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I-Volatile kwaye ityebile kwizinto eziphilayo, i-asteroids yohlobo lwe-C inokuba yenye yezona zinto ziphambili zamanzi eMhlabeni.Okwangoku, ii-chondrites ezithwala i-carbon zinika eyona ngcamango ilungileyo yokwakheka kweekhemikhali, kodwa ulwazi malunga neemeteorite lugqwethiwe: kuphela ezona ntlobo zomelele zisinda xa zingena kwiatmosfera emva koko zinxibelelana nokusingqongileyo komhlaba.Apha sibonisa iziphumo zophononongo oluneenkcukacha lwevolumetric kunye ne-microanalytical ye-particle ephambili ye-Ryugu ehanjiswe kuMhlaba yi-Hayabusa-2 spacecraft.Iincinci ze-Ryugu zibonisa ukuhambelana okusondeleyo ekubunjweni kweekhemikhali ezingabonakaliyo kodwa ezitshintshiweyo zamanzi zeCI (uhlobo lwe-Iwuna-uhlobo) lwe-chondrites, ezisetyenziswa ngokubanzi njengesalathisi sokubunjwa ngokubanzi kwenkqubo yelanga.Lo mzekelo ubonisa ubudlelwane obuntsonkothileyo besithuba phakathi kwezinto eziphilayo ezityebileyo ze-aliphatic kunye ne-silicates eleleyo kwaye ibonisa ubushushu obuphezulu obumalunga ne-30 °C ngexesha lokhukuliseko lwamanzi.Sifumene ubuninzi be-deuterium kunye ne-diazonium ehambelana nemvelaphi ye-extrasolar.Amasuntswana e-Ryugu zezona zinto zingangcolisekanga nezingohlulwahlulwayo zakha zafundwa kwaye zilungele ukubunjwa kwenkqubo yelanga.
Ukusukela ngoJuni ka-2018 ukuya kuNovemba ka-2019, iArhente ye-Aerospace Exploration Agency's (JAXA) Hayabusa2 yesiphekepheke seHayabusa2 yenze uphando olubanzi olukude kwi-asteroid Ryugu.Idatha evela kwi-Near Infrared Spectrometer (NIRS3) e-Hayabusa-2 icebisa ukuba i-Ryugu inokuqulunqwa ngento efana ne-thermal kunye / okanye i-shock-metamorphic carbonaceous chondrites.Umdlalo osondeleyo ngu-CY chondrite (uhlobo lwe-Yamato) 2. I-albedo ephantsi ye-Ryugu inokuchazwa ngokubakho kwenani elikhulu lezinto ezityebileyo ze-carbon, kunye nobukhulu be-particle, i-porosity, kunye nemiphumo yemozulu yendawo.I-spacecraft ye-Hayabusa-2 yenza i-landings ezimbini kunye nokuqokelela isampulu kwi-Ryuga.Ngexesha lokufika kokuqala nge-21 kaFebruwari 2019, kwafunyanwa izinto ezingaphezulu, ezazigcinwe kwindawo A ye-capsule yokubuyisela, kwaye ngexesha lokufika kwesibini ngoJulayi 11, 2019, imathiriyeli yaqokelelwa kufuphi ne-crater eyenziweyo eyenziwe yimpembelelo encinci ephathekayo.Ezi sampuli zigcinwe kwi-Ward C. Ukubonakaliswa kokuqala okungonakalisi kweengqungquthela kwiSigaba 1 kumagumbi akhethekileyo, ahlambulukileyo kwaye acocekileyo azaliswe yi-nitrogen kwiindawo ezilawulwa yi-JAXA zibonise ukuba iinqununu zeRyugu zazifana kakhulu ne-CI4 chondrites kwaye zibonise "amanqanaba ahlukeneyo okuguquguquka"3.Ukuhlelwa okubonakalayo okuchaseneyo kwe-Ryugu, okufana ne-CY okanye i-CI chondrites, kunokusombululwa kuphela nge-isotopic eneenkcukacha, i-elemental, kunye ne-mineralogical characterization ye-Ryugu particles.Iziphumo ezithiwe thaca apha zibonelela ngesiseko esiluqilima sokumisela ukuba yeyiphi kwezi ngcaciso zimbini zokuqala zokwakheka ngokubanzi kwe-asteroid Ryugu enokwenzeka.
Iipellets ezisibhozo zeRyugu (malunga ne-60mg iyonke), ezine zisuka kwiChamber A nezine ezivela kwiChamber C, zabelwa kwiSigaba 2 sokulawula iqela leKochi.Injongo ephambili yophando kukucacisa indalo, imvelaphi kunye nembali yendaleko ye-asteroid Ryugu, kunye nokubhala ukufana kunye nokungafani kunye neminye imizekelo eyaziwayo ye-extraterrestrial efana ne-chondrites, i-particle interplanetary dust (IDPs) kunye ne-comets ezibuyayo.Iisampulu eziqokelelwe yi-NASA's Stardust mission.
Uhlalutyo olunzulu lwemineralogical yeenkozo zeRyugu ezintlanu (A0029, A0037, C0009, C0014 kunye neC0068) zibonise ukuba zidibaniswe ngokucokisekileyo kunye ne-coarse-grained phyllosilicates (~ 64-88 vol.%; Umzobo 1a, b, i-Supplement1).kunye netafile eyongezelelweyo 1).I-coarse-grained phyllosilicates iyenzeka njenge-pinnate aggregates (ukuya kumashumi ee-microns ngobukhulu) kwiimatriki ezicolekileyo, ezityebileyo ze-phyllosilicate (ezingaphantsi kwee-microns ezimbalwa ngobukhulu).Amasuntswana e-silicate afakwe ileyikeyi zii-symbionts ze-serpentine-saponite (Umfanekiso 1c).I-(Si + Al)-Mg-Fe imephu ibonisa kwakhona ukuba i-matrix ye-silicate ene-bulk layered inokwakheka okuphakathi phakathi kwenyoka kunye ne-saponite (Umfanekiso 2a, b).I-matrix ye-phyllosilicate iqukethe amaminerali e-carbonate (~ 2-21 vol.%), amaminerali e-sulfide (~ 2.4-5.5 vol.%), kunye ne-magnetite (~ 3.6-6.8 vol.%).Enye yeengqungquthela ezihlolwe kulolu cwaningo (i-C0009) iqulethe ixabiso elincinci (~ 0.5 vol.%) ye-silicates ye-anhydrous (i-olivine kunye ne-pyroxene), enokukunceda ukuchonga umthombo wemithombo eyenza i-Ryugu stone5 eluhlaza.Le silicate ye-anhydrous inqabile kwiipellets ze-Ryugu kwaye zachongwa ngokuqinisekileyo kwi-C0009 pellet.Iikhabhonathi zikhona kwi-matrix njengamaqhekeza (ngaphantsi kwamakhulu ambalwa emicrons), ubukhulu becala idolomite, enemilinganiselo encinci yecalcium carbonate kunye nebrinell.I-Magnetite yenzeka njengamasuntswana azimeleyo, iiframboids, iiplakhi, okanye i-spherical aggregates.I-Sulfides ibonakaliswe kakhulu yi-pyrrhotite ngendlela engaqhelekanga yeeprisms / iipleyiti okanye i-laths.I-matrix iqulethe inani elikhulu le-submicron pentlandite okanye ngokudibanisa ne-pyrrhotite. Izigaba ezityebileyo zekhabhoni (<10 µm ngobukhulu) zenzeka kuyo yonke indawo kwi-matrix ene-phyllosilicate-rich. Izigaba ezityebileyo zekhabhoni (<10 µm ngobukhulu) zenzeka kuyo yonke indawo kwi-matrix ene-phyllosilicate-rich. Богатые углеродом фазы (размером <10 мкм) встречаются повсеместно в богатой филлосиликатами матрице. Izigaba ezityebileyo zekhabhoni (<10 µm ngobukhulu) zenzeka kuyo yonke indawo kwi-matrix ene-phyllosilicate-rich.富含碳的相（尺寸<10 µm）普遍存在于富含层状硅酸盐的基质中。富含碳的相（尺寸<10 µm）普遍存在于富含层状硅酸盐的基质中。 Богатые углеродом фазы (размером <10 мкм) преобладают в богатой филлосиликатами матрице. Izigaba ezityebileyo zeCarbon (<10 µm ngobukhulu) zihamba phambili kwi-matrix ecebileyo ye-phyllosilicate.Ezinye iiminerali ezincedisayo ziboniswa kwi-Supplementary Table 1. Uluhlu lwamaminerali olunqunywe kwi-X-ray ye-diffraction pattern ye-C0087 kunye ne-A0029 kunye ne-A0037 umxube ihambelana kakhulu nesigqibo kwi-CI (i-Orgueil) i-chondrite, kodwa ihluke kakhulu kwi-CY kunye ne-CM (i-Mippleregument ye-data ye-Migheri kunye ne-Find Figure) eyandisiweyo (i-Migheri 1 kunye nohlobo lwe-Firegued ye-Findregued).Umxholo opheleleyo we-element ye-Ryugu grains (A0098, C0068) iphinda ihambelane ne-chondrite 6 CI (idatha eyandisiweyo, i-Fig. 2 kunye ne-Supplementary Table 2).Ngokwahlukileyo, i-chondrites ye-CM iyancipha kwizinto ezinokulinganisela kunye neziguquguqukayo, ngakumbi i-Mn kunye ne-Zn, kwaye iphezulu kwizinto eziphikisayo7.Ugxininiso lwamasuntswana athile luyohluka kakhulu, olunokuba luphawu lwendalo engafaniyo yesampulu ngenxa yobungakanani obuncinci bamasuntswana azimeleyo kunye nesiphumo somkhethe wesampulu.Zonke iimpawu ze-petrological, mineralological and elemental zibonisa ukuba iinkozo zeRyugu zifana kakhulu ne-chondrites CI8,9,10.Okuphawulekayo kukungabikho kwe-ferrihydrite kunye ne-sulfate kwiinkozo ze-Ryugu, ebonisa ukuba ezi zimbiwa kwi-CI chondrites zenziwe yimozulu yomhlaba.
a, Umfanekiso we-X-reyi ehlanganisiweyo we-Mg Kα (obomvu), u-Ca Kα (oluhlaza), i-Fe Kα (ebhlowu), kunye ne-S Kα (etyheli) icandelo elomileyo elikhazimlisiweyo C0068.Iqhezu liquka i-silicates eleleyo (obomvu: ~ 88 vol%), i-carbonates (idolomite; ukukhanya okuluhlaza: ~ 1.6 vol%), imagnetite (blue: ~ 5.3 vol%) kunye neesulfides (tyheli: sulfide = ~ ~ 2.5% vol. isincoko. b, umfanekiso wengingqi yecontour kwi-backscattered vol. Imagnethi, ijusi -ilitye lesepha, iSrp - inyoka c, i-electron microscopy (TEM) yosasazo oluphezulu (TEM) umfanekiso wesaponite-serpentine intergrowth ebonisa amabhanti elattice enyoka kunye ne-saponite ye-0.7 nm kunye ne-1.1 nm, ngokulandelelanayo.
Ukubunjwa kwe-matrix kunye ne-layer silicate (kwi-%) ye-Ryugu A0037 (izangqa ezibomvu eziqinileyo) kunye ne-C0068 (iingqungquthela eziluhlaza okwesibhakabhaka) ziboniswe kwi-(Si + Al) -Mg-Fe ternary system.a, Iziphumo ze-Electron Probe Microanalysis (EPMA) ezicwangcisiweyo malunga ne-CI chondrites (Ivuna, Orgueil, Alais) i-16 eboniswe kwigrey ukuthelekisa.b, Ukuskena i-TEM (STEM) kunye ne-energy dispersive X-ray spectroscopy (EDS) uhlalutyo oluboniswe ngokuthelekisa ne-Orgueil9 kunye ne-Murchison46 meteorites kunye ne-hydrated IDP47.I-fine-grained and coarse-grained phyllosilicates yahlaziywa, igwema iincinci ezincinci ze-iron sulfide.Imigca echokoziweyo ku-a kunye no-b ibonisa imigca yokuchithwa kwe-saponite kunye nenyoka.Ukubunjwa kwe-iron-rich rich in a kungenzeka ngenxa ye-submicron iron sulfide grains ngaphakathi kweenkozo ze-silicate ezilayishiwe, ezingenakukhutshwa ngaphandle kwesisombululo sesithuba sohlalutyo lwe-EPMA.Amanqaku edatha anomxholo we-Si ophezulu kune-saponite kwi-b inokubangelwa kubukho be-nanosized amorphous silicon-rich material in the interstices of the phyllosilicate layer.Inani lohlalutyo: N=69 ye-A0037, N=68 ye-EPMA, N=68 ye-C0068, N=19 ye-A0037 kunye ne-N=27 ye-C0068 ye-STEM-EDS.c, imephu ye-isotope ye-trioxy particle Ryugu C0014-4 xa kuthelekiswa nemilinganiselo ye-chondrite CI (Orgueil), CY (Y-82162) kunye neenkcukacha zoncwadi (CM kunye neC2-ung) 41,48,49.Sifumene idatha ye-Orgueil kunye ne-Y-82162 meteorites.I-CCAM ngumgca we-anhydrous carbonaceous chondrite minerals, i-TFL ngumgca wokuhlula umhlaba.d, Δ17O kunye ne-δ18O iimephu ze-Ryugu i-particle C0014-4, i-CI chondrite (i-Orgueil), kunye ne-CY chondrite (Y-82162) (esi sifundo).Δ17O_Ryugu: Ixabiso le-Δ17O C0014-1.Δ17O_Orgueil: I-Avareji ye-Δ17O yexabiso le-Orgueil.Δ17O_Y-82162: Umyinge Δ17O ixabiso le-Y-82162.Idatha ye-CI kunye ne-CY evela kwiincwadi ze-41, i-48, i-49 nazo ziboniswa ukuthelekisa.
Uhlalutyo lwe-isotope ye-Mass of oxygen lwenziwa kwi-1.83 mg yesampula yezinto ezithathwe kwi-granular C0014 nge-laser fluorination (Iindlela).Ukuthelekisa, siqhube iikopi ezisixhenxe ze-Orgueil (CI) (ubunzima bubonke = 8.96 mg) kunye neekopi ezisixhenxe ze-Y-82162 (CY) (ubunzima obupheleleyo = 5.11 mg) (Itheyibhile eyongezelelweyo 3).
Kwikhiwane.I-2d ibonisa ukwahlukana okucacileyo kwe-Δ17O kunye ne-δ18O phakathi kobunzima be-particle ye-Orgueil kunye ne-Ryugu xa kuthelekiswa ne-Y-82162.I-Δ17O ye-Ryugu C0014-4 i-particle iphezulu kune-Orgeil particle, nangona i-overlap kwi-2 sd.Amasuntswana e-Ryugu anexabiso eliphezulu le-Δ17O xa kuthelekiswa ne-Orgeil, enokuthi ibonise ungcoliseko lwalo lwamva lwehlabathi ukususela ekuweni kwayo ngo-1864. Imo yezulu kwimekobume yomhlaba11 ibangela ukudityaniswa kweoksijini yomoya, izisa uhlalutyo olupheleleyo kufutshane nomgca womhlaba (TFL).Esi sigqibo sihambelana nedatha ye-mineralogical (exoxiwe ngaphambili) ukuba i-Ryugu iinkozo aziqukethe i-hydrates okanye i-sulfates, ngelixa i-Orgeil yenza.
Ngokusekelwe kwidatha ye-mineralogical engentla, ezi ziphumo zixhasa umbutho phakathi kwe-Ryugu grains kunye ne-CI chondrites, kodwa ulawula umbutho we-CY chondrites.Inyaniso yokuba iinkozo ze-Ryugu azihambelani ne-CY chondrites, ebonisa iimpawu ezicacileyo ze-mineralogy ye-dehydration, iyamangalisa.Uqwalaselo lwe-Orbital lweRyugu lubonakala lubonisa ukuba iye yaphelelwa ngamanzi emzimbeni kwaye ke ngoko kusenokwenzeka ukuba yenziwe ngezinto zeCY.Izizathu zalo mahluko ubonakalayo azikacaci.Uhlalutyo lwe-oksijini ye-isotope yezinye iinqununu ze-Ryugu zichazwe kwiphepha elihambelanayo 12. Nangona kunjalo, iziphumo zolu lwazi olwandisiweyo lwedatha lukwahambelana nombutho phakathi kweengqungquthela zeRyugu kunye ne-CI chondrites.
Ukusebenzisa iindlela ezilungelelanisiweyo ze-microanalysis (i-Supplementary Fig. 3), siye savavanya ukuhanjiswa kwendawo ye-organic carbon phezu kwendawo yonke ye-ion egxininisiweyo ye-beam fraction (FIB) C0068.25 (Figs. 3a-f).Isakhiwo esihle i-X-ray yokufunxa i-spectra yekhabhoni (NEXAFS) kumda okufutshane kwicandelo C0068.25 ebonisa amaqela asebenzayo amaninzi - i-aromatics okanye i-C=C (285.2 eV), i-C=O (286.5 eV), i-CH (287.5 eV) kunye ne-C (=O)O (288.8 i-eg 2 i-eV) -i-288.8 i-eg eV isakhiwo . ), oku kuthetha iqondo eliphantsi lokutshintsha kwe-thermal.I-CH enamandla kakhulu (i-287.5 eV) ye-party organics ye-C0068.25 ihluke kwi-insoluble organics ye-carbonaceous chondrites efundwe ngaphambili kwaye ifana kakhulu ne-IDP14 kunye ne-cometary particles efunyenwe yi-Stardust mission.Incopho ye-CH eqinile kwi-287.5 eV kunye ne-aromatics ebuthakathaka kakhulu okanye i-C = C i-peak kwi-285.2 eV ibonisa ukuba i-organic compounds zizityebi kwii-aliphatic compounds (Umfanekiso 3a kunye ne-Supplementary Fig. 3a).Iindawo ezityebileyo kwiikhompawundi ze-aliphatic eziphilayo zifakwe kwi-phyllosilicates ye-coarse-grained, kunye nakwiindawo ezinevumba elibi (okanye i-C = C) ye-carbon structure (Fig. 3c, d).Ngokwahlukileyo, i-A0037,22 (i-Supplementary Fig. 3) ibonise ngokuyinxenye umxholo ophantsi wemimandla ye-aliphatic carbon-rich.I-mineralogy engaphantsi kwezi zinkozo zizityebi kwi-carbonates, efana ne-chondrite CI 16, ebonisa ukuguqulwa okubanzi kwamanzi omthombo (iThebhile eyongezelelweyo 1).Iimeko ze-oxidizing ziya kuthanda ukugxila okuphezulu kwe-carbonyl kunye namaqela asebenzayo e-carboxyl kwiikhompawundi ze-organic ezinxulumene ne-carbonates.Ukuhanjiswa kwe-submicron yezinto eziphilayo kunye ne-aliphatic carbon structures kunokwahluka kakhulu ekuhanjisweni kwe-silicates ene-coarse-grained layered silicates.Iingcebiso ze-aliphatic organic compounds ezinxulumene ne-phyllosilicate-OH zifunyenwe kwi-meteorite ye-Tagish Lake.Idatha edibeneyo ye-microanalytical ibonisa ukuba izinto eziphilayo ezizityebi kwi-aliphatic compounds zingasasazeka kwi-C-type asteroids kwaye ihambelana ngokusondeleyo ne-phyllosilicates.Esi sigqibo sihambelana neengxelo zangaphambili ze-aliphatic / i-aromatic CHs kwi-Ryugu particles eboniswe yi-MicroOmega, i-microspectral microscope ekufutshane ne-infrared.Umbuzo obalulekileyo kunye ongasonjululwanga kukuba ingaba iipropathi ezizodwa ze-aliphatic carbon-rich rich organic compounds ezinxulumene ne-coarse-grained phyllosilicates eziqatshelwe kolu cwaningo zifumaneka kuphela kwi-asteroid Ryugu.
a, NEXAFS carbon spectra normalized to 292 eV in the aromamatic (C=C) kummandla otyebileyo (red), kummandla otyebileyo aliphatic (green), kunye matrix (blue).Umgca ongwevu yi Murchison 13 i-insoluble organic spectrum xa kuthelekiswa.okanye, iyunithi yolamlo.b, Ukuskena ukuhanjiswa kwe-X-ray microscopy (STXM) umfanekiso obonakalayo wekhabhoni ye-K-edge ebonisa ukuba icandelo lilawulwa yikhabhoni.c, iploti ye-RGB edibeneyo enevumba elimnandi (C=C) imimandla etyebileyo (ebomvu), imimandla etyebileyo ye-aliphatic (eluhlaza), kunye ne-matrix (ebhlowu).d, izinto eziphilayo ezityebileyo kwiikhompawundi ze-aliphatic zigxininiswe kwi-coarse-grained phyllosilicate, indawo yandiswa ukusuka kwiibhokisi ezinamachaphaza amhlophe ku-b kunye no-c.e, iinanospheres ezinkulu (ng-1) kwindawo eyandisiweyo ukusuka kwibhokisi enamachokoza amhlophe ku-b no-c.Kuba: pyrrhotite.Pn: nickel-chromite.f, Nanoscale Secondary Ion Mass Spectrometry (NanoSIMS), Hydrogen (1H), Carbon (12C), kunye neNitrogen (12C14N) imifanekiso esisiseko, 12C/1H imifanekiso yomlinganiselo wento, kunye nomnqamlezo δD, δ13C, kunye δ15N imifanekiso ye-isotopu - Icandelo PG-3C kunye ne-presolar 4 ye-presolar Tahlulo etyebileyo: i-presolar Tablement 4 etyebileyo (i-presolar 1).
Izifundo ze-Kinetic zokuthotywa kwezinto eziphilayo kwi-Murchison meteorites zinokunika ulwazi olubalulekileyo malunga nokusabalalisa okungafaniyo kwe-aliphatic organic matter etyebileyo kwiinkozo zeRyugu.Olu pho nonongo lubonisa ukuba i-aliphatic CH bonds kwi-organic matter iqhubeka ukuya kubushushu obuphezulu malunga ne-30 ° C kumzali kunye / okanye utshintsho kunye nobudlelwane bexesha lobushushu (umz. iminyaka engama-200 kwi-100 ° C kunye ne-0 ° C iminyaka eyi-100 yezigidi) ..Ukuba i-precursor ayitshisi kwiqondo lokushisa elinikeziweyo ngaphezu kwexesha elithile, ukusabalalisa kwangaphambili kwe-aliphatic organics rich in phyllosilicate kunokugcinwa.Nangona kunjalo, utshintsho lwamanzi omthombo lwamanzi lunokwenza kube nzima ukutolika, njengoko i-carbonate-rich A0037 ayibonisi nayiphi na imimandla ye-carbon-rich aliphatic ehambelana ne-phyllosilicates.Olu tshintsho lobushushu luphantsi luhambelana nobukho becubic feldspar kwiinkozo zeRyugu (Itheyibhile eyoNgezelelweyo 1) 20.
I-Fraction C0068.25 (ng-1; Figs. 3a–c,e) iqulethe i-nanosphere enkulu ebonisa ukunuka kakhulu (okanye i-C=C), i-aliphatic ephakathi, kunye ne-spectra ebuthathaka ye-C (=O) O kunye ne-C=O..Ukutyikitywa kwekhabhoni ye-aliphatic ayihambelani nesignesha ye-bulk i-insoluble organics kunye ne-organic nanospheres ehambelana ne-chondrites (Umfanekiso 3a) 17,21.Uhlalutyo lwe-Raman kunye ne-infrared spectroscopic ye-nanospheres eLake Tagish lubonise ukuba lubandakanya i-aliphatic kunye ne-oxidized organic compounds kunye ne-disordered polycyclic aromatics organic compounds kunye nesakhiwo esiyinkimbinkimbi22,23.Ngenxa yokuba i-matrix ejikelezileyo iqulethe izinto eziphilayo ezityebileyo kwiikhompawundi ze-aliphatic, ukutyikitywa kwekhabhoni ye-aliphatic kwi-ng-1 inokuba yinto yohlalutyo.Kuyathakazelisa ukuba i-ng-1 iqulethe i-silicates e-amorphous embedded (Umfanekiso 3e), isicatshulwa esingakabikwa kuyo nayiphi na i-organics extraterrestrial.I-amorphous silicates ingaba yindalo ye-ng-1 okanye isiphumo se-amorphization ye-silicates enamanzi / i-anhydrous nge-ion kunye / okanye i-electron beam ngexesha lokuhlalutya.
I-NanoSIMS imifanekiso ye-ion yecandelo le-C0068.25 (umzobo 3f) ubonisa utshintsho olufanayo kwi-δ13C kunye ne-δ15N, ngaphandle kweenkozo ze-presolar ezinobuncwane obukhulu be-13C ye-30,811 ‰ (PG-1 kumfanekiso we-δ13C kwi-Fig. 3f) (I-Supplementary Table).Imifanekiso ye-X-ray yokuqala yengqolowa kunye ne-high-resolution TEM imifanekiso ibonisa kuphela i-carbon concentration kunye nomgama phakathi kwe-basal planes ye-0.3 nm, ehambelana negraphite.Kuyaphawuleka ukuba amaxabiso δD (841 ± 394‰) kunye δ15N (169 ± 95‰), etyetyiswe kwizinto eziphilayo aliphatic ezinxulumene phyllosilicates coarse-grained, zijika zibe phezulu kancinci kunomndilili wonke ummandla C (δD = 539 ‰ ± 1).‰, δ15N = 67 ± 15 ‰) kwi-C0068.25 (iTheyibhile eyoNgezelelweyo 4).Olu qwalaselo lubonisa ukuba i-aliphatic-rich organics in coarse-grained phyllosilicates inokuba yeyokuqala ngakumbi kunendalo engqongileyo, kuba le yokugqibela inokuthi itshintshe i-isotopic kunye namanzi ajikelezileyo kumzimba wokuqala.Kungenjalo, olu tshintsho lwe-isotopic lunokunxulumana nenkqubo yokuqala yokwakheka.Kutolikwa ukuba i-silicates ene-fine-grained layered kwi-CI chondrites yenziwe ngenxa yokuguqulwa okuqhubekayo kweqoqo lokuqala le-coarse-grained anhydrous silicate.I-aliphatic-rich-rich organic matter inokuba yenziwe kwi-precursor molecules kwi-protoplanetary disk okanye i-interstellar medium ngaphambi kokusekwa kwenkqubo yelanga, kwaye emva koko yatshintshwa kancinane ngexesha lokutshintsha kwamanzi kwi-Ryugu (enkulu) yomzimba womzali. Ubungakanani (<1.0 km) be-Ryugu buncinci kakhulu ukugcina ngokwaneleyo ubushushu bangaphakathi ukwenzela ukuguqulwa kwamanzi ukwenza iiminerali ezinama-hydrous25. Ubungakanani (<1.0 km) be-Ryugu buncinci kakhulu ukugcina ubushushu bangaphakathi ngokwaneleyo ukuguqulwa kwamanzi ukwenza iiminerali ezinama-hydrous25. Размер (<1,0 км) Рюгу слишком мал, чтобы поддерживать достаточное внутреннее тепло для водного изменения с образованием водных. Ubungakanani (<1.0 km) I-Ryugu incinci kakhulu ukugcina ubushushu bangaphakathi obaneleyo ukwenzela ukutshintsha kwamanzi ukwenza iiminerali zamanzi25. Ryugu 的尺寸（<1.0 公里）太小，不足以维持内部热量以进行水蚀变形成含水矿物25. Ryugu 的尺寸（<1.0 公里）太小，不足以维持内部热量以进行水蚀变形成含水矿物25. Размер Рюгу (<1,0 км) слишком мал, чтобы поддерживать внутреннее тепло для изменения воды с образованием водных минералов25. Ubungakanani beRyugu (<1.0 km) buncinci kakhulu ukuxhasa ubushushu bangaphakathi ukutshintsha amanzi ukwenza iiminerali zamanzi25.Ke ngoko, abanduleli beRyugu amashumi eekhilomitha ngobukhulu banokufuneka.Izinto eziphilayo ezityebileyo kwiikhompawundi ze-aliphatic zinokugcina izilinganiso ze-isotope zangaphambili ngenxa yokudibanisa ne-coarse-grained phyllosilicates.Nangona kunjalo, ubume be-isotopic abathwali abanobunzima buhlala bungaqinisekanga ngenxa yokudityaniswa okuntsonkothileyo kunye nokuthambileyo kwamacandelo ahlukeneyo kula maqhezu eFIB.Ezi zinokuba zizinto eziphilayo ezityebileyo kwiikhompawundi ze-aliphatic kwi-Ryugu granules okanye i-coarse phyllosilicates ezingqongileyo.Qaphela ukuba izinto eziphilayo phantse kuzo zonke i-carbonaceous chondrites (kubandakanywa ne-CI chondrites) zivame ukuba zizityebi kwi-D kune-phyllosilicates, ngaphandle kwe-CM Paris 24, i-26 meteorites.
Izilayidi zevolumu δD kunye ne-δ15N ye-FIB izilayi ezifunyenwe kwi-A0002.23 kunye ne-A0002.26, i-A0037.22 kunye ne-A0037.23 kunye ne-C0068.23, i-C0068.25 kunye ne-C0068.26 ye-FIB izilayi (iitotali zezinye izilayi ze-fib ze-compari ezisuka kwezinye ii-slices ezisixhenxe ze-FIBs ze-SIM kunye nezilayidi ezisixhenxe ze-FIBs ze-SIM). inkqubo yelanga iboniswe kwifig.4 (Itheyibhile eyoNgezelelweyo 4)27,28.Utshintsho lwevolumu kwi-δD kunye ne-δ15N kwiiprofayili ze-A0002, A0037, kunye ne-C0068 zihambelana nezo zi-IDP, kodwa ziphezulu kune-CM kunye ne-CI chondrites (umzobo 4).Qaphela ukuba uluhlu lwamaxabiso δD for Comet 29 isampuli (-240 ukuba 1655 ‰) mkhulu kunaleyo Ryugu.Imiqulu δD kunye ne-δ15N yeeprofayili ze-Ryukyu, njengomthetho, zincinci kune-avareji ye-comets yosapho lwe-Jupiter kunye nefu le-Oort (umzobo 4).Amaxabiso asezantsi e-δD e-CI chondrites angabonakalisa impembelelo yokungcoliseka komhlaba kwezi sampuli.Ukunikezelwa kwezinto ezifanayo phakathi kweeBells, iLake Tagish, kunye ne-IDP, i-heterogeneity enkulu kwi-δD kunye ne-δN ixabiso kwiincinci ze-Ryugu zingabonisa utshintsho kwiisignesha zokuqala ze-isotopic ze-organic and aqueous compositions kwinkqubo yokuqala yelanga.Utshintsho olufanayo lwe-isotopic kwi-δD kunye ne-δN kwi-Ryugu kunye neengqungquthela ze-IDP zibonisa ukuba zombini zinokuthi zenziwe kwizinto ezivela kumthombo ofanayo.Kukholelwa ukuba ii-IDPs zivela kwimithombo ye-cometary 14.Ke ngoko, iRyugu inokuthi iqulethe izinto ezifana ne-comet kunye / okanye ubuncinci isixokelelwano selanga sangaphandle.Nangona kunjalo, oku kunokuba nzima kunokuba sichaza apha ngenxa (1) umxube we-spherulitic kunye ne-D-rich yamanzi kumzimba womzali we-31 kunye (2) ne-comet's D / H ratio njengomsebenzi we-cometary 32.Nangona kunjalo, izizathu zokubonwa kwe-heterogeneity ye-hydrogen kunye ne-nitrogen isotopes kumasuntswana e-Ryugu aziqondwa ngokupheleleyo, ngokuyinxenye ngenxa yenani elilinganiselweyo lohlalutyo olukhoyo namhlanje.Iziphumo ze-hydrogen kunye ne-nitrogen isotope iinkqubo zisaphakamisa ukuba kungenzeka ukuba i-Ryugu iqulethe izinto ezininzi ezivela ngaphandle kwe-Solar System kwaye ngaloo ndlela inokubonisa ukufana okuthile kwi-comets.Iprofayile ye-Ryugu ayizange ibonise unxulumano lubonakalayo phakathi kwe-δ13C kunye ne-δ15N (iTheyibhile eyoNgezelelweyo yesi-4).
Ukubunjwa kwe-isotopic ye-H kunye ne-N ye-isotopic ye-Ryugu (izangqa ezibomvu: i-A0002, i-A0037; izangqa eziluhlaza okwesibhakabhaka: i-C0068) ihambelana nobukhulu belanga 27, i-Jupiter ithetha intsapho (JFC27), kunye ne-Oort cloud comets (OCC27), i-IDP28, kunye ne-carbonaceous chondrules.Ukuthelekiswa kwe-meteorite 27 (CI, CM, CR, C2-ung).Ukwakhiwa kwe-isotopic kunikwe kwiTheyibhile eyoNgezelelweyo yesi-4. Imigca echokoziweyo ngamaxabiso e-isotopu asemhlabeni ku-H kunye no-N.
Ukuthuthwa kwezinto eziguquguqukayo (umz. izinto eziphilayo kunye namanzi) ukuya eMhlabeni kuhlala kuyinkxalabo26,27,33.I-submicron ye-organic matter ehambelana ne-coarse phyllosilicates kwi-Ryugu particles ezichongiweyo kolu cwaningo lunokuba ngumthombo obalulekileyo wee-volatiles.Izinto eziphilayo kwi-coarse-grained phyllosilicates zikhuselwe kangcono kwi-degradation16,34 kunye nokubola35 kunezinto eziphilayo kwi-matrices ene-fine-grained.Ukuqulunqwa kwe-isotopic enzima ye-hydrogen kumasuntswana kuthetha ukuba akunakwenzeka ukuba ibe kuphela komthombo wokuguquguquka ohanjiswe kuMhlaba wokuqala.Ziyakwazi ukuxutywa kunye namacandelo kunye nokwakheka kwe-hydrogen isotopic elula, njengoko bekucetywayo kutshanje kwi-hypothesis yobukho bamanzi aqhutywa ngumoya welanga kwi-silicates.
Kolu phononongo, sibonisa ukuba i-CI meteorites, ngaphandle kokubaluleka kwe-geochemical njengabameli bendlela yonke yenkqubo yelanga, i-6,10 iisampulu ezingcolileyo zomhlaba.Sikwabonelela ngobungqina obuthe ngqo bokusebenzisana phakathi kwezinto ezityebileyo ze-aliphatic eziphilayo kunye neeminerali ze-hydrous ezingabamelwane kwaye sicebisa ukuba i-Ryugu inokuba ne-extrasolar material37.Iziphumo zolu phononongo zibonisa ngokucacileyo ukubaluleka kwesampulu ethe ngqo yeprotoasteroids kunye nesidingo sokuthutha iisampulu ezibuyisiweyo phantsi kweemeko ezingasebenziyo neziyinyumba.Ubungqina obunikwe apha bubonisa ukuba amasuntswana e-Ryugu ngokungathandabuzekiyo yenye yezona zinto zingangcoliswanga zenkqubo yelanga ekhoyo kuphando lwebhubhoratri, kwaye uphononongo olongezelelweyo lwale sampuli zixabisekileyo ngokungathandabuzekiyo luya kwandisa ukuqonda kwethu kweenkqubo zokuqala zelanga.Amasuntswana eRyugu awona mboniso ubalaseleyo wokubunjwa kwenkqubo yelanga.
Ukumisela i-microstructure eyinkimbinkimbi kunye neempawu zeekhemikhali zeesampuli ze-submicron scale, sasebenzisa i-synchrotron radiation-based computed tomography (SR-XCT) kunye ne-SR X-ray diffraction (XRD) -CT, FIB-STXM-NEXAFS-NanoSIMS-TEM uhlalutyo.Akukho kuthotywa, ungcoliseko ngenxa yeatmosfera yomhlaba, kwaye akukho monakalo osuka kumasuntswana acolekileyo okanye iisampulu zoomatshini.Okwangoku, siye saqhuba uhlalutyo lwe-volumetric olucwangcisiweyo sisebenzisa i-electron microscopy (SEM)-EDS, i-EPMA, i-XRD, uhlalutyo lwe-instrumental neutron activation (INAA), kunye nezixhobo ze-laser oxygen isotope fluorination.Iinkqubo zokuvavanya ziboniswe kwi-Supplementary Figure 3 kwaye uvavanyo ngalunye luchazwe kula macandelo alandelayo.
Amacandelo avela kwi-asteroid Ryugu yafunyanwa kwimodyuli ye-Hayabusa-2 yokungena kwakhona kwaye ihanjiswe kwi-JAXA Control Centre eSagamihara, eJapan, ngaphandle kokungcolisa umoya woMhlaba4.Emva kokubonakaliswa kweempawu zokuqala nezingonakalisi kwiziko elilawulwa yi-JAXA, sebenzisa izikhongozeli ezitywiniweyo zokuhambisa phakathi kwendawo kunye neengxowa zesampulu zesampulu (ikristale yesafire eyi-10 okanye eyi-15 mm ububanzi kunye nentsimbi engenasici, ngokuxhomekeke kubungakanani besampulu) ukunqanda ukuphazamiseka kokusingqongileyo.okusingqongileyo.y kunye/okanye izingcolisi zomhlaba (umz. umphunga wamanzi, ii-hydrocarbons, iigesi ze-atmospheric kunye namasuntswana amahle) kunye nongcoliseko olunqamlezayo phakathi kweesampulu ngexesha lokulungiswa kwesampulu kunye nothutho phakathi kwamaziko kunye neeyunivesithi38.Ukuphepha ukuthotywa kunye nongcoliseko ngenxa yentsebenziswano kunye neatmosfera yomhlaba (umphunga wamanzi kunye neoksijini), zonke iintlobo zokulungiselela isampula (kubandakanywa ukutshiphuzela ngetshizi yetantalum, usebenzisa isarha yedayimane yocingo olulungeleleneyo (Meiwa Fosis Corporation DWS 3400) kunye nokusika epoxy) ukulungiselela ukufakela) zaqhutywa kwiglovebox phantsi kwebhokisi yeglove phantsi ecocekileyo eyomileyo 60 ° ~ 1 ~ 200 ℃ inqaku le-200 C ~ 5 ).Zonke izinto ezisetyenzisiweyo apha zihlanjululwa kunye nokudibanisa kwamanzi e-ultrapure kunye ne-ethanol usebenzisa amaza e-ultrasonic amaza ahlukeneyo.
Apha sifunda i-National Polar Research Institute (NIPR) yokuqokelela i-meteorite ye-Antarctic Meteorite Research Centre (CI: Orgueil, CM2.4: Yamato (Y) -791198, CY: Y-82162 kunye neCY: Y 980115).
Ukudluliselwa phakathi kwezixhobo ze-SR-XCT, i-NanoSIMS, i-STXM-NEXAFS kunye nohlalutyo lwe-TEM, sisebenzise umnini wesampulu ye-ultrathin jikelele echazwe kwizifundo zangaphambili38.
Uhlalutyo lwe-SR-XCT lweesampuli ze-Ryugu lwenziwa ngokusebenzisa i-BL20XU / SPring-8 inkqubo edibeneyo ye-CT.Inkqubo edibeneyo ye-CT iqulethe iindlela ezahlukeneyo zokulinganisa: inkalo ebanzi yokujonga kunye nesisombululo esisezantsi (WL) imowudi yokubamba isakhiwo sonke sesampulu, inkalo encinci yokujonga kunye nesisombululo esiphezulu (NH) indlela yokulinganisa ngokuchanekileyo indawo yesampuli.umdla kunye ne-radiographs ukufumana iphethini ye-diffraction yomthamo wesampulu, kwaye wenze i-XRD-CT ukufumana umzobo we-2D wezigaba ze-mineral plane ezinqamlekileyo kwisampuli.Qaphela ukuba yonke imilinganiselo ingenziwa ngaphandle kokusebenzisa inkqubo eyakhelwe-ngaphakathi ukususa umnini wesampuli ukusuka kwisiseko, ukuvumela imilinganiselo echanekileyo ye-CT kunye ne-XRD-CT.Isixhobo se-X-ray yemowudi ye-WL (BM AA40P; i-Hahamatsu Photonics) ixhotyiswe ngekhamera eyongezelelweyo ye-4608 × 4608 pixel metal-oxide-semiconductor (CMOS) (C14120-20P; I-Hamamatsu Photonics) ene-scintillator equka i-10 ye-10 lutetim ¥ ye-aluminium kunye nobukhulu be-Alluminum1 ye-aluminium eyodwa lala ilensi.Ubungakanani bepixel kwimowudi ye-WL malunga ne-0.848 µm.Ngaloo ndlela, indawo yokujonga (i-FOV) kwimodi ye-WL imalunga ne-6 mm kwimodi ye-CT ye-offset.I-NH mode X-ray detector (BM AA50; Hamamatsu Photonics) yayixhotyiswe nge-20 µm engqingqwa ye-gadolinium-aluminium-gallium garnet (Gd3Al2Ga3O12) i-scintillator, ikhamera ye-CMOS (C11440-22CU) kunye nesisombululo se-2048 × 2048;Hamamatsu Photonics) kunye ne × 20 lens.Ubungakanani bepixel kwimowudi ye-NH yi ~0.25 µm kwaye indawo yokujonga yi ~0.5 mm.I-detector ye-XRD mode (i-BM AA60; i-Hahamatsu Photonics) yayixhotyiswe nge-scintillator ebandakanya i-50 µm engqingqwa ye-P43 (Gd2O2S: Tb) isikrini se powder, i-2304 × 2304 pixel resolution yekhamera ye-CMOS (C15440-20UP ye-Photonics) kunye ne-Hamama ye-Photonics le-lens.Isixhobo sinobungakanani bepixel obusebenzayo obuyi-19.05 µm kunye nendawo yokujonga eyi-43.9 mm2.Ukwandisa i-FOV, sisebenzise inkqubo ye-CT ye-offset kwimodi ye-WL.Umfanekiso wokukhanya ogqithisiweyo wokwakhiwa kwakhona kwe-CT uquka umfanekiso okwi-180 ° ukuya kwi-360 ° ebonakaliswe ngokuthe tye kwi-axis yokujikeleza, kunye nomfanekiso kuluhlu lwe-0 ° ukuya kwi-180 °.
Kwimo ye-XRD, i-X-ray beam igxininiswe yi-Fresnel zone plate.Kule modi, i-detector ifakwe i-110 mm emva kwesampuli kwaye isitofu se-beam si-3 mm phambi kwe-detector.Imifanekiso ye-Diffraction kwi-2θ ukusuka kwi-1.43 ° ukuya kwi-18.00 ° (i-grating pitch d = 16.6-1.32 Å) ifunyenwe kunye nebala le-X-ray eligxininise emazantsi kwindawo yokujonga i-detector.Isampulu ihamba ngokuthe nkqo ngamaxesha aqhelekileyo, ngokujika kwesiqingatha kwinqanaba ngalinye lokuskena ngokuthe nkqo.Ukuba i-mineral particles iyanelisa imeko ye-Bragg xa ijikelezwe ngu-180 °, kunokwenzeka ukufumana i-diffraction ye-mineral particles kwi-plane ethe tye.Imifanekiso ye-diffraction iye yadityaniswa ibe ngumfanekiso omnye kwinyathelo ngalinye lokuskena ngokuthe nkqo.Iimeko zovavanyo lwe-SR-XRD-CT ziphantse zifane nezo ze-SR-XRD assay.Kwimo ye-XRD-CT, i-detector ibekwe kwi-69 mm emva kwesampuli.Imifanekiso ye-Diffraction kwi-2θ ububanzi ukusuka kwi-1.2 ° ukuya kwi-17.68 ° (d = 19.73 ukuya kwi-1.35 Å), apho zombini i-X-ray beam kunye ne-beam limiter zihambelana nombindi wendawo yokujonga i-detector.Skena isampuli ngokuthe tye kwaye ujikelezise isampuli 180 °.Imifanekiso ye-SR-XRD-CT yakhiwa ngokutsha ngencopho yeminerali yokuqina njengamaxabiso epikseli.Ngokuskena okuthe tyaba, isampuli iqhele ukuskenwa ngamanyathelo angama-500–1000.
Kuzo zonke iimvavanyo, amandla e-X-reyi ayenziwe kwi-30 keV, kuba lo ngumda ongaphantsi wokungena kwe-X-reyi kwiimeteorites ezinobubanzi obumalunga ne-6 mm.Inani lemifanekiso efunyenwe kuyo yonke imilinganiselo ye-CT ngexesha lokujikeleza kwe-180 ° yi-1800 (3600 yeprogram ye-CT ye-offset), kwaye ixesha lokuvezwa kwemifanekiso yayiyi-100 ms kwimodi ye-WL, i-300 ms kwimodi ye-NH, i-500 ms ye-XRD, kunye ne-50 ms.ms ye-XRD-CT ms.Ixesha lokuskena isampula eliqhelekileyo limalunga nemizuzu eyi-10 kwimodi ye-WL, imizuzu eyi-15 kwimodi ye-NH, iiyure ze-3 ze-XRD, kunye neeyure ze-8 ze-SR-XRD-CT.
Imifanekiso ye-CT yakhiwa ngokutsha nge-convolutional back projection kunye nesiqhelo kwi-linear attenuation coefficient ukusuka kwi-0 ukuya kwi-80 cm-1.Isoftware yeSlice yasetyenziselwa ukuhlalutya idatha ye-3D kwaye isoftware ye-muXRD yasetyenziselwa ukuhlalutya idatha ye-XRD.
Amasuntswana e-Ryugu e-Epoxy-fixed (A0029, A0037, C0009, C0014 kunye ne-C0068) aye akhazimliswa ngokuthe ngcembe kumphezulu ukuya kwinqanaba le-0.5 µm (3M) yefilimu yokugquma idayimane phantsi kweemeko ezomileyo, zithintela imathiriyeli ukuba idibane nomphezulu ngexesha lenkqubo yokupolishwa.Umphezulu opolishiweyo wesampulu nganye waqala wavavanywa ngemicroscope ekhanyayo kwaye emva koko ii-electron zasasazwa ngasemva ukufumana i-mineralogy kunye nemifanekiso ye-texture (BSE) yeesampulu kunye nezinto ezisemgangathweni ze-NIPR zisebenzisa i-JEOL JSM-7100F SEM exhotyiswe nge-spectrometer yamandla e-dispersive (AZtec).amandla) umfanekiso.Kwisampula nganye, umxholo wezinto eziphambili kunye ezincinci zahlalutywa kusetyenziswa i-electron probe microanalyzer (EPMA, JEOL JXA-8200).Hlalutya i-phyllosilicate kunye ne-carbonate particles kwi-5 nA, imigangatho yendalo kunye ne-synthetic kwi-15 keV, i-sulfides, i-magnetite, i-olivine, kunye ne-pyroxene kwi-30 nA.Amabakala e-Modal abalwa ukusuka kwiimephu zezinto kunye nemifanekiso ye-BSE kusetyenziswa i-software ye-ImageJ 1.53 enemigangatho efanelekileyo ebekwe ngokungenamthetho kwiminerali nganye.
Uhlalutyo lwe-oxygen isotope lwenziwa kwiYunivesithi evulekileyo (eMilton Keynes, e-UK) ngokusebenzisa inkqubo ye-laser fluorination ye-infrared.Iisampulu zeHayabusa2 zaziswa kwiDyunivesithi eVulekileyo 38 kwizikhongozeli ezizaliswe yinitrogen ukuze zidluliselwe phakathi kwezibonelelo.
Ukulayisha isampulu kwenziwa kwibhokisi yegilavu ​​yenitrogen enezinga leoksijini eligadiweyo elingaphantsi kwe-0.1%.Kuba Hayabusa2 umsebenzi analytical, umbambi Ni isampulu entsha yenziwe, equka imingxunya isampuli ezimbini kuphela (ububanzi 2.5 mm, ubunzulu 5 mm), enye Hayabusa2 amasuntswana kunye nezinye umgangatho obsidian yangaphakathi.Ngexesha lohlalutyo, isampuli kakuhle equlathe izinto Hayabusa2 yagqunywa ngefestile BaF2 yangaphakathi malunga 1 mm ubukhulu kunye 3 mm ububanzi ukubamba isampuli ngexesha reaction laser.Ukuhamba kwe-BrF5 kwisampulu kwagcinwa ngumjelo wokuxuba igesi osikiwe kumnini wesampuli ye-Ni.Igumbi lesampulu liphinde lahlengahlengiswa ukuze lisuswe kumgca we-vacuum fluorination kwaye emva koko livulwe kwibhokisi yeglavu ezaliswe yinitrogen.Igumbi elineziqwenga ezibini litywinwe ngesitywina soxinizelelo se-gasket yobhedu kunye ne-EVAC yokuKhupha ngokukhawuleza i-CeFIX 38 chain clamp.Ifestile ye-BaF2 eyi-3 mm engaphezulu kwegumbi ivumela ukujonga ngaxeshanye isampuli kunye nokufudumeza kwelaser.Emva kokulayisha isampuli, phinda ubambe igumbi kwaye uphinde udibanise kumgca we-fluorinated.Ngaphambi kokuhlalutya, igumbi lesampulu lifudunyezwe phantsi kwe-vacuum malunga ne-95 ° C ngobusuku bonke ukususa nayiphi na i-adsorbed.Emva kokufudumeza ubusuku bonke, igumbi livunyelwe ukupholisa kwiqondo lokushisa kwaye emva koko inxalenye evezwe emoyeni ngexesha lokudluliselwa kwesampuli yahlanjululwa nge-aliquots ezintathu ze-BrF5 ukususa umswakama.Ezi nkqubo ziqinisekisa ukuba isampulu ye-Hayabusa 2 ayivezwanga emoyeni kwaye ayingcoliswanga kukufuma ukusuka kwinxalenye yomgca we-fluorinated ephuma emoyeni ngexesha lokulayisha isampulu.
I-Ryugu C0014-4 kunye ne-Orgueil (CI) iisampulu ze-particle zahlalutywa kwimodi "eyodwa" elungisiweyo42, ngelixa uhlalutyo lwe-Y-82162 (CY) lwenziwa kwi-tray enye kunye neesampuli ezininzi ze-41.Ngenxa yokubunjwa kwabo kwe-anhydrous, akuyimfuneko ukusebenzisa indlela enye ye-CY chondrites.Iisampuli zafudunyezwa kusetyenziswa i-Photon Machines Inc. infrared CO2 laser.amandla angama-50 W (10.6 µm) axhonywe kwi-XYZ gantry phambi kwe-BrF5.Inkqubo yevidiyo eyakhelwe-ngaphakathi ibeka iliso kwindlela yokusabela.Emva kwe-fluorination, i-O2 ekhululiwe yaxutywa ngokusebenzisa imigibe emibini ye-cryogenic nitrogen kunye nebhedi eshushu ye-KBR ukususa nayiphi na i-fluorine engaphezulu.Ukubunjwa kwe-isotopic ye-oksijini ecocekileyo yahlalutywa kwi-Thermo Fisher MAT 253 ye-spektrometer ye-channel ye-dual-channel ene-mass resolution malunga ne-200.
Kwezinye iimeko, ubungakanani begesi ye-O2 ekhutshiweyo ngexesha lokusabela kwesampulu ibingaphantsi kwe-140 µg, engumda oqikelelweyo wokusebenzisa isixhobo se-bellows kwi-MAT 253 mass spectrometer.Kule meko, sebenzisa i-microvolumes ukuhlalutya.Emva kokuhlalutya amasuntswana e-Hayabusa2, umgangatho wangaphakathi we-obsidian ufakwe i-fluorinated kunye nokwakheka kwe-isotope ye-oxygen.
I-Ions ye-NF + NF3 + iqhekeza iphazamisa umqadi kunye nobunzima be-33 (16O17O).Ukuphelisa le ngxaki enokubakho, iisampulu ezininzi zicutshungulwa kusetyenziswa iinkqubo zokwahlula i-cryogenic.Oku kunokwenziwa kwindlela eya phambili phambi kohlalutyo lwe-MAT 253 okanye njengohlalutyo lwesibini ngokubuyisela igesi ehlalulweyo kwi-sieve ekhethekileyo ye-molecular kwaye iphinde idlulise emva kokuhlukana kwe-cryogenic.Ukwahlulwa kweCryogenic kubandakanya ukubonelela ngerhasi kwisihluzo semolekyuli kubushushu benitrogen engamanzi kwaye emva koko siyikhuphe kwisisefu sokuqala semolekyuli kubushushu obuyi-130°C.Uvavanyo olubanzi lubonise ukuba i-NF + ihleli kwi-sieve yokuqala ye-molecular kwaye akukho nxalenye ebalulekileyo eyenzekayo ngokusebenzisa le ndlela.
Ngokusekelwe kuhlalutyo oluphindaphindiweyo lwemigangatho yethu yangaphakathi ye-obsidian, ukuchaneka ngokubanzi kwenkqubo kwimodi ye-bellows yile: ± 0.053 ‰ ye-δ17O, ± 0.095 ‰ ye-δ18O, ± 0.018‰ ye-Δ17O (2 sd).Uhlalutyo lwe-isotope yeoksijini lunikezelwa kwi-delta notation eqhelekileyo, apho i-delta18O ibalwa ngolu hlobo:
Kwakhona sebenzisa umlinganiselo we-17O/16O we-δ17O.I-VSMOW ngumgangatho wehlabathi weVienna Mean Sea Water Standard.I-Δ17O imele ukutenxa kumgca wokuqhekeka komhlaba, kwaye ifomula yokubala ithi: Δ17O = δ17O - 0.52 × δ18O.Zonke iinkcukacha ezithiwe thaca kwiTheyibhile eyoNgezelelweyo yesi-3 zilungisiwe.
Amacandelo amalunga ne-150 ukuya kwi-200 nm ubukhulu akhutshwe kwiincinci ze-Ryugu usebenzisa isixhobo se-Hitachi High Tech SMI4050 FIB kwi-JAMSTEC, i-Kochi Core Sampling Institute.Qaphela ukuba onke amacandelo e-FIB afunyenwe kwiinqununu ezingalungiswanga zamacandelo angalungiswanga emva kokususwa kwiinqanawa ezizaliswe yigesi ye-N2 yokudluliselwa kwe-interbject.Ezi ziqwenga azizange zilinganiswe nge-SR-CT, kodwa zacutshungulwa ngokutyhileka okuncinci kumoya ojikeleze umhlaba ukuthintela umonakalo onokwenzeka kunye nongcoliseko olunokuchaphazela i-carbon K-edge spectrum.Emva kokubekwa kwe-tungsten yokhuselo lomaleko, ummandla womdla (ukuya kuthi ga kwi-25 × 25 μm2) unqunyulwe kwaye uncitshiswe nge-Ga + ion beam kwi-voltage ekhawulezayo ye-30 kV, emva koko kwi-5 kV kunye ne-probe current ye-40 pA ukunciphisa umonakalo ongaphezulu.Amacandelo e-ultrathin emva koko abekwe kwi-mesh yethusi eyandisiweyo (i-Kochi mesh) 39 esebenzisa i-micromanipulator exhotywe nge-FIB.
I-Ryugu A0098 (1.6303mg) kunye neepellets ze-C0068 (0.6483mg) zavalwa kabini kumaphepha e-polyethylene asulungekileyo aphezulu kwibhokisi yeglavu ecocekileyo enenitrogen kwi-SPring-8 ngaphandle kokudibana nomoya womhlaba.Ukulungiswa kwesampulu ye-JB-1 (ilitye elibhekiselele kwijoloji ekhutshwe yiGeological Survey yaseJapan) yenziwa kwiYunivesithi yaseTokyo Metropolitan.
I-INAA ibanjelwe kwiziko le-Integrated Radiation kunye neNzululwazi yeNyukliya, kwiYunivesithi yaseKyoto.Iisampulu zahlanjululwa kabini ngemijikelo yokukhanya eyahlukileyo ekhethiweyo ngokwesiqingatha sobomi be-nuclide esetyenziselwa ubungakanani bento.Okokuqala, isampuli yayifakwe kwi-tube ye-pneumatic irradiation imizuzwana ye-30.I-Fluxes ye-neutron eshushu kunye ne-fast in fig.I-3 yi-4.6 × 1012 kunye ne-9.6 × 1011 cm-2 s-1, ngokulandelanayo, ukumisela imixholo yeMg, Al, Ca, Ti, V kunye noMn.Iikhemikhali ezifana ne-MgO (i-99.99% ubumsulwa, i-Soekawa Chemical), i-Al (i-99.9% yococeko, i-Soekawa Chemical), kunye ne-Si metal (i-99.999% yococeko, i-FUJIFILM Wako I-Chemical ecocekileyo) nayo yafakwa i-radiated ukuze ilungele ukuphazamisa ukuphendula kwenyukliya njenge (n, n).Isampuli nayo i-irradiated kunye ne-sodium chloride (i-99.99% ubumsulwa; i-MANAC) ukulungisa utshintsho kwi-neutron flux.
Emva kwe-neutron irradiation, i-polyethylene sheet yangaphandle yatshintshwa entsha, kunye nemitha ye-gamma ekhutshwe yisampuli kunye nereferensi yalinganiswa ngokukhawuleza nge-Ge detector.Iisampuli ezifanayo zahlaziywa kwakhona kwiiyure ze-4 kwi-tube ye-pneumatic irradiation.I-2 ine-neutron fluxes ye-thermal kunye ne-fast neutron ye-5.6 1012 kunye ne-1.2 1012 cm-2 s-1, ngokulandelanayo, ngokumisela i-Na, K, Ca, Sc, Cr, Fe, Co, Ni, Zn, Ga, As, Content Se, Sb, Os, Ir kunye ne-Au.Iisampulu zokulawula i-Ga, As, Se, Sb, Os, Ir, kunye ne-Au zaye zahlanjululwa ngokusetyenziswa kweemali ezifanelekileyo (ukusuka kwi-10 ukuya kwi-50 μg) yezisombululo ezisemgangathweni zogxininiso olwaziwayo lwezi zinto kumacandelo amabini ephepha lokucoca, elandelwa yi-irradiation yeesampuli.Ubalo lwemitha ye-gamma lwenziwa kwiziko le-Integrated Radiation kunye neNzululwazi yeNyukliya, iYunivesithi yaseKyoto kunye neZiko loPhando le-RI, iYunivesithi yaseTokyo Metropolitan.Iinkqubo zokuhlalutya kunye nezixhobo zokubhekisela ekumiselweni kobungakanani bezinto ze-INAA ziyafana nezo zichazwe kumsebenzi wethu wangaphambili.
I-X-ray diffractometer (i-Rigaku SmartLab) yayisetyenziselwa ukuqokelela iipatheni ze-diffraction yeesampuli ze-Ryugu A0029 (<1 mg), i-A0037 (≪1 mg) kunye ne-C0087 (<1 mg) kwi-NIPR. I-X-ray diffractometer (i-Rigaku SmartLab) yayisetyenziselwa ukuqokelela iipatheni ze-diffraction yeesampuli ze-Ryugu A0029 (<1 mg), i-A0037 (≪1 mg) kunye ne-C0087 (<1 mg) kwi-NIPR. Рентгеновский дифрактометр (Rigaku SmartLab) использовали для сбора дифракционных картин образцов Ryugu A0029 (<1 мг), A0037 (≪1 мг) и 1 NIPR. I-X-ray diffractometer (i-Rigaku SmartLab) yayisetyenziselwa ukuqokelela iipatheni ze-diffraction ye-Ryugu A0029 (<1 mg), i-A0037 (≪1 mg), kunye ne-C0087 (<1 mg) iisampuli kwi-NIPR.使用X 射线衍射仪(Rigaku SmartLab) 在NIPR 收集Ryugu 样品A0029 (<1 mg)、A0037 (<1 mg) 和C0087 (<1 mg) 的衍射图案。使用X 射线衍射仪(Rigaku SmartLab) 在NIPR 收集Ryugu 样品A0029 (<1 mg)、A0037 (<1 mg) 和C0087 (<1 mg) 的衍射图案。 Дифрактограммы образцов Ryugu A0029 (<1 мг), A0037 (<1 мг) kunye C0087 (<1 мг) были получены в NIPR с использованием рентгеновгенгей рентгеного в NIPR с использованием рентгеновгенов ренгенгей Iipatheni ze-X-ray diffraction yeesampuli i-Ryugu A0029 (<1 mg), i-A0037 (<1 mg) kunye ne-C0087 (<1 mg) zifunyenwe kwi-NIPR kusetyenziswa i-X-ray diffractometer (Rigaku SmartLab).Zonke iisampulu zaculwa zaba ngumgubo ocolekileyo kwi-silicon ye-wafer engabonisi kukhanya kusetyenziswa ipleyiti yeglasi yesafire emva koko yasasazwa ngokulungeleleneyo kwi-silicon ye-wafer engabonisiyo ngaphandle kolwelo (amanzi okanye utywala).Iimeko zokulinganisa zimi ngolu hlobo lulandelayo: I-Cu Kα X-ray ye-ray yenziwe kwi-tube voltage ye-40 kV kunye ne-tube current ye-40 mA, ubude be-slit slit yi-10 mm, i-divergence angle (1/6) °, i-in-plane yokujikeleza isantya yi-20 rpm, kwaye uluhlu luthatha i-2θ (i-0) i-angle ye-2θ (i-0 kabini ukuya kwi-3 i-angle ye-2) ° i-2 kunye ne-3 i-angle ye-2.Kwasetyenziswa iBragg Brentano optics.I-detector yi-one-dimensional silicon semiconductor detector (D / teX Ultra 250).I-X-reyi ye-Cu Kβ yasuswa kusetyenziswa isihluzo se-Ni.Ukusebenzisa iisampuli ezikhoyo, imilinganiselo ye-synthetic magnesian saponite (JCSS-3501, i-Kunimine Industries CO. Ltd), inyoka (i-leaf serpentine, i-Miyazu, i-Nikka) kunye ne-pyrrhotite (i-monoclinic 4C, i-Chihua, i-Mexico Watts) yafaniswa nokuchonga iincopho kunye nokusetyenziswa kwedatha yedatha ye-PDF Didoloff data yedatha yedatha yedatha ye-PDF. 071-1662) kunye nemagnetite (PDF 00-019-0629).Idatha ye-Diffraction evela kwi-Ryugu nayo yafaniswa nedatha kwi-hydroaltered carbonaceous chondrites, i-Orgueil CI, i-Y-791198 CM2.4, kunye ne-Y 980115 CY (isigaba sokufudumala se-III, i-500-750 ° C).Ukuthelekisa kubonise ukufana ne-Orgueil, kodwa kungekhona nge-Y-791198 kunye ne-Y 980115.
I-spectra ye-NEXAFS ene-carbon edge K ye-ultrathin yamacandelo eesampuli ezenziwe kwi-FIB zilinganiswe ngokusebenzisa i-STXM BL4U ishaneli kwiziko le-UVSOR synchrotron kwi-Institute of Molecular Sciences (Okazaki, Japan).Ubungakanani bebala lomqadi ogxile kwipleyiti yezone yeFresnel bumalunga ne-50 nm.Isinyathelo samandla ngu-0.1 eV kwisakhiwo esihle sommandla okufutshane (283.6-292.0 eV) kunye ne-0.5 eV (280.0-283.5 eV kunye ne-292.5-300.0 eV) kwiingingqi zangaphambili nangasemva.ixesha lomfanekiso ngamnye pixel wamiselwa 2 ms.Emva kokukhutshwa, igumbi lokuhlalutya le-STXM lizaliswe nge-helium ngoxinzelelo malunga ne-20 mbar.Oku kunceda ukunciphisa i-thermal drift yezixhobo ze-X-ray optics kwigumbi kunye nomnini wesampuli, kunye nokunciphisa umonakalo wesampuli kunye / okanye i-oxidation.I-NEXAFS Imbonakalo yekhabhoni ye-K-edge yenziwe kwidatha egciniweyo kusetyenziswa isoftware ye-aXis2000 kunye nesoftware ye-STXM yokuthengisa idatha.Qaphela ukuba isampuli yokudlulisa isampuli kunye nebhokisi yeglavu zisetyenziselwa ukuphepha i-oxidation yesampuli kunye nokungcoliswa.
Ukulandela uhlalutyo lwe-STXM-NEXAFS, ukubunjwa kwe-isotopic ye-hydrogen, i-carbon, kunye ne-nitrogen ye-Ryugu FIB slices yahlalutywa ngokusebenzisa i-isotope imaging kunye ne-JAMSTEC NanoSIMS 50L.I-Cs + i-primary beam egxininisiweyo malunga ne-2 pA ye-carbon kunye ne-nitrogen isotope yohlalutyo kunye ne-13 pA yohlalutyo lwe-isotope ye-hydrogen i-rasterized phezu kwendawo emalunga ne-24 × 24 µm2 ukuya ku-30 ​​× 30 µm2 kwisampuli.Emva kwemizuzu emi-3 yokutshiza kwi-primary beam yangoku, uhlalutyo ngalunye lwaqalwa emva kokuzinziswa koxinzelelo lwesibini.Uhlalutyo lwe-carbon kunye ne-nitrogen isotopes, imifanekiso ye-12C-, 13C-, 16O-, 12C14N- kunye ne-12C15N- yafunyanwa ngaxeshanye kusetyenziswa ukufumanisa i-electron ye-multiplier multiplex esixhenxe kunye nesisombululo sobunzima malunga ne-9000, eyaneleyo ukwahlula zonke iikhompawundi ze-isotopic ezifanelekileyo.ukuphazamiseka (okt 12C1H kwi-13C kunye ne-13C14N kwi-12C15N).Uhlalutyo lwe-isotopi ye-hydrogen, i-1H-, i-2D- kunye ne-12C-imifanekiso ifunyenwe ngesisombululo sobunzima malunga ne-3000 kunye nokufunyanwa kwezinto ezininzi kusetyenziswa i-electron multipliers ezintathu.Uhlalutyo ngalunye lunemifanekiso engama-30 eskeniweyo yendawo enye, kunye nomfanekiso omnye oquka i-256 × 256 pixels yohlalutyo lwe-carbon kunye ne-nitrogen isotope kunye ne-128 × 128 pixels yohlalutyo lwe-hydrogen isotope.Ixesha lokulibaziseka yi-3000 µs nge-pixel nganye yohlalutyo lwe-carbon kunye ne-nitrogen isotopu kunye ne-5000 µs nge-pixel nganye yohlalutyo lwe-hydrogen isotope.Sisebenzise i-1-hydroxybenzotriazole hydrate njengemigangatho ye-hydrogen, i-carbon kunye ne-nitrogen isotope ukulinganisa i-instrumental mass fractionation45.
Ukumisela ukubunjwa kwe-silicon isotopic yegraphite ye-presolar kwiprofayili ye-FIB C0068-25, sisebenzise iziphindaphindi ze-electron ezintandathu kunye nesisombululo sobunzima malunga ne-9000. Imifanekiso iqulethe i-256 × 256 pixels kunye nexesha lokulibaziseka le-3000 µs nge-pixel nganye.Silinganise isixhobo sokwahlulahlula ngobuninzi sisebenzisa ii-silicon wafers njenge-hydrogen, i-carbon, kunye nemigangatho ye-silicon isotope.
Imifanekiso ye-Isotope yacutshungulwa kusetyenziswa i-NASA's NanoSIMS45 imaging software.Idatha yalungiswa ngexesha lokufa lokuphindaphinda i-electron (44 ns) kunye nemiphumo yokufika ngexesha elinye.Ulungelelwaniso lokuskena olwahlukileyo kumfanekiso ngamnye ukulungisa ukukhukuliseka komfanekiso ngexesha lokufunyanwa.Umfanekiso wokugqibela we-isotopu wenziwa ngokongeza iiyoni zesibini kumfanekiso ngamnye kwipikseli nganye yokuskena.
Emva kohlalutyo lwe-STXM-NEXAFS kunye ne-NanoSIMS, amacandelo afanayo e-FIB ahlolwe kusetyenziswa i-microscope yothumelo lwe-electron (JEOL JEM-ARM200F) kwi-voltage esheshayo ye-200 kV e-Kochi, e-JAMSTEC.I-microstructure yabonwa ngokusebenzisa i-TEM ekhanyayo kunye ne-high-angle scanning TEM kwintsimi emnyama.Izigaba zezimbiwa zachongwa nge-spot electron diffraction kunye ne-lattice band imaging, kwaye uhlalutyo lwekhemikhali lwenziwa yi-EDS nge-100 mm2 ye-silicon drift detector kunye ne-JEOL Analysis Station 4.30 software.Kucazululo lobungakanani, uphawu lweX-reyi yobunzulu bento nganye bulinganiswe kwimowudi yokuskena ye-TEM kunye nexesha elimiselweyo lokufunyanwa kwedatha ye-30 s, indawo yokuskena ye-beam ye ~ 100 × 100 nm2, kunye nomsinga we-50 pA.Umlinganiselo (i-Si + Al) -Mg-Fe kwii-silicates ezicwangcisiweyo zagqitywa ngokusebenzisa i-coefficient yokulinga k, elungiswe ukutyeba, efunyenwe kumgangatho we-pyropagarnet yendalo.
Yonke imifanekiso kunye nohlalutyo olusetyenziswe kolu phononongo luyafumaneka kwi-JAXA Data Archive and Communication System (DARTS) https://www.darts.isas.jaxa.jp/curation/hayabusa2.Eli nqaku libonelela ngedatha yokuqala.
Kitari, K. et al.Ukwakhiwa komphezulu we-asteroid 162173 Ryugu njengoko kubonwa sisixhobo seHayabusa2 NIRS3.Inzululwazi 364, 272-275.
Kim, AJ Yamato-uhlobo lwe-carbonaceous chondrites (CY): ii-analogues ze-Ryugu asteroid surface?I-Geochemistry 79, 125531 (2019).
Pilorjet, S. et al.Uhlalutyo lokuqala lokuqulunqa iisampuli zeRyugu lwenziwa kusetyenziswa i-MicroOmega hyperspectral microscope.I-Astron yeSizwe.6, 221–225 (2021).
Yada, T. et al.Uhlalutyo lokuqala lwesampulu ye-Hyabusa2 ibuyile kwi-C-uhlobo lwe-asteroid Ryugu.I-Astron yeSizwe.6, 214–220 (2021).