a few percent may be derived from the anal. of the complete near-IR spectrum. [on SciFinder (R)]81Schmitt, Bernard Quirico, Eric Lellouch, Emmanuel60European Space Agency, [Special Publication], SP ESA SP-338 Proc. - Symp. Titan, 1991 383-8 1992CAN 118:172842 53-9 Mineralogical and Geological Chemistry Lab. Glaciol. Geophys. Environ.,Grenoble,Fr. Journal 0379-6566 written in English. 74-82-8 (Methane); 74-84-0 (Ethane); 74-85-1 (Ethylene) Role: PRP (Properties) (solid, near-IR spectra of, Titan's surface in relation to)Planets (Saturn, Titan satellite, surface of, near-IR of solid hydrocarbons in relation to); Infrared spectra (near-IR, of solid methane and ethene and ethane, Titan's surface in relation to) Titan surface hydrocarbon solid near IR LK Jones, Thomas D.PJoseph, JeffreyPJoseph, Jeffrey C. Jull, A. J. Timothy K. -H. Fricke K. Cernis K. E. Simmons K. H. Sharam K. Rages K. S. Noll(*K. ZdanaviciusKabin, KonstantinKaiser, Ralf I.P Kaldeich, B. Kamat, S. S. Kaneko, T.(* Kaneko, TakeoKarkoschka, E.Karkoschka, ErichKasprzak, WaynePKasting, James F. Keller, C. N.Keller, Richard M. Kessler, M. F. Khanna, R. J. Khanna, R. K. Khare, B. Khare, B. N. Khare, B.N.* Khare, BishunKhare, Bishun N.P Khelifi, A.* Khlifi, M.(*Khlifi, MohammedP Kim, S. J.(* Kim, Sang J.Kim, Sang JoonPKinjo, MasatakaPKirby, Stephen H.Kliore, Arvydas J.  Klug, D. D.* Kobayashi, K.Kobayashi, Kensei Kochavi, E.*Koehne, JessicaPKoffi-Kpante, K.P Koike, J.Koike, ToshiyukiP Kojiro, D. R.Kondrat'ev, K. YaKossacki, Konrad J. Kouassi, N.*Kouvaris, Louis C.  Kralj, Joel*Krasnopolsky, Vladimir A.Kress, Monika E.P Kuhn, W. R.*Kuhn, William R.P Kuiper, G. P.Kulkarni, S. R.P Kunde, V. Kunde, V. G.Kuznetsova, YuP L. A. Capone L. A. Mayo(*L. A. Sromovsky L. ChengL. H. WassermanL. J. Allamandola L. J. Spilker L. Lellouch* L. M. Lara(* L. Mugnier(* L. Vapillon*L. W. Esposito L.M. Lara L.P. Giver(* L.P.GiverLabracherie, L.P Lafait, J.(* Lago, V.@ Lai, OlivierLambert, I. R.P Lammer, H.(*Lammer, HelmutP Lane, A. L.* Lara, L. -M. Lara, L. M.*Larson, Harold P.Laube, ManfredP Laufer, D.(* Le Duc, E.(* Lebehot, A.* Lebonnois, S.Lebonnois, SebastienLebreton, J. -P.Lebreton, J. P.PLebreton, Jean-Pierre Lecacheux, A. Lecacheux, J. Lecluse, C.*Ledvina, S. A.PLee, Anthony Y. T.  Lellouch, E.Lellouch, Emmanuel  Lemmon, M. T.Lemmon, Mark T.P Lenzen, R.(*Leone, Stephen R. Lesser, Peter Leto, G.<Letourneur, B.P Levy, G. S.* Levy, M. Lewis, J. S. Lewis, John*Lewis, John S.P Lidman, C.(*Liebman Shirley, A.Liebman, Shirley A. Lindal, G. F.Lindgren, C. J.P Lisina, L. R. Liu, Renzhang Liu, Yifan(* Lobo, A. P.*Lopez-Moreno, J. J.Lopez-Valverde, M.  Lorenz, R. D. Lorenz, R.D.Lorenz, Ralph D.P Loureiro, J.Loveday, J. S.P Lowe, C. U.*Lumine, Jonathan I.Lunine Jonathan, I. Lunine, J.(* Lunine, J. I.Lunine, Jonathan I. Lutz, B. L.*Lutz, Barry L.PM. A. Knuckles M. AllenM. Banaszkiewicz M. Bruns M. Cabane M. Combes M. Dang-Nhu* M. E. Summers M. Fitaire(* M. G. Gazeau M. G. Tomasko M. Hoffmann* M. Nezel M. R. Wing(*M. Roos-Serote M. Sato M. T. Lemmon M. W. Rees(*M. W. Williams M.-C. Gazeau M.Cabane M.Heinrich(* M.S. Matthews M.T.Lemmon(* M.W.WilliamsMacFarlane, Joseph J. Macintosh, B. Maguire, W.*Maguire, W. C. Mahaffy, P.*Maillard, J. P.PMaillard, Jean PierreMaillard, Jean-Pierre $g\;lhNitriles Role: GOC (Geological or astronomical occurrence), PRP (Properties), OCCU (Occurrence) (in haze xrNitriles Role: GOC (Geological or astronomical occurrence), PRP (Properties), OCCU (Occurrence) (in Titan's clouds&Nitriles Role: GOC (Geological or astronomical occurrence), PRP (Properties), OCCU (Occurrence) (tholins soly. in, in Titan's aerosolsls TNNitriles Role: OCCU (Occurrence) (in atm. of Titan, vertical distributions of)Nitriles Role: OCCU (Occurrence) (in Titan's stratosphere, optical properties of, low-pressure continuous-flow plasma-discharge exptl. simulations in relation to)lgNitriles Role: RCT (Reactant), RACT (Reactant or reagent) (photochem. of, on Titan satellite of Saturn)+LNitriles: CH, chemistryst Nitrogen nitrogen atm evolution Titan $nitrogen atm Jupiter satelliteali$ nitrogen atm Titan meteor impact,(%nitrogen atom reaction methyl radical4/nitrogen carbon dioxide plasma jet spectrometry@X2S+ electronic transition in Titan radiative atm.)+L4.nuclear thermal rocket propellant Mars mission@Nucleation (cloudhcNucleation (exptl. study of nucleation properties of aerosols in the atmospheres of Mars and Titan)B$Nucleic acid bases(ab4.observations of planetary satellites with ISO)`(#ocean atm evolution Titan satellitevo Oceans (methane, on Titan)7HEOceans (of Titan, org. synthesis in, as model of prebiotic evolution)of CH radical with CH4, C2H2, C2H4, C2H6, and but-1-ene studied between 23 and 295 K with respect to reactions in planetary atmospheres)DTQOpacity (pressure-induced gas, of Titan's atm., thermal structure in relation to)Optical absorptiont ahcOptical absorption (collision-induced rototranslational, of methane pairs, quantum computations of)^D("Optical absorption (cross-sections0PMOptical absorption (IR, of deuteromethane broadened by hydrogen and nitrogen)PJOptical absorption (IR, of nitrogen and its mixt. with argon and hydrogen)/X Optical absorption (lab. measurements of absorption coeffs. for 727 nm band of methane at 77 K and comparison with results derived from spectra of Giant planets)Optical properties, p$Optical properties (of tholinsfac$ Optical properties (translucencyalhoptical properties, prodn. rate, and compn. of the org. aerosols and clouds on Saturn's satellite Titan)LOptical propertyoOptical reflectiont a Opticse: $org chem Titan atm life originFor org compd atm Titan satellite0+org compd photochem formation planetary atmor org compd prodn solar system \ysis of the time-dependent chemical evolution of Titan haze tholinAN 2002:824051yHaze particles exert a significant influence over the thermodn. and radiation absorption properties of the Titan haze, as well as its complex org. chem. Characterization of both the mol. and the submicrometer components of the haze is therefore vital for understanding the global properties of Titan. We have carriedxrFluorescence spectra of Titan tholins: in-situ detection of astrobiologically interesting areas on Titan's surfaceAN 2004:776927We report the three-dimensional fluorescence spectra of Titan tholins in water and acetonitrile, and sep. some of the fluorescent components of tholins using two-dimensional thin layer chromatog. In acetonitrile, tholins exhibit a broad fluorescence with a max. at 471 nm, and an excitation max. at 410 nm. The fluorescence spectrum of a water extn. displays a more complicated spectrum with multiple peaks. TLC results indicate the presence of at least three distinct fluorescent species. In addn., we obtained the two-dimensional fluorescence spectrum of tholins in water ice at 77 K, close to the surface temp. of Titan. The fluorescence of tholins in a 77 K ice matrix is red-shifted in comparison to a water soln., and undergoes a further red-shift when the water soln. is heated prior to freezing. These results suggest that a simple fluorescence probe could be used on the surface of Titan to identify sites where tholins have been mixed with water, and possibly reveal information about the extent of heating the tholin-water mixt. has undergone. This would be useful for a future mission with the goal of examg. the org. chem. of Titan. [on SciFinder (R)]jdHodyss, Robert McDonald, Gene Sarker, Niladri Smith, Mark A. Beauchamp, Patricia M. Beauchamp, J. L. Icarus6 General Biochemistry Noyes Laboratory of Chemical Physics,California Institute of Technology,Pasadena,CA,USA. Journal 0019-1035 written in English.h 171 2 525-530i 2004525-530i 2004\VHubbard, J. S., G. E. Voecks, G. L. Hobby, J. P. Ferris, E. A. Williams, D. E. Nicodem 1975tCUltraviolet-Gas Phase and -Photocatalytic Synthesis from CO and NH3i B @ J. Mol. Evol.5  223 - 241F?Hubbard, W. B., B. Sicardy, R. Miles, A. J. Hollis, R. W. Forrest, I. K. M. Nicolson, G. Appleby, W. Beisker, C. Bittner, H. -J. Bode, M. Bruns, H. Denzau, M. Nezel, E. Riedel, H. Struckmann, J. E. Arlot, F. Roques, F. Sevre, W. Thuillot, M. Hoffmann, E. H. Geyer, C. Buil, F. Colas, J. Lecacheux, A. Klotz, E. Thouvenot, J. L. Vidal, E. Carreira, F. Rossi, C. Blanco, S. Cristaldi, Y. Nevo, H. J. Reitsema, N. Brosch, K. Cernis, K. Zdanavicius, L. H. Wasserman, D. M. Hunten, D. Gautier, E. Lellouch, R. V. Yelle, B. Rizk, F. M. Flasar, C. C. Porco, D. Toublnac, G. Corugedo 1993.(The occultation of 28 Sagittari by TitanAstron. Astrophys. 269 541 - 563 Hunten, D. M. 1973`The escape of H2 from Titan  @ J. atmos. Sci.30 726b[Hunten, D. M., M. G. Tomasko, F. M. Flasar, R. E. Samuelson, D. F. Strobel, D. J. Stevenson 1984 Titan "Gehrels, T., Matthews, M.S., Saturn Tucson "University of Arizona Presso671--759.'Hutzell, W. T., C. P. McKay, O. B. Toon 1993JCEffects of time-varying haze production on Titan's geometric albedo Icarus 105162--174F?GIBIJSSYPV\NaOcXdeRfhhijl[mnoopqqrsst!!7^u%vyy=={~/<< 6w22229D 5555TJJ """####--@@300'''  ((((!""##$%& Faulin19979 Ferris1966 Ferris1966 Ferris1973 Ferris1973 Ferris1974 Ferris1974 Ferris1974 Ferris1975 Ferris1975e Ferris1981f Ferris1982g Ferris1982zS Ferris1990 Ferris1995 Ferris1996 Ferris1997 Ferris2000 Ferris2003zh Ferris20033 Ferris2003z! Feuchtgruber19988 Feuchtgruber1999@d Feuchtgruber1999@I Feuchtgruber2000@K Feuchtgruber2002@L Feuchtgruber2003i Fink1979 Fischer2001 Fitaire1995 Fitaire19957 Fitaire19978 Fitaire19999 Fitaire2000, Flasar1981 Flasar19811 Flasar19822 Flasar19919j Flasar19986 Flores197897 Flores19799x Forrest1973 Forrest1980k Fortes2000 Foster19999d Fouchet1999 Fouchet2003l Fox1975m Fox1996 Francisco1994 Freeman2001 Freiman1974 Frere1989 Frere1989- Frere1990nFroboese19830- Frommhold1987 Frost2002. Fujii1999J Fusco20017 G. Appleby1993o G. Bjoraker1993! G. Bjoraker1998vG. D. McDonald1993 G. E. Voecks1975 G. Graner1993- G. Israel1990J G. Kockarts1990 G. L. Hobby1975 G. Paubert1990' Gabis1992o Gan1992 Gan1992 Gan1994p Gao2002C Gautier1989D Gautier1989` Gautier1989 Gautier1989E Gautier1991 Gautier1995, Gautier1995 Gautier1996 Gautier1997H Gautier1997q Gautier1997I Gautier2000 Gautier2002 Gautier2002 Gautier2002L Gautier2003w Gavel1999; Gazeau1995zV Gazeau19951 Gazeau1997z Gazeau1998z< Gazeau1999z Gazeau1999zN Gazeau19999/ Gazeau2000 Gazeau20000? Gazeau2001? Gazeau20011r Gazeau2002@ Gazeau20033s Geake1992t Geake1998u Geballe1996} Geballe1998 Geballe20000 Geballe2003v Geballe2003@ Gee2003J Gendron2001w Ghez19991w Gibbard1999x Gillett1973y Gillett1975: Giver1983; Giver1983< Giver1983 Giver1984z Gladstone1993Glandorf2000@8 Glenar20030 Gombosi2001 Goorvitch1983R Gourley1998Granahan1997@F Graner19939K Griffin2002{Griffith1991p|Griffith19920Griffith19922Griffith19970}Griffith199800Griffith200200Griffith200302Griffith2003PvGriffith2003p~ Gross1974 Guan20022 Guez1997r Guez19989S Guillemin1990; Guillemin1995V Guillemin1995 Guillemin1996N Guillemin1999 Guillemin2000 Guillemin2001 Guiraud1996 Gupta19814 Gurwell1995E Gush20020 Guthrie20017 H. -J. Bode1993/ H. Cottin20007 H. Denzau19935H. E. Matthews19976H. E. Matthews1998H. E. Revercomb1981 H. Hart1983 H. J. Cleaves20027H. J. Reitsema19939 H. Levison20037 H. Struckmann1993 H.V.Ghyseghem1989Haberman20020E Halpern2002 Halvorson1977/Hamdouni19990 Handa2001 Hanel1981 Hanel1982 Hansen19977 Hansen2001 Hapke1978 Harpold1996 Harpold1998 Harpold2002*Hartmann19951Hartmann19980 Hartung2004 Hashimoto2001R Hatcher1998# Hathi2004 Hattori1982 He19969Heinrich1994p& Henry1991 Herath19819 Herbst20044! Herman19855Hibbitts1997@5 Hidayat19976 Hidayat19988 Hillman2003 Hochard1995 Hodyss2004 Holberg1982 Holtz1983 Honda1998Horsfall19550Hosokawa20011 Houas1996 Houck1980 Hubbard1975 Hubbard19807 Hubbard1993Hubbard1993807 Hubbard1993d19807 Hubbard19937 Hubbard1993807 Hubbard19937 Hubbard19937 Hubbard1993807 Hubbard199319807 Hubbard19937 Hubbard1993d19807 Hubbard19937 Hubbard19937 Hubbard1993807 Hubbard19937 Hubbard1993er2003L Feuchtgruber2003i Fink1979 Fischer2001, Flasar1981 Flasar19811 Flasar19822 Flasar19919j Flasar19986 Flores19789 Flores1979z7 Flores19799x Forrest1973 Forrest1980k Fortes2000d Fouchet1999 Fouchet2003l Fox1975m Fox1996 Freeman2001 Freiman1974I Frere1989 Frere1989- Frere1990nFroboese19830- Frommhold1987 Frost2002. Fujii1999J Fusco20017 G. Appleby1993o G. Bjoraker1993! G. Bjoraker1998 G. Cernogora1999vG. D. McDonald1993G. D. McDonald1994 G. E. Voecks1975L G. E. Wood1983 G. Graner1993- G. Israel1990 G. Israel1999J G. Kockarts1990 G. L. Hobby1975 G. Paubert1990o Gan1992 Gan1992 Gan1994p Gao2002 Gautier1989( Gautier1989C Gautier1989D Gautier1989` Gautier1989 Gautier1989E Gautier1991 Gautier1995 Gautier1996 Gautier1997H Gautier1997q Gautier1997I Gautier2000 Gautier2002 Gautier2002 Gautier2002L Gautier2003w Gavel1999; Gazeau1995zV Gazeau19951 Gazeau1997 Gazeau1997z Gazeau1998 Gazeau1998z< Gazeau1999z/ Gazeau2000 Gazeau20000? Gazeau2001r Gazeau2002s Geake1992t Geake1998u Geballe1996} Geballe1998 Geballe20000 Geballe2003v Geballe2003J Gendron2001w Ghez19991w Gibbard1999x Gillett1973y Gillett1975z Gladstone1993Glandorf2000@8 Glenar20030 Gombosi2001 Goorvitch1983Granahan1997@F Graner19939K Griffin20021Griffith1991P{Griffith1991p|Griffith19920Griffith19922Griffith19970}Griffith199800Griffith200200Griffith200302Griffith2003PvGriffith2003p~ Gross1974 Guez1997r Guez19989 Guez19989; Guillemin1995V Guillemin1995 Guillemin1996 Guillemin1999 Guillemin2000 Guiraud19963 Gupta1981 Gupta19814 Gurwell1995 Guthrie20017 H. -J. Bode1993L H. B. Hotz1983/ H. Cottin20007 H. Denzau19935H. E. Matthews19976H. E. Matthews1998H. E. Revercomb1981 H. Hart1983@ H. Imanaka20022 H. J. Cleaves20027H. J. Reitsema19939 H. Levison2003>H. Ogino19848?H. Ogino1986P7 H. Struckmann1993 H.V.Ghyseghem1989Haberman20020 Halvorson1977/Hamdouni19990 Handa2001 Hanel1981 Hanel1982 Hansen19977 Hansen2001 Hapke1978 Harpold1996 Harpold1998 Harpold2002*Hartmann19951Hartmann19980 Hartung2004 Hashimoto2001 Hattori1982Heinrich1994p Herath19819 Herbst20044! Herman19855Hibbitts1997@5 Hidayat19976 Hidayat19988 Hillman2003 Hodyss2004 Holberg1982 Holtz1983 Honda1998Horsfall19550Hosokawa20011 Houas1996 Houck1980 Hubbard1975 Hubbard19807 Hubbard1993鄿  Cruikshank19999 Cruikshank2001 Cruikshank2002 Cruikshank2004z Cuby20033 Curtis20000 D. B. Donner1973 D. B. Donner1973c D. C. Humm1984BD. E. Jennings1981UD. E. Jennings1981xD. F. Jennings19839 D. F. Strobel1984D. F. Strobell1997 D. Gautier1990 D. Gautier19907 D. Gautier199395 D. Gautier19976 D. Gautier1998 D. J. Tholen19919C D. L. Coffeen1982 D. L. Coffeen1983J D. M. Hunten19907 D. M. Hunten199397 D. Toublnac1993 D. W. Nooner1974da Silva2002p Dalton2004 Dandouras1997Q Danehy1978FDang Nhu19933) Daniell1992 Danielson1977 Danielson1986De Bergh19810De Bergh19860RDe Bergh19880SDe Bergh19900Tde Bergh19940/De Bergh19990H De Graauw1997I de Graauw2000K de Graauw2002 De la Rosa2001zwde Pater19999^ De Vanssay1992zU de Vanssay1993z' de Vanssay1995V de Vanssay1995G De Vanssay1999zW Debergh1984X DeBergh1987 Deme19929 DeMore1999DeRuiter1996@ DeZeeuw2001Y Dheandhanoo1984ZDimitrov19970[Dimitrov1997pDimitrov2004@\ Dire2000 Dixon1993] Do1990^ Do1992_ Do1992U Do19931 Dobrijevic2003z Donahue1978 Donahue2002 Dondi2001 Dones2003dDrossart19990Drossart200115 Dubach19766 Dubach19871 Dubey1999`Dubouloz1989pDubouloz19899Dubouloz19890 Duc1995 Dudeck1996 Dudeck19999 Dudeck20011, Duong1985a Durham2003 Dutuit20044E. A. Williams19757 E. Carreira1993 E. Chassefiere1992 E. Chassefiere1993mE. Chassefiere1995 E. Gendron19977$ E. Gendron2001 E. Gerard19907 E. H. Geyer1993K E. Karkoschka1993 E. Lellouch19907 E. Lellouch1993 E. Lellouch19977 E. Riedel1993c E. S. Barker19844 E. T. Arakawa19877 E. Thouvenot19933= E.T. Arakawa1984E.Y. Lau19929 Echegut2001 Edgington1999 Ehrenfreund1995 Eigenbrode2001z Elias1971 Elsila20044=Encrenaz19810FEncrenaz19933bEncrenaz19940HEncrenaz19977cEncrenaz19970Encrenaz19999dEncrenaz19990IEncrenaz20000KEncrenaz20022Encrenaz20030LEncrenaz20033* Engel1995+ English1996=Epchtein19810 Er198685Eshleman19810Eshleman1983p et al.19819 et al.19821F. Colas199097F. Colas19939p F. Hourdin20029 F. M. Flasar198447 F. M. Flasar19939 F. Raulin1975- F. Raulin1990 F. Raulin19917 F. Roques19937F. Rossi19939F. Roues199097F. Sevre19933 F. Sevres1990=F. Suits19841jF.Raulin2001z Fairley2000 Fanale19979 Fanale19979irley2000 Fanale19979ley2000 Fanale199792000 Fanale199792000 Fanale19979ley2000 Fanale19979ley2000 Fanale19979ley2000 Fanale1997900 Fanale19979y2000 Fanale1997900 Fanale19979y2000 Fanale19979 Fanale19979y2000 Fanale199792000 Fanale199792000 Fanale1997900 Fanale1997900 Fanale1997900 Fanale199792000 Fanale199792000 Fanale19979y2000 Fanale19979y2000 Fanale19979y2000 Fanale199792000 Fanale1997900 Fanale199792000 Fanale199792000 Fanale199792000 Fanale199792000 Fanale199792000 Fanale199792000 Fanale1997900 Fanale1997900 Fanale199792000 Fanale199792000 Fanale19979ley2000 Fanale19979y2000 Fanale19979ley2000 Fanale199792000 Fanale19979ZSRobotic planetary science missions enabled with small NTR engine/stage technologiesnAN 1995:684378LFThe high specific impulse (Isp) and engine thrust-to-wt. ratio of liq. H (LH2)-cooled nuclear thermal rocket (NTR) engines makes them ideal for upper stage applications to difficult robotic planetary science missions. A small 15 thousand pound force (klbf) NTR engine using a U-Zr-Nb ternary carbide fuel (Isp .apprx.960 s at .apprx.3025 K) developed in the Commonwealth of Independent States (CIS) is examd. and its use on an expendable injection stage provides major increases in payload delivered to the outer planets (Saturn, Uranus, Neptune and Pluto). Using a single Titan IV-class launch vehicle, with a lift capability to low Earth orbit (LEO) of .apprx.20 metric tons (t), an expendable NTR upper stage can inject 2 Pluto Fast Flyby spacecraft (PFF/SC) plus support equipment--combined mass of .apprx.508 kg--on high energy, 6.5-9.2 yr direct trajectory missions to Pluto. A conventional chem. propulsion mission would use a liq. O (LOX)/LH2 Centaur upper stage and 2 solid rocket kick motors to inject a single PFF/SC on the same Titan IV launch vehicle. For follow on Pluto missions, the NTR injection stage would use a Jupiter gravity assist (JGA) maneuver to launch a LOX/liq. methane (CH4) capture stage (Isp .apprx.375 s) and a Pluto orbiter spacecraft weighing between .apprx.167-312 kg, with chem. propulsion, a Pluto orbiter mission is not a viable option because of inadequate delivered mass. Using a standardized NTR injection stage and the same single Titan IV launch scenario, direct flight (no gravity assist) orbiter missions to Saturn, Uranus and Neptune are also enabled with transit times of 2.3, 6.6, and 12.6 yr, resp. Injected mass includes a storable, N tetroxide/monomethyl hydrazine (N2O4/MMH) capture stage (Isp .apprx.330 s) and orbiter payloads 340 to 820% larger than that achievable using a LOX/LH2-fueled injection stage. The paper discusses NTR technol. and mission characteristics, shows NTR stage and payload accommodations within the 26.2 m long Titan IV payload fairing, and discusses NTR stage performance as a function of assumed cryogenic tank technol. [on SciFinder (R)]Borowski, Stanley K. AIP Conference Proceedings 324t Pt. 1i 311-19 1995TNCAN 123:239983 71-13 Nuclear Technology NASA Lewis Research Center,Cleveland,OH,USA. Journal 0094-243X written in English. 60-34-4 (Monomethyl hydrazine); 10544-72-6 (Nitrogen tetroxide) Role: TEM (Technical or engineered material use), USES (Uses) (Robotic planetary science missions enabled with small NTR engine/stage technologies)Space vehicles (Robotic planetary science missions enabled with small NTR engine/stage technologies) robotic nuclear therm * *\VThe Titan haze revisited: Magnetospheric energy sources and quantitative tholin yieldsAN 1995:472119Lab. measurements are made of the radiation yields of complex org. solids produced from N2/CH4 gas mixts. contg. 10 or 0.1% CH4. These tholins resemble org. aerosols produced in the atmospheres of Titan, Pluto, and Triton. The tholin yields are large compared to the total yield of gaseous products: nominally, 13 (C + N)/100 eV for Titan tholin and 2.1 (C + N)/100 eV for Triton tholin. High-energy magnetospheric electrons responsible for tholin prodn. represent a class distinct from the plasma electrons considered in models of Titan's airglow. Electrons with E > 20 keV provide an energy flux .apprx.1 * 10-2 erg cm-2 sec-1, implying from our measured tholin yields a mass flux of 0.5 to 4.0 * 10-14 g cm-2 sec-1 of tholin. The corresponding thickness of the tholin sedimentary column accumulated over 4 Gyr on Titan's surface is 4-30 m. This figure is in agreement with required mass fluxes computed from recent radiative transfer and sedimentation models. If, however, these results, derived from expts. at .apprx.2 mb, are applied to lower pressure levels toward peak auroral electron energy deposition and scaled with pressure as the gas-phase org. yields, the derived tholin mass flux is at least an order of magnitude less. We attribute this difference to the fact that tholin synthesis occurs well below the level of max. electron energy deposition and to possible contributions to tholins from UV-derived C2-hydrocarbons. The Titan tholin, produced by magnetospheric electrons, is alone sufficient to supply at least a significant fraction of Titan's haze; this result is consistent with the fact that the optical properties of Titan tholin, among all proposed materials, are best at reproducing Titan's geometric albedo spectrum from near UV to mid-IR in light-scattering models. [on SciFinder (R)]6/Thompson, W. Reid McDonald, Gene D. Sagan, Carl7 Icarus 112o2r 376-81 1994jdCAN 122:244517 53-9 Mineralogical and Geological Chemistry Laboratory Planetary Studies,Cornell University,Ithaca,NY,USA. Journal 0019-1035 written in English. 74-82-8 (Methane); 7727-37-9 (Nitrogen) Role: GOC (Geological or astronomical occurrence), OCCU (Occurrence) (haze in the atm. of Titan with magnetospheric energy sources and quant. tholin yields)Planets (Saturn, Titan satellite, haze in the atm. of Titan with magnetospheric energy sources and quant. tholin yields); Haze (atm., haze in the atm. of Titan with magnetospheric energy sources and quant. tholin yields); Organic compounds Role: GOC (Geological or astronomical occurrence), OCCU (Occurrence) (tholins, haze in the atm. of Titan with magnetospheric energy sources and quant. tholin yields) planet Titan haze magnetosphere energy sourcer (atm., haze in the atm. of Titan with magnetospheric energy sources and quant. tholin yields); Organic compounds Role: GOC (Geological or astronomical occurrence), OCCU (Occurrence) (tholins, haze in the atm. of Titan with magnetospheric energy sources and quant. tholin yields) planet Titan haze magnetosphere energy sourcerTomasko, M., P. H. Smith 1982pjPhotometry and polarimetry of Titan: Pioneer 11 observations and their implications for aerosol properties Icarus5165 - 95<5Toon, O. B., C. P. McKay, C. A. Griffith, R. P. Turcoy 1992*$A Physical Model of Titan's Aerosols Icarus95 24--53RKToublanc, D., J. P. Parisot, J. Brillet, D. Gautier, F. Raulin, C. P. McKay 19952,Photochemical modeling of Titan's atmosphere Icarus 113 2 - 26(!Toupance, G., F. Raulin, R. Buvet 1975ztFormation of prebiochemical compounds in models of the primitive Earth's atmosphere. 1 CH4-NH3 and CH4-N2 atmosphereOrigins of Lifeo62 83-90iExperiment, coronaJCTran, B. N., J. C. Joseph, J. P. Ferris, P. D. Persans, J. J. Cherae 2003rkSimulation of Titan haze formation using a photochemical flow reactor: The optical constants of the polymer  Icarus 165 379 - 390,&Tran, B. N., J. P. Ferris, J. J. Chera 2003~xThe photochemical formation of a Titan haze analog. Structural analysis by X-ray photoelectron and infrared spectroscopy Icarus 162i 114 - 124r Q8 ?`ZRadiation (solar, absorption of, by compds. in Titan atm., radiative heat transfer during)tra0-Radiation (solar, interaction with Titan atm.Radiation chemistry0Radicals Role: FMU (Formation, unclassified), GFM (Geological or astronomical formation), PEP (Physical, engineering or chemical process), PRP (Properties), FORM (Formation, nonpreparative), PROC (Process) (result of methane decompn. and active nitrogenRadicals Role: PEP (Physical, engineering or chemical process), PRP (Properties), PROC (Process) (reaction kinetics of CH radical with CH4, C2H2, C2H4, C2H6, and but-1-ene studied between 23 and 295 K with respect to reactions in planetary atmospheres)<Radio wave (S-bandf t|xradioactive surface of Titan predicted from sedimentation of radiocarbon-rich atm. hazes of tholins, HCN, and acetylene)'4/radiocarbon Titan atm haze surface radioactiviy@D>Radiolysis (electron, of alkane ices, org. solid formation in)le ($radionuclide decay satellite meltingo Rainwater Raman spectraReaction kinetics Reaction mechanism (gas-phaseLIreactions of N+, N+2, and HCN+ with CH4, C2H2, and C2H4a in Titan's atm.) Reactors (flow, photochem.ati Red giantsreflectance and transmittance factors, extinction coeff., and other optical and chem. properties of tholins, as lab. analogs of aerosols of Titan)$Reflection spectra (UV-visiblee s,&Reflection spectra (UV-visible diffuse/W,(Reflection spectra (UV-visible, specular refraction ethane methane liq(#refraction liq alkane refractometertiRefractive index Refractive index (of polymersLHRefractive index and Optical refraction (detn. of low-temp., of alkanes)8PKRefractive index and Optical refraction (of liquefied gas mixts., detn. of)X \WRefractive index and Optical refraction (of tholins, comet spectrometry in relation to)D84Refractometers (cryogenic, for liquefied gas mixts.)@;Refractometers (Huygens SSP, for planetary surface studies)y Remote sensing@=Remote sensing (Cassini radar remote sensing of Titan surface0-Remote sensing (Voyager spacecraft IR spectra`]report and implications of the first observation of C4N2 in lab. simulations of Titan's atm.) review aerosol Titan tholinf 85review anaerobic bacteria biogeochem exobiol research`]review and latest results of lab. investigations of Titan's aerosols and the role of tholins)<9review atm compn structure Jupiter Saturn IR spectroscopy($review atm Titan atm heating coolingo review extraterrestrial lifee0,review extraterrestrial life robot detectioncreview Neptune satellitei4.review nonterrestrial planet atm isotope ratio@($review org compd atm Titan satellitet$review org synthesis atm Titaniew$review outer Solar system chemte,D@review phanerozoic cold vent biota exobiol extraterrestrial lifei@:review planet atm org compd formation high energy particle (G($review planet structure atm thermodnt$review planetary atm photochemroc(%review Solar System chem planet Titan0+review Titan atm compn meteorol perspective7review Titan atm model, areview Titan atm org chem$ review Titan atm org gas aerosoll$!review Titan atm origin evolution review titan atm photochemell@;review Titan exploration instrumentation tholins spacecraft@,)review Titan lightning energy biochem atmreview Titan org chem0*review Titan prebiotic org synthesis modeltan0*review Titan satellite atm org chem tholin. o$review Titan Saturn atm methanee,KJIHGFDECBA@>?=<;:9876543120/.-,+*)('& $#"!%    >T Lunine2003 Lunine20033 Lutz1976Q Lutz19787 Lutz1981 Lutz1982T Lutz1983W Lutz19849 Lutz1986ZX Lutz19879R Lutz19881S Lutz19901/ Lutz19999|M. A. Knuckles19977M. Bruns19939l M. Cabane1993m M. Cabane1995n M. Cabane1997$ M. Combes2001 M. Dang-Nhu1993 M. Fitaire1982' M. G. Gazeau19959 M. G. Tomasko19847 M. Hoffmann19937M. Nezel19933v M. R. Wing19931oM. Roos-Serote2000C M. Sato1982 M. Sato1983 M. T. Lemmon1996 M. W. Rees1963= M.W.Williams1984 MacFarlane1980zw Macintosh1999U Maguire1981w Maguire1981 Maguire1981 Maguire1982 Mahaffy1996Maillard19810SMaillard19900Maillard19922GMaillard19955Maillard19979 Mancinelli1990z Manning1996 Mansour1994 Marcano2001 Marco2004Margulis19770 Markham1963 Marston1989E Marten19911V Marten2002 Martin19977 Martin1997 Masuda20010 Matson19979 Matson2002 Matson20020 Matsui20042Matthews19920RMatthews1998Matthews2003p Mauersberger2002@w Max1999z Mayo1991~ Mayo1997 Mayo1997McCarthy19800 McCord1971 McCord1997McDonald1991pMcDonald1991pMcDonald1992PMcDonald1994pMcDonald1994pMcDonald1996@McDonald19999McDonald2004@ McEwan1998 McEwan20000 McEwan20011 McEwan20033 McEwan20044, McKay1985 McKay1988+ McKay1988 McKay1989Y McKay1991 McKay1992[ McKay1993 McKay1995G McKay1995, McKay1995\ McKay1996 McKay1997 McKay1997 McKay1997 McKay1997w McKay1999 McKay1999 McKay1999 McKay2001 McKay2001( McKay2001p McKay2002 McKay2002 McKay2002 McKay2002 McKay20038 McKay2003 McKay2003 McKay2004 McKay20042 McKay2004McKellar19890,McKenzie19850 McLain2004_ Meier2000 Meisse19933 Meisse19944Mendillo2003gMeot-Ner19780x Merrill1973 Metzger2000K Meyyappan2002L Meyyappan2003( Mill19921s Mill19922t Mill19988} Miller19989 Miller2002eMilligan20000R Minard1998P Minard2000Q Minard2000Miyakawa2002Miyakawa20033 Molek2004= Molina19919`Molina-Cuberos1999Molina-Cuberos1999Molina-Cuberos2000Molina-Cuberos2000Molina-Cuberos2001)Molina-Cuberos2001 Moore1998 Moore2003L Moore2003Mordaunt19930V Moreno20020& Morgan19801F Morgan2002eMorimoto19810fMorimoto19820gMorimoto1982p Morley19933C Morris1982r Morton2003 Moses2000 Moskalenko1982z Mota1998o Mourey1982z Mousis2002 Mousis2002zMueller-Wodarg2003J Mugnier2001aMuhleman1990P4Muhleman1995PK Muller20020 Muller-Wodarg2002A Murray1963 Mvondo2000z7 N. Brosch1993e N. Noy19799/N. Smith20000 Nagano19828 Nagy19819 Nagy1984m Nagy19866 Nagy2001 Nahoum1992 Nascimento1998z Nath1997 Nava19899 Navale1998Navarro-Gonzalez19970Navarro-Gonzalez1998@Navarro-Gonzalez2000@Navarro-Gonzalez2001@Navarro-Gonzalez2001Navarro-Gonzalez2001Navarro-Gonzalez2001Navarro-Gonzalez2002c Neff1984 Nelmes20011 Nelmes20033 Nelson1978 Nesbitt1989(Neubauer20010; Neukum1997v Nicodem1975 Nicolas2004 Niemann1996 Niemann2002d Noll1996 Noll20000 Noll2002fv Noll20030 Nollet1999 Notesco1997 Noy1984 Null19801 O'Brien1995 O'Brien1996` O'Brien1999 O'Brien2002 O'Hara19878f O. B. Toon1980 O. B. Toon19879 O. Lai1997s$ O. Lai20012 O. S. Zamek1974 Ochiai1981z Ogino1984 Ogino1986 Ohashi20010 Okabe1996 Opansky1996Oremland19890 Orgel1966 Orgel1966# Ori2001 Oro1960 Oro1961 Oro1974 Oro1999H Orton1997 Osamura2004 Oshima19949 Oshima1997aI Ott2000K Ott2002L Ott2003 Owen1974 Owen1975" Owen19757 Owen1976 Owen1977oQ Owen19787= Owen19811 Owen19811 Owen1982 Owen1982 Owen1982T Owen1983gW Owen19849 Owen1986ZX Owen19879R Owen19881S Owen19901{ Owen19911| Owen19921 Owen1992z Owen19939} Owen19981_ Owen2000t Owen2000s Owen20020 Owen2002gF Owen20020E Ozier2002 P. Lesser1974  P. Rannou1993 P. Rannou2002 P. Schenk2003j P.Coll2001o+ P.R. Ratcliff1996 Paillou2003^Paillous19929Paillous19960Paillous19990 Palacios-Pru2001@ Palumbo1993, Parisot1995) Parker19929 Parris1988o Parzhin1982 Patnaik1996 Patrick1996 Paubert19935 Paubert19976 Paubert1998 Pavlov2001 Pavlov2001z2 Pavlov20044 Payne1989 Pearl1981 Pearl1982Pellerin19990Pellerin20010d Pendleton1996  Perez-Hoyos2004 Persans2003h Persans2003 Pietrogrande2001@ Pintassilgo1999 Pinto1980H Pinto1984 Pirraglia1981 Pirraglia1982 Podolak1977e Podolak1979 Podolak1979 Podolak1984 Podolak1984 Pointu19821Pointu19821 Pointu19821k1984 Pointu1982184 Pointu19821dolak1984 Pointu198211984 Pointu1982184 Pointu19821k1984 Pointu19821 Pointu19821k1984 Pointu1982184 Pointu198211984 Pointu19821 Pointu19821 Pointu19821 Pointu19821lak1984 Pointu19821 Pointu19821k1984 Pointu19821 Pointu19821 Pointu19821 Pointu1982184 Pointu198211984 Pointu1982184 Pointu1982184 Pointu198211984 Pointu19821 Pointu1982184 Pointu19821 Pointu19821dolak1984 Pointu19821k1984 Pointu19821 Pointu19821 Pointu19821 Pointu19821 Pointu1982184 Pointu198211984 Pointu19821 Pointu19821 Pointu19821 Pointu19821k1984 Pointu19821 Pointu19821lak1984 Pointu19821k1984 Pointu1982184 Pointu19821974 Owen1977oT Owen1983g_ Owen2000ts Owen20020b P. Coll2001k P. Coll2002 P. D. Persans2003 P. Lesser1974  P. Rannou1993 P. Rannou2002 P. Rannou2002 P. Schenk2003j P.Coll2001o^ P.Drossart20010+ P.R. Ratcliff1996^P.Rannou20010P.Rannou20033 Paillou2003 Palacios-Pru2001@) Parker19929 Parris1988o Patnaik1996 Paubert19935 Paubert19976 Paubert1998d Pendleton1996 Persans2003 Pietrogrand2001 Pietrogrande2001@ Pinto1980 Pinto1984e Podolak1979 Podolak1979 Pointu19821G@  olecular Ion-Molecule Reactions in Titan's AtmosphereoAN 2002:235479We have applied @9Termolecular Ion-Molecule Reactions in Titan's AtmosphereoAN 2002:235479We have applied information from the thermochem. of cluster ions to a model of the Titan atm. Using lab. thermodn. data on the clustering of ions with both nitrogen and methane from the literature, we find that substantial clustering of ions with the atm. nitrogen occurs from about 100 km down to the surface. The temp. and no. d. profiles of the various chem. species in the atm. of Titan were also taken from the literature. A specific anal. of the clustering of HCNH+ with nitrogen was performed. It was found that for HCNH+ substantial clustering will occur in a nitrogen atm. at the temps. and pressures found in the Titan tropopause. The thermochem. data of the three ions: HCNH+, N2H+, and CH5+ are very similar. By inference the N2H+ and CH5+ ions are also expected to undergo substantial clustering. Assuming no factors other than equil. thermodn. to control the cluster size, the max. av. cluster size found was 65.5 at the tropopause. At the surface, the cluster size decreased to about 25. (c) 2001 Academic Press. [on SciFinder (R)],%Anicich, Vincent G. McEwan, Murray J. Icarus 154g2h522-530n 2001CAN 137:111938 53-9 Mineralogical and Geological Chemistry Jet Propulsion Laboratory,California Institute of Technology,Pasadena,CA,USA. Journal 0019-1035 written in English. 7727-37-9D (Nitrogen) Role: GFM (Geological or astronomical formation), GPR (Geological or astronomical process), FORM (Formation, nonpreparative), PROC (Process) (cluster complexes with cations; thermochem. modeling of literature data predicts that single ions of HCNH+, N2H+, and CH5+ undergo significant clustering with N2 mols. of the Titan atm. at altitudes of <100 km); 12357-66-3D (Diazenylium); 15135-49-6D (Methane, monoprotonated); 21107-92-6D (Methylium, imino-) Role: GFM (Geological or astronomical formation), GPR (Geological or astronomical process), FORM (Formation, nonpreparative), PROC (Process) (thermochem. modeling of literature data predicts that single ions of HCNH+, N2H+, and CH5+ undergo significant clustering with N2 mols. of the Titan atm. at altitudes of <100 km)Cluster ions; Titan (thermochem. modeling of literature data predicts that single ions of HCNH+, N2H+, and CH5+ undergo significant clustering with N2 mols. of the Titan atm. at altitudes of <100 km) Titan atm cluster cation nitrogen2uction of organic gases and aerosols by electrical activity in Titan's tropospheric clouds AN 1999:6354VOThe corona discharge chem. of a Titan simulated atm. was investigated by GC-FTIR-MS techniques. The main products are hydrocarbons (ethane, ethyne, ethene, propane, 2-methylpropane, n-butane, n-pentane, and n-hexane), nitriles (hydrogen cleThe spectrum of gaseous methane at 77 K in the 1.1-2.6 mm region: a benchmark for planetary astronomyiAN 1990:188373The spectrum of CH4 obtained in CH4 plus N2 mixts. at a temp. of 77 K was recorded with a spectral resoln. of 0.14 cm-1 in the region 3800 to 9100 cm-1. The expts. were performed with long paths (66 or 88 m) in a cooled absorption cell using a Fourier-transform spectrometer. Data are presented here at low and medium resoln., and examples of some spectral regions are also shown at high resoln. The complete results are available from the author in an Appendix. Comparisons are made with previous model calcns. of CH4 absorption, and with the obsd. spectrum of Nepturn's satellite, Triton. The results should be useful for the interpretation of the spectra of Triton, Titan, and Pluto. They will also be of value for testing model calcns. of low-temp. CH4 absorption, which, thus verified, can be used with greater confidence to analyze observations of Jupiter, Saturn, Uranus, and Neptune. [on SciFinder (R)]McKellar, A. R. W."Canadian Journal of Physicsp67111027-35 198960CAN 112:188373 73-9 Optical, Electron, and Mass Spectroscopy and Other Related Properties Herzberg Inst. Astrophys.,Natl. Res. Counc. Canada,Ottawa,ON,Can. Journal 0008-4204 written in English. 74-82-8 (Methane) Role: PRP (Properties) (IR spectra of low-temp. gaseous, planetary astronomy in relation to)Planets (low temp. methane IR spectra in study of); Infrared spectra (of methane, at low temps., planetary astronomy in relation to); Astrophysics (astronomy, planetary, methane IR spectra in) IR methane planetary astronomyt-Jation of organic compounds from simulated Titan atmosphere: perspectives of the Cassini missionXQKoike, Toshiyuki Kaneko, Takeo Kobayashi, Kensei Miyakawa, Shin Takano, YoshinoriUchu seibutsu kagaku 2003 Oct173 188-9Department of Chemistry and Biotechnology, Yokohama National University 0914-9201 Japan Journal; Article; (JOURNAL ARTICLE) English 2003598064Gas mixtvpCollision-induced rototranslational absorption spectra of methane-methane pairs at temperatures from 50 to 300 KAN 1987:466759Previously (B. and F. 1987), rigorous quantum computations of the rototranslational absorption spectra of MeH-MeH pairs were communicated which closely reproduce existing lab. measurements at 124-300 K at 0-750 cm-1. Since the computations are complex, how the spectra can be reproduced from simple, anal. functions that closely model the quantum profiles and the lab. measurements are described. For 50-300 K, the rototranslational, collision-induced spectra of MeH pairs were obtained accurately on small computers in seconds. No measurements exist for comparison with the computational results at the lower temps. (<124 K). [on SciFinder (R)].,%Borysow, Aleksandra Frommhold, LotharcAstrophysical Journal 318o2, Pt. 1 940-3m 19872+CAN 107:66759 73-1 Optical, Electron, and Mass Spectroscopy and Other Related Properties Phys. Dep.,Univ. Texas,Austin,TX,USA. Journal 0004-637X written in English. 74-82-8 (Methane) Role: PRP (Properties) (collision-induced rototranslational absorption spectra of pairs of, quantum computations of)tOptical absorption (collision-induced rototranslational, of methane pairs, quantum computations of); Quantum electrodynamics (of collision-induced rototranslational absorption spectra of methane pairs); Planets (Saturn, Titan satellite, collision-induced rototranslational spectra of methane pairs quantum computations in relation to) methane collision rototranslational absorption theory/ sure broadening and shift coefficients for H2, He and N2 in the 3n2 band of 12CH3D retrieved by a multispectrum fitting techniqueAN 1999:386319F?Improved detns. of CH3D abundances, and of the D to H ratio (D/H) in the atm. methane of Saturn,Pressure broadening and shift coefficients for H2, He and N2 in the 3n2 band of 12CH3D retrieved by a multispectrum fitting techniqueAN 1999:386319F?Improved detns. of CH3D abundances, and of the D to H ratio (D/H) in the atm. methane of Saturn, Uranus, Neptune and Titan are reachable with a complete set of spectroscopic parameters for the 3n2 band of 12CH3D which take into account the dominant gases in these atms. (i.e. H2, He and N2). Line intensities and self-broadening coeffs. derived from a previous anal. made by the authors' group for 255 lines in the region of the 3n2 band of 12CH3D at 1.55 mm were recently reported. The authors present 12CH3D line broadening coeffs. and pressure-induced shifts by H2, He and N2. A set of Fourier transform spectra recorded at Kitt Peak National Observatory with pressures of 100, 250 and 500 torr for H2 and N2, and 600 torr for He, was used for this study. Data redn. was performed using a nonlinear least-squares fitting multispectrum program developed for this purpose. The broadening coeffs., averaged over K, range roughly between 0.0685 and 0.0569 cm-1 atm-1 for 12CH3D-H2, between 0.0434 and 0.0335 cm-1 atm-1 for 12CH3D-He, and between 0.0665 and 0.0533 cm-1 atm-1 for 12CH3D-N2, up to a max. J of 14. The uncertainties .apprx.1.5% in the H2 and N2 broadening cases, and 3% in the He case. The pressure shift coeffs. averaged over both J and K are -0.0067 cm-1 atm-1 for 12CH3D-H2, +0.0021 cm-1 atm-1 for 12CH3D-He, and -0.0119 cm-1 atm-1 for 12CH3D-N2. The authors est. an uncertainty in these av. shift coeffs. of 15% in the H2 and N2 broadening cases, and of 35% in the He case. Dependences in J and K for these parameters also were studied with empirical expressions. [on SciFinder (R)]e81Boussin, C. Lutz, B. L. Hamdouni, A. De Bergh, C.i@9Journal of Quantitative Spectroscopy & Radiative Transferg631i 49-84e 1999 CAN 131:108324 73-1 Optical, Electron, and Mass Spectroscopy and Other Related Properties Groupe de Spectrometrie Moleculaire et Atmospherique, UPRESA - CNRS 6089, UFR Sciences,Reims,Fr. Journal 0022-4073 written in English. 676-49-3 (Methane-d); 1333-74-0 (Hydrogen); 7440-59-7 (Helium); 7727-37-9 (Nitrogen) Role: PEP (Physical, engineering or chemical process), PRP (Properties), PROC (Process) (pressure broadening and shift coeffs. for H2, He and N2 in 3n2 band of 12CH3D retrieved by a multispectrum fitting technique)`ZCollisional relaxation; Collisions; Interstellar space; Neptune; Planets; Saturn; Titan; Uranus (pressure broadening and shift coeffs. for H2, He and N2 in 3n2 band of 12CH3D retrieved by a multispectrum fitting technique) pressure broadening shift coeff hydrogen helium nitrogen band; multispectrum fitting technique methane collision transitionK4-Observations of planetary satellites with ISOiAN 2002:979948Several observational programs were conducted with ISO (Kessler et al., 1996) aiming at the investigation of the near- and far- IR spectrum of the satellites of the giant planets. Thus, Jupiter's satellites Callisto, Io, and Ganymede were explored mainly with the spectrometers, while the spectrum of Titan, Saturn's largest satellite, was investigated thoroughly by all the instruments. The anal. of the data has provided original and precious information on the satellites' surfaces and Titan's atm. in particular. [on SciFinder (R)] Coustenis, A. Encrenaz, Th Lellouch, E. Salama, A. Muller, Th Burgdorf, M. J. Schmitt, B. Feuchtgruber, H. Schulz, B. Ott, S. de Graauw, Th Griffin, M. J. Kessler, M. F. Advances in Space Research309 1971-1977 2002CAN 138:290634 53-9 Mineralogical and Geological Chemistry Paris-Meudon Observatory,DESPA,Meudon,Fr. Journal 0273-1177 written in English. 74-82-8 (Methane); 74-84-0 (Ethane); 74-85-1 (Ethene); 74-90-8 (Hydrocyanic acid); 74-98-6 (Propane); 74-99-7 (Propyne); 124-38-9 (Carbon dioxide); 460-12-8 (1,3-Butadiyne); 676-49-3 (Methane-d); 7446-09-5 (Sulfur dioxide); 7732-18-5 (Water) Role: GOC (Geological or astronomical occurrence), OCCU (Occurrence) (observations of planetary satellites with ISO)Jupiter (Ganymede satellite; observations of planetary satellites with ISO); Satellites (Ganymede; observations of planetary satellites with ISO); Jupiter (Io satellite; observations of planetary satellites with ISO); Satellites (Io; observations of planetary satellites with ISO); Satellites; Titan (observations of planetary satellites with ISO) giant planet satellite sulfur oxide water hydrocarbon(<$ Satellites (Triton, atm. aerosoluences on the morphol. of simulated Triton and Titan atm. aerosol tholins obtained by inductively coupled plasma from CH4-N2 gas mixts.)XjcCoustenis, A., A. Salama, B. Schulz, S. Ott, E. Lellouch, Th. Encrenaz, D. Gautier, H. Feuchtgruber. 2003<5Titan's atmosphere from ISO mid-infrared spectroscopy. Icarus 161s 383 - 403Titan, gas, Observatione&Cruikshank, D. P., J. S. Morgan 19800*Titan: Suspected Near-Infrared Variability Astrophys. J. 235 L53 - L54Titan, ObservationrkCruikshank, D. P., L. J. Allamandola, W. K. Hartmann, D. J. Tholen, R. H. Brown, C. N. Matthews, J. F. Belle 1991<6Solid CN Bearing Material on Outer Solar System Bodies Icarus94 345 - 353>8de Vanssay, E., M. G. Gazeau, J. C. Guillemin, F. Raulin 1995NGExperimental simulation of Titan's organic chemistry at low temperaturerPlanet. Space Sci.4325 - 31 istry of Titan Icarus 115e119-125a$experiment, UV, cyanoacetylene Clarke, D.W., J.P. Ferris\ 1996B;Mechanism of cyanoacetylene photochemistry at 185 and 254nmJ. Geophys. Res. 101r 7575-7584$experiment, UV, cyanoacetylene Clarke, D.W., J.P. Ferris 1997haTitan Haze: Structure and Properties of Cyanoacetylene and Cyanoacetylene-Acetylene Photopolymersl Icarus 127s158-17210)experiment, UV, cyanoacetylene, acetylene L (Cess, Robert D.P Chang, S.Chang, SherwoodPChanover, N. J.PChanover, N.J. Chaquin, P.*Chaquin, PatrickPChassefiere, E.Chassefiere, Eric Chauville, J. Chen, Bin Chen, C. T.* Cheng, L. Chera, J. J.Chera, John J.P Chudamani, S. Chyba, C. Chyba, C. F. Clark, J. Clark, R. N.Clark, Roger N.P Clarke, D.W.Clemett, S. J. Close, L. M.Cody, George D.PColaprete, TonyP Coll, P.$ Coll, Patrice Combes, M.(*Combes, MichelPCombi, Michael R.Commandeur, J.P Conrath, B.*Conrath, B. J.Consolmagno, Guy J. Corugedo, G. Coscia, D.(* Coscia, David Cosia, D. Cosia, David Cottin, Herve Courtin, R.*Courtin, RegisP Coustenis, A.Coustenis, AthenaCravens, T. E.P Crepin, C.(* Croft, T. A. Crovisier, J.Cruikshank, D.PCruikshank, D. P.Cruikshank, Dale P. Cuby, J. G.*Curtis, Daniel B. D. B. Donner D. C. Humm(* D. Coschia(* D. Coscia D. CruikshankD. E. JenningsD. E. ShemanskyD. F. Jennings D. F. StrobelD. F. Strobell D. Gautier(*D. J. Stevenson D. J. Tholen D. L. Coffeen D. M. Hunten D. MoureyD. N. SweetnamD. P. Cruikshank D. Toublnac* D. W. Nooner D.A.Glenar(* D.S.Sklarew* da Silva, A. Dalton, J. B. Dandouras, J.Danehy, Robert G. Dang Nhu, MaiDaniell, P. M.PDanielson, G. EdwardDanielson, R. E.P De Bergh, C.De Bergh, Catherine De Graauw, ThDe la Rosa, J. G. de Pater, I.de Vanssay, E.De Vanssay, Etienne Debergh, C.* Deme, N. DeMore, W.B.DeRuiter, CynthiaDeZeeuw, Darren L. Dheandhanoo, SeksanDimitrov, VasiliPDire, James R.PDishoeck, E. F. v.  Dixon, R. N. Do, L.G,Dobrijevic, M.PDonahue, T. M.PDonahue, Thomas M. Dondi, F. Dones, L. Drossart, P. Dubach, J.(*Dubey, Manvendra K. Dubouloz, N. Duc, E.$ Dudeck, M.(* Duong, N. D.Durham, William B.  Dutuit, OdileE. A. Williams E. Carreira*E. Chassefiere E. de Vanssay E. Gendron(* E. Gerard E. H. Geyer* E. KarkoschkaE. L. O. Bakes E. Lellohch* E. Lellouch* E. Ochiai E. Riedel E. S. Barker E. T. Arakawa E. Thouvenot E.L.O. Bakes E.T. Arakawa E.Y. Lau Echegut, P.*Edgington, S. G.PEhrenfreund, P.Eigenbrode, Jennifer L.+LElias, Jonathan H. Elsila, Jamie E.P Encrenaz, P. Encrenaz, T. Encrenaz, ThEncrenaz, Therese Engel, S. English, M.A. Epchtein, N. Er, CevatEshleman, V. R.P et al.J F. Colas F. Hourdin(* F. M. Flasar F. Raulin F. Roques F. Rossi F. Roues F. Sevre F. Sevres F. Suits F.RaulinFairley, David A. Fanale, F. P. Faulin, F.(* Ferris, J. P. Ferris, J.P.Ferris, James P.PFeuchtgruber, H. Fink, Uwe Fischer, G.* Fitaire, M.* Flasar, F. M. Flores, J.(* Flores, JoseForrest, W. J.P Fortes, A. D.Foster, Laura L.P Fouchet, T.* Fox, J. L.(* Fox, KennethFrancisco, Joseph S. interaction between the magnetosphere of Saturn and Titan's ionosphereAN 2001:533175A three-dimensional (3-D) multi-species MHD model was used to study the interaction of Titan's ionosphere and Saturn's magnetosphere. The three generic species which were considered are light (e.g., H+, H+2, and H+3), medium (e.g., N+ aPJThe interaction between the magnetosphere of Saturn and Titan's ionosphereAN 2001:533175A three-dimensional (3-D) multi-species MHD model was used to study the interaction of Titan's ionosphere and Saturn's magnetosphere. The three generic species which were considered are light (e.g., H+, H+2, and H+3), medium (e.g., N+ and CH+5), and heavy (e.g., N+2 and HCNH+) ion species. The effects of exospheric mass loading, major chem. reactions, and ion-neutral collisions were considered. The upstream parameters were selected to be the nominal values for the case when Titan is in the magnetosphere of Saturn. The simulation results are compared with Voyager measurements as well as related model calcns. The 3-D three-species model results reproduce reasonably well the global features such as magnetic barrier, magnetotail, and the distributions of the major ionospheric species. The outward escape flux of the major ionospheric species (i.e., the heavy ion species), from the tail is calcd. to be approx. 6.5 * 1024 S-1. [on SciFinder (R)]Nagy, Andrew F. Liu, Yifan Hansen, Kenneth C. Kabin, Konstantin Gombosi, Tamas I. Combi, Michael R. DeZeeuw, Darren L. Powell, Kenneth G. Kliore, Arvydas J.60Journal of Geophysical Research, [Space Physics] 106lA4 6151-6160 2001CAN 135:245205 53-9 Mineralogical and Geological Chemistry Space Physics Research Laboratory, Department of Atmospheric, Oceanic and Space Sciences,University of Michigan,Ann Arbor,USA. Journal 0148-0227 written in English. 13966-04-6 (Nitrogen, ion (N2+); 21107-92-6 (Methylium, imino-) Role: GOC (Geological or astronomical occurrence), GPR (Geological or astronomical process), OCCU (Occurrence), PROC (Process) (heavy ion; light-medium-heavy ion MHD simulation of the interaction between the magnetosphere of Saturn and Titan's ionosphere); 12184-90-6 (Hydrogen, ion (H21+); 12586-59-3 (Proton); 28132-48-1 (Hydrogen, ion (H31+) Role: GOC (Geological or astronomical occurrence), GPR (Geological or astronomical process), OCCU (Occurrence), PROC (Process) (light ion; light-medium-heavy ion MHD simulation of the interaction between the magnetosphere of Saturn and Titan's ionosphere); 14158-23-7 (Nitrogen, ion (N1+); 15135-49-6 (Methane conjugate acid) Role: GOC (Geological or astronomical occurrence), GPR (Geological or astronomical process), OCCU (Occurrence), PROC (Process) (medium ion; light-medium-heavy ion MHD simulation of the interaction between the magnetosphere of Saturn and Titan's ionosphere))Saturn; Titan (light-medium-heavy ion MHD simulation of the interaction between the magnetosphere of Saturn and Titan's ionosphere) Saturn magnetosphere Titan ionosphere MHD modelike, Y. J. Pendletono 1996KTitan's 5 mm spectral window: carbon monoxide and the albedo of the surface      Icarus 126 625 - 631Oro, J. 19600*Synthesis of adenine from ammonium cyanide$Biochem. Biophys. Res. Commun.2 407 - 412Oro, J., S. S. Kamat 1961ZTAmino-acid Synthesis from Hydrogen Cyanide under Possible Primitive Earth Conditions Nature 190e 442 - 443XtWpmental simulation of Titan's organic chemistry at low temperature AN 1995:660400A new program of simulation expts. has been started using temp. conditions close to those of Titan's environment, more compatible with the build-up and detection of orgs. stable piAbundance of deuterium in the outer solar system from ground-based measurements of monodeuterated methaneAN 1985:457085f_CH3D absorptions were detected in spectra of Saturn, Uranus, and Titan recorded at .apprx.1.6 m with the Fourier transform spectrometer at the 4m telescope of Kitt Peak National Observatory. Preliminary results of the measurements of the CH3D/CH4 ratio in the atms. of these 2 giant planets and of the satellite Titan are presented. [on SciFinder (R)]A& Debergh, C. Lutz, B. L. Owen, T. ("Obs. Paris-Meudon,Paris-Meudon,Fr. 6 pp 1984CAN 103:57085 53-9 Mineralogical and Geological Chemistry Report written in English. 676-49-3 Role: OCCU (Occurrence) (in atms., of Saturn and Titan satellite and Uranus); 7782-39-0 Role: OCCU (Occurrence) (in outer solar system, abundance of, from ground-based measurements)(Planets (Saturn, atms. of, monodeuterated methane in); Planets (Saturn, Titan satellite, atms. of, monodeuterated methane in); Planets (Uranus, atms. of, monodeuterated methane in) deuterium solar system abundance; monodeuterated methane Saturn Uranus Titan, VPMonodeuterated methane in the outer Solar system. Part 3: Its abundance on Titan AN 1988:9139The 3n 2 band of CH3D was detected in spectra of Titan recorded at 1.6m with Fourier Transform Spectrometer. A value for the CH3D/CH4 mixing ratio of 6.6 (+6.6 or -3.3) * 10-4 was obtained from a comparison between the obsd. Titan spectra and synthetic spectra. This value is .apprx.2 times higher than the value measured on Uranus and .apprx.6 times higher than on Jupiter and on Saturn. It corresponds to D/H of 1.65 (+1.65 or -0.8) * 10-4, nominally 8 times higher than the most commonly accepted value for the protosolar D/H. The value on Titan for D/H in CH4 is comparable to the D/H ratio measured in terrestrial H2O. [on SciFinder (R)]4.DeBergh, C. Lutz, B. L. Owen, T. Chauville, J. Obs. Paris,Paris,Fr. 16 ppt 1987CAN 108:9139 53-9 Mineralogical and Geological Chemistry Report 0565-7059 written in English. 676-49-3 (Methane-d) Role: OCCU (Occurrence) (in Titan satellite, abundance of)wjcPlanets (Saturn, Titan satellite, monodeuterated methane on) monodeuterated methane Titan satellite 08 f \VOn the sources of ultraviolet absorption in the spectra of Titan and the outer planetsAN 1977:180418In response to the observations of the UV deficiencies shown by all of the outer planets and Titan, models were proposed to explain the low albedos by absorption by particles in the upper atms. of these objects. These particles are generally believed to be photochem. formed from gases in the upper atms., primarily CH4 and H2. Such processes may also be operative on Titan. The results of some lab. expts. of the proton irradn. of mixts. of gases including CH4 H2, NH3, etc., have shown that liq. and solid materials are produced that are strong UV absorbers. However, the material produced from the CH4 + H2 mixt. was colorless, indicating that species contg. elements other thana C and H are necessary for the prodn. of color. Two such elements are N (as NH3 or N2) and S (as H2S) and colored materials were produced from such mixts. None of these materials has spectral properties identical to those shown by the planets. Therefore it is necessary that mixts. (and/or cloud layers) of the photochem. materials be present. [on SciFinder (R)]& Scattergood, Thomas Owen, Tobias Icarus304. 780-8  1977CAN 86:180418 73-7 Spectra by Absorption, Emission, Reflection, or Magnetic Resonance, and Other Optical Properties Dep. Earth Space Sci.,State Univ. New York,Stony Brook,NY,USA. Journal 0019-1035 written in English. 7664-41-7; 7727-37-9; 7783-06-4 Role: USES (Uses) (as source of UV-absorbing materials in planetary atm.); 74-82-8 Role: RCT (Reactant), RACT (Reactant or reagent) (reaction of, with hydrogen and other gases as source of UV absorbing materials in planets)RKPlanets (UV absorbing materials in, source of) planet UV absorbing materialo .'Organic chemistry in Titan's atmosphere$AN 1983:110784A review, with 5 refs., on the chem. of CH4 in Titan's atm., the compn. of dust that comprises Titan's haze layer, and isotope fractionation in planetary atms. [on SciFinder (R)]Scattergood, Thomasl NASA,Ames,IA,USA.atnCAN 98:110784 53-0 Mineralogical and Geological Chemistry Report; General Review 0191-7811 written in English. 679-97 1982Planets (atm. of, isotope fractionation in); Planets (Saturn, Titan satellite, atm. of, org. chem. of) review Titan atm org chem; planet atm isotope fractionation review; methane chem Titan atm reviewf`Gas chromatographic instrumentation for the analysis of aerosols and gases in Titan's atmosphereAN 1987:226770d]During the next decade or so, NASA, in conjunction with the European Space Agency, plans to send a spacecraft to the Saturnian system so that local studies of Saturn and its satellite, Titan, can be made. In order to study the atm. of Titan, analyses of both aerosols and gases will have to be made. To accomplish this, gas chromatog. instrumentation for the collection and anal. of org. gases and aerosols in Titan's atm. is being developed. The aerosols will be collected and then subjected to pyrolysis gas chromatog. (GC). Results using a simple GC system and tholin, made by subjecting a nominal Titan mixt. (96.8% N2, 3% CH4, 0.2% H2) to laser-supported shocks, show that many compds., including hydrocarbons and simple nitriles, can be identified by this technique. Atm. gases will be collected using large vol. (>10 cm3) sample loops and then analyzed by gas chromatog. Large vol. samples are required because the ambient pressures, where the probe instruments are first deployed, will be low (<10 mbar). Preliminary studies using a 20 cm3 sampling system and a very sensitive metastable ionization detector show that hydrocarbon components at the 10 ppb level can be detected. Work will continue to improve GC sensitivity, minimize anal. time, and develop interfaces with suitable sample collectors for anal. of atmospheres by future spacecraft. [on SciFinder (R)]RKScattergood, T. W. Valentin, J. R. O'Hara, B. J. Kojiro, D. R. Carle, G. C.l("Journal of Geophysical Research, BCAN 106:226770 80-2 Organic Analytical Chemistry Dep. Earth Space Sci.,State Univ. New York,Stony Brook,NY,USA. Journal 0196-6936 written in English.92B4 E723-8 1987JDAerosols (anal. of, from atm. of Titan, gas chromatog. instrumentation for); Chromatographs (for anal. of aerosols and org. gases in atm. of Titan); Sampling apparatus (for atm. of Titan); Hydrocarbons; Nitriles Role: ANST (Analytical study) (identification of, in atm. of Titan, gas chromatog. instrumentation for); Planets (Saturn, Titan satellite, anal. of atm. of, gas chromatog. instrumentation for) Titan atm analysis gas chromatograph; Saturn atm analysis gas chromatograph; org gas identification Titan atm; hydrocarbon identification Titan atm; aerosol analysis Titan atmb[Scattergood, T.W., C.P.McKay, W.J.Borucki, L.P.Giver, H.V.Ghyseghem, J.E.Parris, S.L.Miller 1989zsProduction of Organic Compounds in Plasmas: A Comparison among Electric Sparks, Laser-Induced Plasmas, and UV Lightr Icarus81413--328.'experiment, Plasmas, spark, LIP, UV, GC2.'Scattergood, T.W., E.Y. Lau, B.M. Stone 19921. Laboratory Investigations of Shapes, Size Distributions, and Aggregation of Particles Produced by UV Photolysis of Model Titan Atmosphere Icarus99 98-105D>experiment, UV, size distribution, acetylene, hydrogen cyanide1989zsProduction of Organic Compounds in Plasmas: A Comparison among Electric Sparks, Laser-Induced Plasmas, and UV Lightr Icarus81413--328.'experiment, Plasmas, spark, LIP, UV, GC2.'Scattergood, T.W., E.Y. Lau, B.M. Stone 19921. Laboratory Investigations of Shapes, Size Distributions, and Aggregation of Particles Produced by UV Photolysis of Model Titan Atmosphere Icarus99 98-105D>experiment, UV, size distribution, acetylene, hydrogen cyanide rtance of phase changes in Titan's lower atmosphere. Tools for the study of nucleationANTitan's upper ionosphereAN 1991:147493As a result of electron impact ionization and photoionization, an ionosphere should be built up at the high-altitude region of Titan's atm. From a simple consideration of the Chapman layer theory, the peak electron d. can be detd. to be ~5 * 103 cm-3 at .apprx.1200 km altitude. The complex ion-mol. reactions in the N2-CH4 atmosphere would lead to a mixt. of N2+, CH3+, C2H5+, and H2CN+ ions as the major ion species in the upper ionosphere. The new calcns. presented here also predict the presence of significant amts. of CH5+, N2H+, C2H2+, and C2H3+ ions (i.e., ni ~10-100 cm-3) near the ionospheric peak. Because of fast ion-neutral reactions with CH4 and N2, the no. d. of the Ar+ ions would not exceed a value of >10 cm-3 in the upper ionosphere if Ar has a mixing ratio .apprx.10-2 near the homopause. Interaction with the partially corotating magnetospheric plasma could lead to a significant modification of the ionospheric profile in the high altitudes. The ionospheric flow dynamics are studied in the limits of one-fluid mass-loaded flow and of diffusion-convection approxn. Both approaches show that ion-neutral friction acts as a cushion against plasma streaming effects. [on SciFinder (R)] Ip, W. H.)Astrophysical Journal  362P1, Pt. 1 354-63 1990CAN 114:147493 53-9 Mineralogical and Geological Chemistry Max-Planck-Inst. Aeron.,Katlenburg,Germany. Journal 0004-637X written in English. 74-82-8 (Methane); 74-84-0 (Ethane); 74-85-1 (Ethene); 74-86-2 (Acetylene); 75-05-8 (Acetonitrile); 460-19-5 (Ethanedinitrile); 1333-74-0 (Hydrogen); 7727-37-9 (Nitrogen); 12184-90-6 (Hydrogen ion (H21+); 12357-66-3; 12385-13-6 (Atomic hydrogen); 12539-57-0 (Cyanogen ion(1+); 12601-62-6 (Hydrocyanic acid ion(1+); 13966-04-6 (Nitrogen, ion (N21+); 14158-23-7 (Nitrogen, ion (N1+); 14531-53-4 (Methylium); 14604-48-9 (Ethenylium); 15091-72-2 (Methylene, ion (CH21+); 15135-49-6; 16456-59-0 (Ethynylium); 17778-88-0 (Atomic nitrogen); 20741-88-2 (Methane, ion (CH41+); 21107-92-6; 24361-82-8 (Methyliumylidene); 25215-44-5; 25641-79-6; 37354-81-7; 76092-43-8; 76619-90-4; 81643-07-4; 98499-70-8; 104233-69-4; 118090-84-9 (1,2-Propadien-3-ylium-1-ylidene); 129066-65-5 Role: OCCU (Occurrence) (in upper ionosphere, of Titan satellite of Saturn)piPlanets (Saturn, Titan satellite, upper ionosphere of, compn. of) upper ionosphere Titan satellite Saturn; .c matter in the atmosphere and on the surface of outer Solar system bodiesAN 2001:511265Many bodies in the outer Solar System display the presence of low-albedo materials. These materials, evident on the surface of asteroids, comets, Kuiper Belt objects, and their intermediate evolutionary step (Centaurs) are related to macromol. carbon-bearing materials such as polycyclic arom. hydrocarbons and org. materials such as methanol and related light hydrocarbons, embedded in a dark, refractory, photoprocRKFormation of amino acids from models of Titan and more oxidized atmospheresn AN 1983:49008Protein and nonprotein amino acids were synthesized following hydrolysis of products obtained by high-frequency discharge techniques applied to model atmospheres consisting of N2 as a N source together with CH4 and(or) CO2 as a C source. Highest yields were obtained in the absence of CO2 and from mixts. rich in CH4. Amino acids would indeed be expected on the frozen surface of Titan with its CH4-N2 atmosphere. [on SciFinder (R)]B7CAN 98:49008 6-3 General Biochemistry Jichi Med. Sch.,Minamikawachi,Japan. Journal 0302-1688 written in English. 74-82-8; 124-38-9; 7727-37-9 Role: BIOL (Biological study) (Titan model atm. contg., amino acid formation from); 56-12-2P; 56-40-6P; 56-41-7P; 56-45-1P; 56-84-8P; 56-86-0P; 61-90-5P; 72-18-4P; 73-32-5P; 107-95-9P; 107-97-1P; 305-62-4P; 515-94-6P; 2835-81-6P; 6600-40-4P Role: BSU (Biological study, unclassified), MFM (Metabolic formation), BIOL (Biological study), FORM (Formation, nonpreparative), PREP (Preparation) (formation of, in Titan model atm.)eTNAmino acids Role: BSU (Biological study, unclassified), MFM (Metabolic formation), BIOL (Biological study), FORM (Formation, nonpreparative) (formation of, in Titan model atm.); Atmosphere (reducing, amino acid formation in); Planets (Saturn, Titan satellite of, amino acid formation from model atm. of) amino acid formation Titan atmXQAerosols in Titan's atmosphere: models, sampling techniques and chemical analysis AN 1991:412662There are 2 kinds of particles in the atm. of Titan: a photochem. aerosol formed at high altitude (~400 km) through dissocn. of hydrocarbons by solar photons and charged particles of the Saturn magnetosphere slowly pptg. through the stratosphere, and particles of condensed hydrocarbons and nitriles in the lower stratosphere, below 80 km (with perhaps CH4 clouds between 10 and 40 km). New models of aerosols have been worked out. In the stratosphere, the variations of the mean radius and concn. can be described by resolving the set of microphys. equations in relation to the obsd. extinction profiles of the hazes. Another method is to use an Eulerian modeling which gives as a function of time the evolution of the size distribution for all altitudes by applying microphys. to all space. From 62 km and down into the troposphere, the strong condensation of ethane, methane and other gases modify the processes governing the evolution of aerosols. [on SciFinder (R)]BSpatially resolved images of Titan by means of adaptive optics Icarus 129n 482 - 497yrvations of planetary and satellite atmospheres and surfacesAN 2001:867015~wThe full opening of the submillimeter range with the operation of Herschel is expected to prove very useful f