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Aguquguqukayo futhi anothile ngezinto eziphilayo, ama-asteroids ohlobo lwe-C angase abe omunye wemithombo eyinhloko yamanzi eMhlabeni.Njengamanje, ama-chondrite ane-carbon-bearing anikeza umqondo omuhle kakhulu wokwakheka kwamakhemikhali awo, kodwa ulwazi mayelana nama-meteorite luhlanekezelwe: yizinhlobo ezihlala isikhathi eside kuphela ezisindayo lapho zingena emkhathini bese zixhumana nemvelo yomhlaba.Lapha sethula imiphumela yocwaningo oluningiliziwe lwevolumu kanye ne-microanalytical yezinhlayiyana eziyinhloko ze-Ryugu ezilethwe eMhlabeni umkhumbi-mkhathi i-Hayabusa-2.Izinhlayiya ze-Ryugu zibonisa ukufana okuseduze ekubunjweni kwama-chondrite e-CI (uhlobo lwe-Iwuna-uhlobo lwe-Iwuna) angashintshiwe ngamakhemikhali, asetshenziswa kabanzi njengenkomba yokwakheka okuphelele kwesimiso sonozungezilanga.Lesi sifanekiso sibonisa ubudlelwano bendawo obuyinkimbinkimbi phakathi kwezinto eziphilayo ezinothile nama-silicates agqinsile futhi sibonisa izinga lokushisa eliphakeme elicishe libe ngu-30 °C ngesikhathi sokuguguleka kwamanzi.Sithole inqwaba ye-deuterium ne-diazonium ehambisana nomsuka we-extrasolar.Izinhlayiya ze-Ryugu ziyizinto zangaphandle ezingangcolisiwe nezingahlukaniseki kunazo zonke ezake zafundwa futhi zilingana kangcono nokwakheka kwesimiso sonozungezilanga.
Kusukela ngoJuni 2018 kuya kuNovemba 2019, umkhumbi-mkhathi waseJapan Aerospace Exploration Agency’s (JAXA) Hayabusa2 wenze ucwaningo olunzulu olukude nge-asteroid Ryugu.Idatha evela ku-Near Infrared Spectrometer (NIRS3) ku-Hayabusa-2 iphakamisa ukuthi i-Ryugu ingase yakhelwe ngento efana ne-thermal kanye/noma i-shock-metamorphic carbonaceous chondrites.Okufana kakhulu ne-CY chondrite (uhlobo lwe-Yamato) 2. I-albedo ephansi ye-Ryugu ingachazwa ngokuba khona kwenani elikhulu lezingxenye ezicebile nge-carbon, kanye nosayizi wezinhlayiyana, i-porosity, nemiphumela yesimo sezulu yendawo.Umkhumbi-mkhathi we-Hayabusa-2 wenze ukuhlala okubili nokuqoqwa kwesampula e-Ryuga.Ngesikhathi sokufika kokuqala ngoFebhuwari 21, 2019, kwatholwa impahla engaphezulu, eyagcinwa engxenyeni A yekhephuseli yokubuya, futhi ngesikhathi sokuhlala kwesibili ngoJulayi 11, 2019, impahla yaqoqwa eduze kwe-crater yokwenziwa eyakhiwe i-impaor encane ephathekayo.Lawa masampuli agcinwe ku-Ward C. Ukubonakaliswa kokuqala okungabhubhisi kwezinhlayiya eSiteshini 1 emakamelweni akhethekile, angangcolile futhi ahlanzekile agcwele i-nitrogen ezindaweni eziphethwe yi-JAXA abonise ukuthi izinhlayiya ze-Ryugu zazifana kakhulu ne-CI4 chondrites futhi zibonise "amazinga ahlukahlukene okuhlukahluka"3.Ukuhlukaniswa okubonakala kuphikisana kwe-Ryugu, efana ne-CY noma i-CI chondrite, ingaxazululwa kuphela nge-isotopic enemininingwane, i-elemental, ne-mineralogical characterization yezinhlayiya ze-Ryugu.Imiphumela evezwe lapha inikeza isisekelo esiqinile sokunquma ukuthi iyiphi kulezi zincazelo ezimbili zokuqala zokwakheka okuphelele kwe-asteroid Ryugu okungenzeka kakhulu.
Amapellets e-Ryugu ayisishiyagalombili (cishe isamba esingu-60mg), amane avela ku-Chamber A namane avela ku-Chamber C, abelwa esigabeni sesi-2 sokuphatha ithimba le-Kochi.Umgomo oyinhloko wocwaningo ukucacisa ubunjalo, umsuka kanye nomlando wokuziphendukela kwemvelo kwe-asteroid Ryugu, kanye nokubhala ukufana nokwehluka nezinye izibonelo ezaziwayo zangaphandle njengama-chondrites, izinhlayiya zothuli lwe-interplanetary (IDPs) kanye nezinkanyezi ezinomsila ezibuyayo.Amasampula aqoqwe yi-NASA's Stardust mission.
Ukuhlaziywa okuningiliziwe kwe-mineralogical yezinhlamvu ezinhlanu ze-Ryugu (A0029, A0037, C0009, C0014 kanye ne-C0068) zibonise ukuthi zakhiwe ikakhulukazi ama-phyllosilicates amahle kanye nama-coarse-grained (~ 64-88 vol.%; Fig. 1a, b, Fig. Fig. 1).kanye nethebula elengeziwe 1).Ama-phyllosilicates anezinhlamvu ezimahhadla zenzeka njengama-pinnate aggregate (afinyelela emashumini ama-microns ngosayizi) kumatrices acolile, anothe nge-phyllosilicate (angaphansi kwama-microns ambalwa ngosayizi).Izinhlayiya ze-silicate ezinezingqimba ziyi-serpentine-saponite symbionts (Fig. 1c).Imephu ye-(Si + Al)-Mg-Fe iphinda ibonise ukuthi i-matrix ye-silicate enezingqimba yobuningi inokwakheka okuphakathi phakathi kwenyoka ne-saponite (Fig. 2a, b).I-matrix ye-phyllosilicate iqukethe amaminerali e-carbonate (~ 2-21 vol.%), amaminerali e-sulfide (~ 2.4-5.5 vol.%), kanye ne-magnetite (~ 3.6-6.8 vol.%).Enye yezinhlayiya ezihloliwe kulolu cwaningo (i-C0009) iqukethe inani elincane (~0.5 vol.%) lama-silicates anhydrous (i-olivine ne-pyroxene), engasiza ekuboneni umthombo owenziwe i-Ryugu stone5.Le silicate ye-anhydrous ayivamile kumapellets e-Ryugu futhi ikhonjwe kahle kuphela ku-pellet ye-C0009.Amakhabhoni akhona ku-matrix njengezicucu (ngaphansi kwamakhulu ambalwa ama-microns), ikakhulukazi i-dolomite, enamanani amancane e-calcium carbonate ne-brinell.I-Magnetite yenzeka njengezinhlayiya ezingazodwa, ama-framboid, ama-plaque, noma ama-spherical aggregates.Ama-sulfide amelwe ngokuyinhloko yi-pyrrhotite ngendlela yamaprism/amapuleti angama-hexagonal angajwayelekile noma ama-laths.I-matrix iqukethe inani elikhulu le-submicron pentlandite noma ihlanganiswe ne-pyrrhotite. Izigaba ezinothe ngekhabhoni (<10 µm ngosayizi) zenzeka yonke indawo ku-matrix ecebile nge-phyllosilicate. Izigaba ezinothe ngekhabhoni (<10 µm ngosayizi) zenzeka yonke indawo ku-matrix ecebile nge-phyllosilicate. Богатые углеродом фазы (размером <10 мкм) встречаются повсеместно в богатой филлосиликатами матрице. Izigaba ezinothe ngekhabhoni (<10 µm ngosayizi) zenzeka yonke indawo ku-matrix ecebile nge-phyllosilicate.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 ezicebile ngekhabhoni (<10 µm ngosayizi) zihamba phambili ku-matrix ecebile nge-phyllosilicate.Amanye amaminerali asizayo aboniswa kuThebula Lokwengeza 1. Uhlu lwamaminerali anqunywe kusukela kuphethini ye-X-ray diffraction yengxube ye-C0087 ne-A0029 kanye ne-A0037 ihambisana kakhulu nalokho okunqunywe ku-CI (Orgueil) chondrite, kodwa ihluke kakhulu ku-CY kanye ne-CM (i-Mippleregure nedatha ye-Mippleregure enwetshiwe (uhlobo lwe-Migherigued Figure) olunwetshiweIngqikithi yokuqukethwe kwe-elementi yezinhlamvu ze-Ryugu (A0098, C0068) futhi ihambisana ne-chondrite 6 CI (idatha enwetshiwe, i-Fig. 2 kanye neThebula Lokwengeza 2).Ngokuphambene, ama-chondrite e-CM ancishiswa ezintweni ezilinganisiwe neziguquguqukayo kakhulu, ikakhulukazi i-Mn ne-Zn, futhi iphakeme ku-elementi ephikisayo7.Ukugxiliswa kwamanye ama-elementi kuyahluka kakhulu, okungase kube ukubonakaliswa kokungafani okungokwemvelo kwesampula ngenxa yosayizi omncane wezinhlayiya ezingazodwana kanye nomphumela wokuchelela amasampula.Zonke izici ze-petrological, mineralological and elemental zibonisa ukuthi izinhlamvu ze-Ryugu zifana kakhulu nama-chondrites CI8,9,10.Okuhlukile okuphawulekayo ukungabikho kwe-ferrihydrite ne-sulfate kuzinhlamvu ze-Ryugu, okuphakamisa ukuthi lawa mamineral kuma-CI chondrites akhiwe isimo sezulu sasemhlabeni.
a, Isithombe se-X-ray esiyinhlanganisela se-Mg Kα (ebomvu), i-Ca Kα (eluhlaza), i-Fe Kα (eluhlaza okwesibhakabhaka), kanye no-S Kα (ophuzi) isigaba esipholishiwe esomile esingu-C0068.Ingxenyana iqukethe ama-silicate anezingqimba (obomvu: ~88 vol). – magnetite; juice – soapstone; Srp – serpentine. c, high-resolution transmission electron microscopy (TEM) isithombe sokukhula okujwayelekile kwe-saponite-serpentine esibonisa amabhendi e-serpentine ne-saponite lattice angu-0.7 nm no-1.1 nm, ngokulandelana.
Ukwakheka kwe-matrix ne-silicate enezingqimba (ku-%) yezinhlayiya ze-Ryugu A0037 (imibuthano ebomvu eqinile) kanye nezinhlayiya ze-C0068 (eziqinile eziluhlaza okwesibhakabhaka) kuboniswa ohlelweni lwe-ternary (Si+Al)-Mg-Fe.a, Imiphumela ye-Electron Probe Microanalysis (EPMA) eyakhiwe ngokumelene nama-CI chondrites (Ivuna, Orgueil, Alais)16 eboniswe ngokumpunga ukuze iqhathaniswe.b, I-Scanning TEM (STEM) kanye ne-energy dispersive X-ray spectroscopy (EDS) ukuhlaziya okuboniswe ukuze kuqhathaniswe ne-Orgueil9 ne-Murchison46 meteorites kanye ne-IDP47 enamanzi.Ama-phyllosilicates ahlanjululwe kahle futhi ahlaza okwesibhakabhaka ahlaziywa, agwema izinhlayiya ezincane ze-iron sulfide.Imigqa enamachashazi ku-a no-b ibonisa imigqa yokuqedwa ye-saponite nenyoka.Ukwakheka okucebile ngensimbi ku-a kungase kube ngenxa yezinhlamvu ze-submicron iron sulfide ngaphakathi kwezinhlamvu ze-silicate ezigqinsiwe, ezingakwazi ukukhishwa ngokulungiswa kwendawo yokuhlaziywa kwe-EPMA.Amaphoyinti edatha anokuqukethwe kwe-Si okuphezulu kune-saponite ku-b angase abangwe ukuba khona kwezinto ezicebile nge-silicon amorphous nanosized kuma-interstices ongqimba lwe-phyllosilicate.Inombolo yokuhlaziya: N=69 ye-A0037, N=68 ye-EPMA, N=68 ye-C0068, N=19 ye-A0037 kanye ne-N=27 ye-C0068 ye-STEM-EDS.c.Sithole idatha ye-Orgueil kanye ne-Y-82162 meteorites.I-CCAM iwumugqa wamaminerali e-anhydrous carbonaceous chondrite, i-TFL iwumugqa wokuhlukanisa umhlaba.d, Δ17O kanye ne-δ18O amamephu we-Ryugu particle C0014-4, CI chondrite (Orgueil), kanye ne-CY chondrite (Y-82162) (lolu cwaningo).Δ17O_Ryugu: Inani le-Δ17O C0014-1.Δ17O_Orgueil: Isilinganiso senani elingu-Δ17O le-Orgueil.Δ17O_Y-82162: Isilinganiso senani elingu-Δ17O le-Y-82162.Idatha ye-CI ne-CY evela ezincwadini ezingu-41, 48, 49 nazo ziboniswa ukuze ziqhathaniswe.
Ukuhlaziywa kwe-isotope enkulu yomoya-mpilo kwenziwa kusampula engu-1.83 mg yezinto ezikhishwe ku-granular C0014 nge-laser fluorination (Izindlela).Ukuze siqhathanise, sisebenzise amakhophi ayisikhombisa e-Orgueil (CI) (ingqikithi yesisindo = 8.96 mg) kanye namakhophi ayisikhombisa e-Y-82162 (CY) (ingqikithi yesisindo = 5.11 mg) (Ithebula Elingeziwe 3).
Emkhiwaneni.I-2d ibonisa ukuhlukaniswa okucacile kwe-Δ17O kanye no-δ18O phakathi kwezinhlayiya ezimaphakathi zesisindo ze-Orgueil ne-Ryugu uma kuqhathaniswa ne-Y-82162.I-Δ17O yezinhlayiyana ze-Ryugu C0014-4 iphakeme kunaleyo yezinhlayiyana ze-Orgeil, naphezu kokugqagqana ngo-2 sd.Izinhlayiya ze-Ryugu zinamanani aphezulu e-Δ17O uma kuqhathaniswa ne-Orgeil, engabonisa ukungcoliswa komhlaba kwamuva kusukela ekwindla kwayo ngo-1864. Isimo sezulu endaweni yasemhlabeni11 siphumela ekuhlanganisweni komoyampilo womkhathi, okusondeza ukuhlaziywa okuphelele kumugqa womugqa (TFL).Lesi siphetho sihambisana nedatha ye-mineralogical (okuxoxwe ngayo ngaphambili) yokuthi izinhlamvu ze-Ryugu azinawo ama-hydrates noma ama-sulfate, kuyilapho u-Orgeil enawo.
Ngokusekelwe kudatha ye-mineralogical engenhla, le miphumela isekela ukuhlobana phakathi kwezinhlamvu ze-Ryugu nama-CI chondrite, kodwa ikhipha ukuhlangana kwama-CY chondrite.Iqiniso lokuthi izinhlamvu ze-Ryugu azihlotshaniswa nama-CY chondrites, abonisa izimpawu ezicacile ze-dehydration mineralogy, kuyadida.Ukubhekwa kwe-Orbital ye-Ryugu kubonakala kukhombisa ukuthi iphelelwe amanzi emzimbeni ngakho-ke kungenzeka ukuthi yakhiwe ngezinto ze-CY.Izizathu zalo mehluko osobala azikacaci.Ukuhlaziywa kwe-isotope ye-oxygen kwezinye izinhlayiya ze-Ryugu kuvezwa ephepheni elingumngane 12. Nokho, imiphumela yale sethi yedatha enwetshiwe ibuye ihambisane nokuhlobana phakathi kwezinhlayiya ze-Ryugu nama-chondrite e-CI.
Sisebenzisa amasu okuhlaziya ama-microanalysis (I-Supplementary Fig. 3), sihlole ukusatshalaliswa kwendawo kwekhabhoni ephilayo endaweni yonke yengxenyana ye-ion beam egxilile (FIB) C0068.25 (Figs. 3a–f).Isakhiwo esihle i-X-ray yokumunca i-spectra ye-carbon (NEXAFS) emaphethelweni aseduze esigabeni C0068.25 ebonisa amaqembu amaningana asebenzayo - i-aromatic noma i-C=C (285.2 eV), C=O (286.5 eV), CH (287.5 eV) kanye no-C(=O)O (288.8 i-eg 3 isakhiwo eV. ), okusho izinga eliphansi lokuhlukahluka kokushisa.Isilinganiso esiphezulu se-CH (287.5 eV) se-organic organics ingxenye ye-C0068.25 sihluka ezintweni ezingancibiliki zama-chondrite e-carbonaceous afundwe ngaphambilini futhi sifana kakhulu ne-IDP14 kanye nezinhlayiya ze-cometary ezitholwe i-Stardust mission.Ukuphakama okuqinile kwe-CH ku-287.5 eV kanye nephunga elimnandi elibuthakathaka kakhulu noma i-C=C eliphakeme ku-285.2 eV libonisa ukuthi izinhlanganisela eziphilayo zicebile kuma-aliphatic compounds (Fig. 3a kanye ne-Supplementary Fig. 3a).Izindawo ezicebile kuma-aliphatic organic compounds zitholakala kuma-phyllosilicates angama-coarse-grained, kanye nasezindaweni ezinokwakheka kwekhabhoni okunephunga elimnandi (noma C = C) (Fig. 3c, d).Ngokuphambene, i-A0037,22 (I-Supplementary Fig. 3) ibonise kancane okuqukethwe okuphansi kwezifunda ze-aliphatic carbon-rich.I-mineralogy eyisisekelo yalezi zinhlamvu inothile nge-carbonates, efana ne-chondrite CI 16, ephakamisa ukuguqulwa okubanzi kwamanzi omthombo (Ithebula Lokwengeza 1).Izimo ze-oxidizing zizovuna ukugxila okuphezulu kwamaqembu asebenzayo we-carbonyl ne-carboxyl kumakhompiyutha ezinto eziphilayo ahlotshaniswa ne-carbonates.Ukusatshalaliswa kwe-submicron yezinto eziphilayo ezinezakhiwo ze-aliphatic carbon kungahluka kakhulu ekusatshalalisweni kwama-silicates anengqimba eqinile.Amacebo ezinto eziphilayo ze-aliphatic ezihlotshaniswa ne-phyllosilicate-OH atholwe ku-meteorite ye-Tagish Lake.Idatha ehlanganisiwe ye-microanalytical iphakamisa ukuthi izinto eziphilayo ezicebile kuma-aliphatic compounds zingase zisakazeke kuma-asteroids ohlobo lwe-C futhi zihlotshaniswe eduze nama-phyllosilicates.Lesi siphetho sihambisana nemibiko yangaphambilini yama-CH aliphatic/aromatic ezinhlayiyeni ze-Ryugu eziboniswa yi-MicroOmega, isibonakhulu esiseduze ne-infrared hyperspectral.Umbuzo obalulekile futhi ongaxazululiwe ukuthi izakhiwo eziyingqayizivele ze-aliphatic carbon-rich rich organic compounds ezihlotshaniswa nama-coarse-grained phyllosilicates abonwe kulolu cwaningo atholakala kuphela ku-asteroid Ryugu.
a, i-NEXAFS carbon spectra ijwayeleke ibe ngu-292 eV endaweni enephunga elimnandi (C=C) (ebomvu), endaweni ecebile ye-aliphatic (eluhlaza), kanye naku-matrix (eluhlaza okwesibhakabhaka).Umugqa ompunga yi-Murchison 13 i-insoluble organic spectrum uma uqhathanisa.noma, iyunithi yokulamula.b, Iskena se-X-ray microscopy (STXM) isithombe esibukwayo se-carbon K-edge esibonisa ukuthi isigaba sibuswa ikhabhoni.c, isiqephu esiyinhlanganisela ye-RGB enezifunda ezinothile (C=C) ezicebile (ezibomvu), izifunda ezicebile ze-aliphatic (okuluhlaza), kanye ne-matrix (eluhlaza okwesibhakabhaka).d, izinto eziphilayo ezinothe ngezinhlanganisela ze-aliphatic zigxile ku-phyllosilicate enamahhadla, indawo ikhuliswa kusukela emabhokisini anamachashazi amhlophe ku-b no-c.e, ama-nanospheres amakhulu (ng-1) endaweni akhuliswe ukusuka ebhokisini elinamachashazi amhlophe kokuthi b no-c.Ngoba: pyrrhotite.I-Pn: i-nickel-chromite.f, Nanoscale Secondary Ion Mass Spectrometry (NanoSIMS), Hydrogen (1H), Carbon (12C), kanye ne-Nitrogen (12C14N) izithombe eziyisisekelo, 12C/1H izithombe zesilinganiso sesici, kanye nesiphambano esingu-δD, δ13C, kanye nezithombe ze-isotopu ezingu-δ15N - Isigaba PG-3C esine-presolar 1: i-presolar Tablement 4 enothe kakhulu (i-presolar 1).
Izifundo ze-Kinetic zokucekelwa phansi kwezinto eziphilayo kuma-meteorites e-Murchison zinganikeza ulwazi olubalulekile mayelana nokusatshalaliswa okuhlukahlukene kwe-aliphatic organic matter enothe ngezinhlamvu ze-Ryugu.Lolu cwaningo lubonisa ukuthi amabhondi e-aliphatic CH ku-organic matter aphikelela aze afike ezingeni lokushisa eliphezulu elingaba ngu-30°C kumzali kanye/noma ashintshe ngobudlelwano bezinga lokushisa lesikhathi (isb. iminyaka engu-200 ku-100°C kanye no-0°C eminyakeni eyizigidi eziyi-100) ..Uma i-precursor ingashiswa ezingeni lokushisa elinikeziwe isikhathi esingaphezu kwesikhathi esithile, ukusatshalaliswa kwangempela kwe-aliphatic organics ecebile ku-phyllosilicate kungase kugcinwe.Kodwa-ke, izinguquko zamanzi omthombo we-rock zingase zibe nzima le ncazelo, njengoba i-A0037 ecebile nge-carbonate ingabonisi noma yiziphi izifunda ze-aliphatic ezine-carbon ezihlotshaniswa nama-phyllosilicates.Lokhu kushintsha kwezinga lokushisa eliphansi cishe kuhambisana nokuba khona kwe-cubic feldspar kuzinhlamvu ze-Ryugu (Ithebula Lokwengeza 1) 20.
Ingxenyana engu-C0068.25 (ng-1; Amakhiwane 3a–c,e) iqukethe i-nanosphere enkulu ebonisa iphunga elimnandi kakhulu (noma C=C), i-aliphatic emaphakathi, kanye ne-spectra ebuthakathaka ye-C(=O)O kanye ne-C=O..Isiginesha yekhabhoni ye-aliphatic ayifani nesiginesha yenqwaba yezinto eziphilayo ezingancibilikiyo kanye nama-nanospheres wemvelo ahlotshaniswa nama-chondrites (Umfanekiso 3a) 17,21.Ukuhlaziywa kwe-Raman kanye ne-infrared spectroscopic yama-nanospheres eLake Tagish kubonise ukuthi aqukethe i-aliphatic kanye ne-oxidized organic compounds kanye ne-disordered polycyclic aromatic organic compounds nesakhiwo esiyinkimbinkimbi22,23.Ngenxa yokuthi i-matrix ezungezile iqukethe izinto eziphilayo ezinothile ngenhlanganisela ye-aliphatic, isiginesha ye-aliphatic carbon ku-ng-1 ingase ibe i-artifact yokuhlaziya.Kuyathakazelisa ukuthi i-ng-1 iqukethe ama-silicates a-amorphous ashumekiwe (Fig. 3e), ukuthungwa okungakabikwa kunoma yiziphi izinto eziphilayo ezingaphandle komhlaba.Ama-silicates angama-amorphous angase abe izingxenye zemvelo ze-ng-1 noma aphume ku-amorphization yama-silicates ane-aqueous/anhydrous nge-ion kanye/noma i-electron beam ngesikhathi sokuhlaziya.
Izithombe ze-NanoSIMS ion zesigaba se-C0068.25 (I-Fig. 3f) zibonisa izinguquko ezifanayo ku-δ13C naku-δ15N, ngaphandle kwezinhlamvu ze-presolar ezinokunothisa okukhulu kwe-13C kwe-30,811‰ (PG-1 kusithombe esingu-δ13C ku-Fig. 3f) (Ithebula Lokwengeza).Izithombe ze-X-ray eziyisisekelo zezinhlamvu nezithombe ze-TEM zokucaca okuphezulu zibonisa kuphela ukugcwala kwekhabhoni kanye nebanga phakathi kwezindiza eziyisisekelo ezingu-0.3 nm, ezihambisana negraphite.Kuyaphawuleka ukuthi amanani ka-δD (841 ± 394‰) kanye no-δ15N (169 ± 95‰), acetshiswe odabeni lwe-aliphatic organic oluhlotshaniswa nama-phyllosilicates anamahhadla, aphakama kancane kunesilinganiso saso sonke isifunda C (δD = 539 ‰ ± 1).‰, δ15N = 67 ± 15 ‰) kokuthi C0068.25 (Ithebula Lokwengeza 4).Lokhu kubheka kuphakamisa ukuthi i-aliphatic-rich rich phyllosilicates e-coarse-grained phyllosilicates ingase ibe ye-primitive kune-organics ezungezile, njengoba lokhu okulandelayo kungenzeka ukuthi kushintshisane nge-isotopic namanzi azungezile emzimbeni wangempela.Kungenjalo, lezi zinguquko ze-isotopic zingase futhi zihlobane nenqubo yokuqala yokubunjwa.Kuhunyushwa ukuthi ama-silicates anezingqimba ezinhle ku-CI chondrites akhiwa ngenxa yokuguqulwa okuqhubekayo kwamaqoqo okuqala angama-coarse-grained anhydrous silicate.I-aliphatic-rich rich organic matter kungenzeka ukuthi yakhiwe kusukela kuma-molecule angaphambili kudiski ye-protoplanetary noma i-interstellar medium ngaphambi kokwakhiwa kwesimiso sonozungezilanga, bese ishintshwa kancane ngesikhathi sokushintsha kwamanzi kumzimba womzali we-Ryugu (enkulu). Usayizi (<1.0 km) we-Ryugu mncane kakhulu ukuthi ungagcina ukushisa kwangaphakathi ngokwanele ukuze kuguqulwe amanzi ukuze kwakhe amaminerali anamanzi25. Usayizi (<1.0 km) we-Ryugu mncane kakhulu ukuthi ungagcina ukushisa kwangaphakathi okwanele ukuze kuguqulwe amanzi ukuze kwakhe amaminerali anamanzi25. Размер (<1,0 км) Рюгу слишком мал, чтобы поддерживать достаточное внутреннее тепло для водного изменения с образованием водных 5. Usayizi (<1.0 km) I-Ryugu incane kakhulu ukuthi ingakwazi ukugcina ukushisa okwanele kwangaphakathi ukuze amanzi ashintshe enze amaminerali amanzi25. 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. Usayizi weRyugu (<1.0 km) mncane kakhulu ukusekela ukushisa kwangaphakathi ukushintsha amanzi enze amaminerali amanzi25.Ngakho-ke, abanduleli be-Ryugu bangadingeka amashumi amakhilomitha ngosayizi.I-organic matter ecebile kuma-aliphatic compounds ingase igcine izilinganiso ze-isotope zangempela ngenxa yokuhlotshaniswa nama-phyllosilicates ama-coarse-grained.Kodwa-ke, imvelo eqondile yezinkampani ezithwala isisindo ze-isotopic ihlala ingaqinisekile ngenxa yokuhlangana okuyinkimbinkimbi nokuthambile kwezingxenye ezihlukahlukene kulezi zingxenyana ze-FIB.Lezi kungaba izinto eziphilayo ezicebile kumakhompiyutha e-aliphatic kuma-Ryugu granules noma ama-phyllosilicates amaholo azungezile.Qaphela ukuthi izinto eziphilayo cishe kuwo wonke ama-chondrites e-carbonaceous (okuhlanganisa nama-CI chondrites) avame ukuceba ngo-D kunama-phyllosilicates, ngaphandle kwe-CM Paris 24, 26 meteorites.
Iziqephu zevolumu engu-δD kanye no-δ15N wezingcezu ze-FIB ezitholwe ku-A0002.23 no-A0002.26, A0037.22 no-A0037.23 kanye no-C0068.23, C0068.25 kanye no-C0068.26 FIB tincetu (inani lezinhlayiyana ezintathu ze-RIM ye-compari yezingcezu eziyisikhombisa ze-SIM) ezinezinhlayiya ezintathu ze-FIB SIM isistimu yelanga ikhonjiswe emkhiwaneni.4 (Ithebula Lokwengeza 4)27,28.Izinguquko zevolumu ku-δD naku-δ15N kumaphrofayela we-A0002, A0037, kanye ne-C0068 zihambisana nalawo aku-IDP, kodwa ziphakeme kunama-chondrite e-CM ne-CI (Fig. 4).Qaphela ukuthi ububanzi bamanani angu-δD wesampula ye-Comet 29 (-240 ukuya ku-1655‰) bukhulu kunalelo le-Ryugu.Amavolumu δD kanye no-δ15N wamaphrofayela e-Ryukyu, njengomthetho, mancane kunesilinganiso sezinkanyezi ezinomsila zomndeni we-Jupiter kanye nefu le-Oort (Fig. 4).Amanani aphansi e-δD we-CI chondrite angase abonise umthelela wokungcoliswa komhlaba kulawa masampuli.Uma kubhekwa ukufana phakathi kwe-Bells, i-Lake Tagish, ne-IDP, i-heterogeneity enkulu kumanani angu-δD kanye no-δN ezinhlayiyeni ze-Ryugu ingase ibonise izinguquko kumasiginesha okuqala e-isotopic wezinto eziphilayo kanye nezamanzi kusistimu yelanga yakuqala.Izinguquko ezifanayo ze-isotopic ku-δD no-δN kuzinhlayiya ze-Ryugu ne-IDP ziphakamisa ukuthi kokubili kungenzeka kwakheke kusuka kokubalulekile okuvela emthonjeni ofanayo.Kukholakala ukuthi ama-IDP avela emithonjeni ye-cometary 14.Ngakho-ke, i-Ryugu ingase iqukathe izinto ezifana nenkanyezi enomsila kanye/noma okungenani isistimu yelanga yangaphandle.Kodwa-ke, lokhu kungase kube nzima kakhulu kunalokho esikusho lapha ngenxa (1) ingxube yamanzi ayi-spherulitic kanye ne-D-rich emzimbeni womzali 31 kanye (2) nesilinganiso se-comet sika-D/H njengomsebenzi we-cometary 32.Nokho, izizathu ze-heterogeneity ephawuliwe ye-hydrogen ne-nitrogen isotopes ezinhlayiyeni ze-Ryugu aziqondakali ngokugcwele, ngokwengxenye ngenxa yenani elilinganiselwe lokuhlaziya elitholakala namuhla.Imiphumela yezinhlelo ze-hydrogen ne-nitrogen isotope isaphakamisa ukuthi kungenzeka ukuthi i-Ryugu iqukethe izinto eziningi ezivela ngaphandle kwe-Solar System futhi ngaleyo ndlela ingase ibonise ukufana okuthile kwenkanyezi enomsila.Iphrofayela ye-Ryugu ayizange ibonise ukuhlobana okusobala phakathi kuka-δ13C no-δ15N (Ithebula Lokwengeza 4).
Ingqikithi yokwakheka kwe-isotopic ye-H ne-N yezinhlayiya ze-Ryugu (imibuthano ebomvu: A0002, A0037; imibuthano eluhlaza okwesibhakabhaka: C0068) ihlobana nobukhulu belanga 27, umndeni we-Jupiter mean (JFC27), kanye nenkanyezi enomsila yamafu ye-Oort (OCC27), IDP28, namachondrules e-carbonaceous.Ukuqhathaniswa kwe-meteorite 27 (CI, CM, CR, C2-ung).Ukwakheka kwe-isotopi kunikezwa kokuthi Ithebula Lokwengeza 4. Imigqa enamachashazi amanani e-isotope asemhlabeni we-H kanye no-N.
Ukuthuthwa kwezinto eziguquguqukayo (isb. izinto eziphilayo namanzi) ukuya eMhlabeni kusalokhu kuwukukhathazeka26,27,33.I-submicron organic matter ehlotshaniswa nama-phyllosilicates amaholo ezinhlayiyeni ze-Ryugu ezihlonzwe kulolu cwaningo zingase zibe umthombo obalulekile wokuguquguquka.Izinto eziphilayo kuma-phyllosilicates anezinhlamvu eziqinile zivikeleke kangcono ekuwohlokeni16,34 kanye nokubola35 kunezinto eziphilayo kumatrices anezinhlamvu ezinhle.Ukwakheka kwe-isotopic ye-hydrogen esindayo ezinhlayiyeni kusho ukuthi akunakwenzeka ukuba kube ukuphela komthombo wokuguquguquka ohanjiswe eMhlabeni wokuqala.Zingaxutshwa nezingxenye ezinokwakheka kwe-hydrogen isotopic elula, njengoba kusanda kuhlongozwa ku-hypothesis yokuba khona kwamanzi aqhutshwa umoya welanga kuma-silicates.
Kulolu cwaningo, sibonisa ukuthi ama-meteorite e-CI, naphezu kokubaluleka kwawo kwe-geochemical njengabamele ukwakheka okuphelele kwesistimu sonozungezilanga, i-6,10 amasampuli angcolile asemhlabeni.Siphinde futhi sinikeze ubufakazi obuqondile bokusebenzelana phakathi kwento ephilayo ecebile ye-aliphatic kanye namaminerali angama-hydrous angomakhelwane futhi siphakamisa ukuthi i-Ryugu ingase iqukathe i-extrasolar material37.Imiphumela yalolu cwaningo ikhombisa ngokucacile ukubaluleka kwesampula eqondile ye-protoasteroids kanye nesidingo sokuthutha amasampula abuyisiwe ngaphansi kwezimo ezingasebenzi ngokuphelele neziyinyumba.Ubufakazi obuvezwe lapha bubonisa ukuthi izinhlayiya ze-Ryugu ngokungangabazeki zingenye yezinto ezingangcolisiwe kakhulu zesimiso sonozungezilanga ezitholakalayo ukuze kwenziwe ucwaningo lwaselabhorethri, futhi ukucwaninga okwengeziwe kwala masampula ayigugu ngokungangabazeki kuzokwandisa ukuqonda kwethu izinqubo zakuqala zesistimu sonozungezilanga.Izinhlayiya ze-Ryugu zimelela kahle kakhulu ukwakheka okuphelele kwesimiso sonozungezilanga.
Ukuze sinqume izakhiwo ze-microstructure eziyinkimbinkimbi kanye nezakhi zamakhemikhali zamasampuli esikali se-submicron, sisebenzise ukuhlaziywa kwe-synchrotron radiation-based computed tomography (SR-XCT) kanye ne-SR X-ray diffraction (XRD) -CT, FIB-STXM-NEXAFS-NanoSIMS-TEM.Akukho ukucekelwa phansi, ukungcola ngenxa yomkhathi womhlaba, futhi akukho monakalo ovela ezinhlayiyeni ezinhle noma amasampula emishini.Okwamanje, senze ukuhlaziywa kwevolumu ehlelekile sisebenzisa i-electron microscopy (SEM)-EDS, i-EPMA, i-XRD, i-instrumental neutron activation analysis (INAA), kanye nemishini ye-laser oxygen isotope fluorination.Izinqubo zokuhlola ziboniswa Emfanekisweni Owengeziwe 3 futhi ukuhlola ngakunye kuchazwe ezigabeni ezilandelayo.
Izinhlayiya ze-asteroid Ryugu zitholwe kumojula yokungena kabusha ye-Hayabusa-2 futhi zalethwa ku-JAXA Control Center e-Sagamihara, e-Japan, ngaphandle kokungcolisa umkhathi woMhlaba4.Ngemva kokubonakala kwezinhlamvu zokuqala nezingonakali endaweni ephethwe i-JAXA, sebenzisa iziqukathi zokudlulisa phakathi kwezindawo ezivalekayo kanye nezikhwama zesampula zama-capsule (ikristalu yesafire engu-10 noma 15 mm ububanzi nensimbi engagqwali, kuye ngosayizi wesampula) ukuze ugweme ukuphazamiseka kwemvelo.imvelo.y kanye/noma ukungcola komhlabathi (isb. umhwamuko wamanzi, ama-hydrocarbon, amagesi omkhathi nezinhlayiya ezinhle) kanye nokungcola okunqamula amasampula ngesikhathi sokulungiselela isampula kanye nokuthuthwa phakathi kwezikhungo namanyuvesi38.Ukuze ugweme ukucekelwa phansi nokungcola ngenxa yokusebenzelana nomkhathi womhlaba (umhwamuko wamanzi nomoya-mpilo), zonke izinhlobo zokulungiselela isampula (kuhlanganise nokuchofa ngeshizolo le-tantalum, kusetshenziswa isaha ledayimane elilinganisiwe (i-Meiwa Fosis Corporation DWS 3400) kanye nokusikwa kwe-epoxy) ukulungiselela ukufakwa) zenziwa ebhokisini legilavu ​​ngaphansi kwephuzu elihlanzekile elingu-60 ~ 10 ℃ kuya ku-60 ℃ kuya ku-200 C kuya ku-60 ℃ ukuya ku-2000 C. ).Zonke izinto ezisetshenziswa lapha zihlanzwa ngenhlanganisela yamanzi e-ultrapure kanye ne-ethanol kusetshenziswa amaza e-ultrasonic amaza ahlukene.
Lapha sifunda iqoqo le-National Polar Research Institute (NIPR) le-meteorite ye-Antarctic Meteorite Research Center (CI: Orgueil, CM2.4: Yamato (Y)-791198, CY: Y-82162 kanye ne-CY: Y 980115).
Ukudlulisa phakathi kwamathuluzi e-SR-XCT, NanoSIMS, STXM-NEXAFS nokuhlaziywa kwe-TEM, sisebenzise umbambi wesampula we-ultrathin jikelele ochazwe ezifundweni zangaphambili38.
Ukuhlaziywa kwe-SR-XCT kwamasampuli e-Ryugu kwenziwa kusetshenziswa uhlelo oludidiyelwe lwe-CT lwe-BL20XU/SPring-8.Uhlelo oludidiyelwe lwe-CT luqukethe izindlela ezihlukahlukene zokulinganisa: insimu ebanzi yokubuka kanye nemodi yokuxazulula okuphansi (WL) ukuze uthwebule sonke isakhiwo sesampula, inkambu encane yokubuka kanye nemodi yokuxazulula okuphezulu (NH) yokulinganisa okunembile kwendawo yesampula.intshisekelo nama-radiographs ukuze kutholwe iphethini ye-diffraction yevolumu yesampula, nokwenza i-XRD-CT ukuthola umdwebo we-2D wezigaba zamaminerali zendiza evundlile kusampula.Qaphela ukuthi zonke izilinganiso zingenziwa ngaphandle kokusebenzisa isistimu eyakhelwe ngaphakathi ukuze kukhishwe umbambi wesampula kusukela kusisekelo, okuvumela izilinganiso ezinembile ze-CT ne-XRD-CT.Umtshina we-X-ray wemodi ye-WL (BM AA40P; i-Hahamatsu Photonics) ifakwe enye ikhamera ye-4608 × 4608 pixel metal-oxide-semiconductor (CMOS) (C14120-20P; I-Hamamatsu Photonics) ene-scintillator ehlanganisa ugqinsi lwe-10 lutetim 3 lutetium1 kanye ne-crystal ye-Alluminum eyodwa beka ilensi.Usayizi wephikseli kumodi ye-WL cishe u-0.848 µm.Ngakho, inkambu yokubuka (i-FOV) kumodi ye-WL icishe ibe ngu-6 mm kumodi ye-CT ye-offset.Umtshina we-X-ray wemodi ye-NH (BM AA50; Hamamatsu Photonics) wawufakwe i-gadolinium-aluminium-gallium garnet ewugqinsi engu-20 µm (Gd3Al2Ga3O12) scintillator, ikhamera ye-CMOS (C11440-22CU) enesixazululo esingu-2048 × 2048;Hamamatsu Photonics) kanye ne-×20 lens.Usayizi wephikseli kumodi ye-NH ngu-~0.25 µm futhi inkambu yokubuka ingu-~0.5 mm.Umtshina wemodi ye-XRD (BM AA60; Hamamatsu Photonics) wawufakwe i-scintillator ehlanganisa isikrini esingu-50 µm esiwugqinsi se-P43 (Gd2O2S:Tb), ikhamera ye-CMOS elungiswa ngamaphikseli angu-2304 × 2304 (C15440-20UP) kanye ne-Hamma renics renics.Umtshina unosayizi wamaphikseli osebenzayo ongu-19.05 µm kanye nenkundla yokubuka engu-43.9 mm2.Ukwandisa i-FOV, sisebenzise inqubo ye-CT ye-offset kumodi ye-WL.Isithombe esidlulisiwe sokukhanya sokwakhiwa kabusha kwe-CT siqukethe isithombe esikububanzi obungu-180° ukuya ku-360° esiboniswa ngokuvundlile ku-eksisi yokuzungezisa, kanye nesithombe kububanzi obungu-0° ukuya ku-180°.
Kumodi ye-XRD, i-X-ray beam igxilwe yi-Fresnel zone plate.Kule modi, umtshina ubekwa ngemuva kwesampula ngo-110 mm kanti isitobhi se-beam singama-3 mm ngaphambi komtshina.Izithombe ezihlukanisiwe ku-2θ zisuka ku-1.43° ukuya ku-18.00° (i-grating pitch d = 16.6–1.32 Å) zitholwe ngendawo ye-X-ray egxile ezansi endaweni yokubuka yomtshina.Isampula ihamba iqonde phezulu ngezikhathi ezijwayelekile, ngokujika okuyingxenye kwesinyathelo ngasinye sokuskena esiqondile.Uma izinhlayiya zamaminerali zenelisa isimo se-Bragg lapho sizungeziswa ngo-180°, kuyenzeka kutholwe i-diffraction yezinhlayiya zamaminerali endizeni evundlile.Izithombe ze-diffraction zibe sezihlanganiswa zibe isithombe esisodwa sesinyathelo ngasinye sokuskena esiqondile.Izimo zokuhlola ze-SR-XRD-CT zicishe zifane nalezo zokuhlolwa kwe-SR-XRD.Kumodi ye-XRD-CT, umtshina ubekwe ku-69 mm ngemuva kwesampula.Izithombe ezihlukanisiwe kububanzi obungu-2θ zisukela ku-1.2° kuye ku-17.68° (d = 19.73 kuya ku-1.35 Å), lapho kokubili i-X-ray ne-beam limiter kuhambisana nendawo emaphakathi yendawo yokubuka yomtshina.Skena isampula ngokuvundlile bese uzungezisa isampula ngo-180°.Izithombe ze-SR-XRD-CT zakhiwe kabusha ngokuqina kwamaminerali aphezulu njengamavelu ephikseli.Ngokuskena okuvundlile, isampula ngokuvamile iskenwa ngezinyathelo ezingu-500–1000.
Kuzo zonke izivivinyo, amandla e-X-ray ayemiswe ku-30 ​​keV, njengoba lokhu kuwumkhawulo ophansi wokungena kwe-X-ray kuma-meteorite anobubanzi obungaba ngu-6 mm.Inombolo yezithombe ezitholwe kuzo zonke izilinganiso ze-CT ngesikhathi sokuzungezisa okungu-180° yayingu-1800 (3600 kuhlelo lwe-CT ye-offset), futhi isikhathi sokuchayeka sezithombe sasingu-100 ms kumodi ye-WL, 300 ms kumodi ye-NH, 500 ms ye-XRD, kanye no-50 ms .ms ye-XRD-CT ms.Isikhathi esijwayelekile sokuskena isampula cishe imizuzu engu-10 kumodi ye-WL, imizuzu engu-15 kumodi ye-NH, amahora angu-3 e-XRD, namahora angu-8 ku-SR-XRD-CT.
Izithombe ze-CT zakhiwa kabusha ngokuqagela emuva kwe-convolutional futhi zajwayezwa i-coefficient yomugqa wokunciphisa ukusuka ku-0 kuye ku-80 cm-1.Isofthiwe ye-Slice yasetshenziswa ukuhlaziya idatha ye-3D futhi isofthiwe ye-muXRD yasetshenziswa ukuze kuhlaziywe idatha ye-XRD.
Izinhlayiya ze-Ryugu ezigxilwe yi-Epoxy (A0029, A0037, C0009, C0014 kanye ne-C0068) zapholishwa kancane kancane endaweni zafika ezingeni lefilimu yedayimane elingu-0.5 µm (3M) ngaphansi kwezimo ezomile, igwema ukuthintana nendawo engaphezulu phakathi nenqubo yokupholisha.Indawo epholishiwe yesampula ngayinye yaqale yahlolisiswa ngemakroskopu ekhanyayo kwase kuba ngama-electron ahlakazekile emuva ukuze kutholwe izithombe ze-mineralogy nokuthungwa (BSE) zamasampuli nezinto ezisezingeni eliphakeme ze-NIPR kusetshenziswa i-JEOL JSM-7100F SEM efakwe i-energy dispersive spectrometer (AZtec).amandla) isithombe.Kusampula ngayinye, okuqukethwe kwezinto ezinkulu nezincane kwahlaziywa kusetshenziswa i-electron probe microanalyzer (EPMA, JEOL JXA-8200).Hlaziya izinhlayiya ze-phyllosilicate ne-carbonate ku-5 nA, izindinganiso zemvelo nezokwenziwa ku-15 keV, ama-sulfides, i-magnetite, i-olivine, ne-pyroxene ku-30 ​​nA.Amamaki e-Modal abalwe kusukela ku-elementi yamamephu nasezithombeni ze-BSE kusetshenziswa isofthiwe ye-ImageJ 1.53 enemikhawulo efanelekile esethelwe ngokungafanele kumaminerali ngayinye.
Ukuhlaziywa kwe-isotope ye-oxygen kwenziwa e-Open University (Milton Keynes, UK) kusetshenziswa i-infrared laser fluorination system.Amasampula e-Hayabusa2 alethwa e-Open University 38 ngeziqukathi ezigcwele i-nitrogen ukuze adluliselwe phakathi kwezinsiza.
Ukulayishwa kwesampula kwenziwa ebhokisini legilavu ​​ye-nitrogen enezinga le-oxygen eligadiwe elingaphansi kuka-0.1%.Ngomsebenzi wokuhlaziya we-Hayabusa2, kwakhiwe isibambi sesampula esisha se-Ni, esihlanganisa izimbobo zesampula ezimbili kuphela (ububanzi obungu-2.5 mm, ukujula okungu-5 mm), enye eyezinhlayiya ze-Hayabusa2 enye eyezinga langaphakathi le-obsidian.Ngesikhathi sokuhlaziya, umthombo wesampula oqukethe okokusebenza kwe-Hayabusa2 umbozwe ngefasitela langaphakathi le-BaF2 elicishe libe ngu-1 mm ubukhulu no-3 mm ububanzi ukuze libambe isampula ngesikhathi sokusabela kwe-laser.Ukugeleza kwe-BrF5 kusampula kunakekelwe isiteshi sokuxuba igesi esisikwe kumbambi wesampula we-Ni.Igumbi lesampula liphinde lahlelwa kabusha ukuze likwazi ukukhishwa emugqeni we-vacuum fluorination bese livulwa ebhokisini legilavu ​​eligcwele i-nitrogen.Igumbi elinezicucu ezimbili lalivalwe ngophawu lokucindezela olufakwe i-copper kanye ne-EVAC Quick Release CeFIX 38 chain clamp.Iwindi eliwugqinsi elingu-3 mm le-BaF2 phezulu kwegumbi livumela ukubhekwa ngasikhathi sinye kwesampula nokushisisa nge-laser.Ngemva kokulayisha isampula, qinisa ikamelo futhi bese uxhuma kabusha kulayini we-fluorinated.Ngaphambi kokuhlaziywa, igumbi lesampula lalishiswe ngaphansi kwe-vacuum cishe ku-95°C ngobusuku obubodwa ukuze kususwe noma imuphi umswakama we-adsorbed.Ngemva kokushisisa ubusuku bonke, igumbi lalivunyelwa ukuthi liphole lifike ezingeni lokushisa elilingana negumbi bese ingxenye evezwe emkhathini ngesikhathi sokudlulisa isampula yahlanzwa ngama-aliquot amathathu e-BrF5 ukuze kukhishwe umswakama.Lezi zinqubo ziqinisekisa ukuthi isampula ye-Hayabusa 2 ayivezwa emkhathini futhi ayingcoliswa umswakama ovela engxenyeni yomugqa we-fluorinated ongenelwa emoyeni ngesikhathi sokulayisha isampula.
Amasampula ezinhlayiyana ze-Ryugu C0014-4 ne-Orgueil (CI) ahlaziywa kumodi "eyodwa" eshintshiwe42, kuyilapho ukuhlaziywa kwe-Y-82162 (CY) kwenziwa kuthreyi eyodwa enesampula yemithombo eminingi41.Ngenxa yokwakheka kwawo okune-anhydrous, akudingekile ukusebenzisa indlela eyodwa yama-CY chondrites.Amasampuli ashiswe kusetshenziswa i-Photon Machines Inc. infrared CO2 laser.amandla angu-50 W (10.6 µm) agibele ku-gantry ye-XYZ phambi kwe-BrF5.Isistimu yevidiyo eyakhelwe ngaphakathi iqapha indlela yokusabela.Ngemuva kokufakwa kwe-fluorination, i-O2 ekhululiwe yahluzwa kusetshenziswa izicupho ezimbili ze-cryogenic nitrogen kanye nombhede oshisayo we-KBR ukuze kukhishwe noma iyiphi i-fluorine eyeqile.Ukwakheka kwe-isotopic komoya-mpilo ohlanzekile kwahlaziywa ku-Thermo Fisher MAT 253 ye-dual-channel mass spectrometer enokulungiswa okukhulu okungaba ngu-200.
Kwezinye izimo, inani le-O2 elinegesi elikhishwe ngesikhathi sokusabela kwesampula lalingaphansi kuka-140 µg, okuwumkhawulo olinganiselwe wokusebenzisa idivayisi ye-bellows ku-MAT 253 mass spectrometer.Kulezi zimo, sebenzisa ama-microvolumes ukuze uhlaziye.Ngemva kokuhlaziya izinhlayiya ze-Hayabusa2, indinganiso yangaphakathi ye-obsidian yashintshwa futhi kwanqunywa ukwakheka kwayo kwe-isotope ye-oxygen.
Ama-ion wesiqephu se-NF+ NF3+ aphazamisa ugongolo ngobuningi obungu-33 (16O17O).Ukuqeda le nkinga engaba khona, amasampula amaningi acutshungulwa kusetshenziswa izinqubo zokuhlukanisa i-cryogenic.Lokhu kungenziwa ngendlela eya phambili ngaphambi kokuhlaziywa kwe-MAT 253 noma njengokuhlaziywa kwesibili ngokubuyisela igesi ehlaziywe ku-sieve ekhethekile yamangqamuzana futhi iphinde idlulise ngemva kokuhlukaniswa kwe-cryogenic.Ukuhlukaniswa kwe-Cryogenic kuhilela ukuhlinzeka ngegesi kusihlungi samangqamuzana ekushiseni kwe-nitrogen ewuketshezi bese siyikhipha kusisefo esiyinhloko samangqamuzana ezingeni lokushisa elingu-130°C.Ukuhlola okubanzi kubonise ukuthi i-NF+ isala kusihlungi sokuqala samangqamuzana futhi akukho ukuhlukaniswa okubalulekile okwenzekayo kusetshenziswa le ndlela.
Ngokusekelwe ekuhlaziyweni okuphindaphindiwe kwezindinganiso zethu zangaphakathi ze-obsidian, ukunemba okuphelele kwesistimu kumodi ye-bellows ithi: ±0.053‰ ku-δ17O, ±0.095‰ ku-δ18O, ±0.018‰ ku-Δ17O (2 sd).Ukuhlaziywa kwe-isotope ye-oxygen kunikezwa ku-delta notation ejwayelekile, lapho i-delta18O ibalwa ngokuthi:
Futhi sebenzisa isilinganiso esingu-17O/16O ku-δ17O.I-VSMOW iyindinganiso yamazwe ngamazwe ye-Vienna Mean Sea Water Standard.I-Δ17O imele ukuchezuka emugqeni wokuhlukaniswa komhlaba, futhi ifomula yokubala ithi: Δ17O = δ17O – 0.52 × δ18O.Yonke imininingwane evezwe ku-Supplementary Table 3 ishintshiwe.
Izigaba ezicishe zibe ngu-150 kuya ku-200 nm obukhulu zikhishwe ezinhlayiyeni ze-Ryugu kusetshenziswa ithuluzi le-Hitachi High Tech SMI4050 FIB e-JAMSTEC, i-Kochi Core Sampling Institute.Qaphela ukuthi zonke izigaba ze-FIB zitholwe ezingxenyeni ezingacutshungulwanga zezinhlayiya ezingakacutshungulwa ngemva kokukhishwa emikhunjini egcwele igesi ye-N2 ukuze kudluliselwe izinto ezingaphakathi.Lezi zingcezu azizange zikalwe nge-SR-CT, kodwa zacutshungulwa ngokuchayeka okuncane emkhathini womhlaba ukuze kugwenywe ukulimala okungaba khona kanye nokungcoliswa okungase kuthinte i-spectrum ye-carbon K-edge.Ngemva kokufakwa kongqimba oluvikelayo lwe-tungsten, isifunda esithakaselwayo (esifika ku-25 × 25 μm2) sisikwa futhi sancishiswa nge-Ga+ ion beam nge-voltage esheshayo engu-30 kV, bese kuba ngu-5 kV kanye ne-probe current engu-40 pA ukuze kuncishiswe umonakalo ongaphezulu.Izingxenye ze-ultrathin zabe sezibekwa phezu kwemeshi yethusi ekhulisiwe (i-Kochi mesh) 39 kusetshenziswa i-micromanipulator efakwe i-FIB.
I-Ryugu A0098 (1.6303mg) kanye ne-C0068 (0.6483mg) amapellets avalwa kabili emashidini e-polyethylene ahlanzekile kakhulu ebhokisini legilavu ​​eligcwele initrogen ku-SPring-8 ngaphandle kokusebenzelana nomkhathi womhlaba.Ukulungiswa kwesampula kwe-JB-1 (itshe lereferensi ye-geological ekhishwe i-Geological Survey yase-Japan) kwenziwa e-Tokyo Metropolitan University.
I-INAA ibanjelwe e-Institute for Integrated Radiation and Nuclear Sciences, eNyuvesi yaseKyoto.Amasampula afakwe imisebe kabili ngemijikelezo yokunisela ehlukene ekhethwe ngokuya ngesigamu sempilo ye-nuclide esetshenziselwa ukulinganisa kwezakhi.Okokuqala, isampula yafakwa kwithubhu ye-pneumatic irradiation imizuzwana engu-30.Ukuguquguquka kwama-neutron ashisayo nasheshayo kufig.Oku-3 kungu-4.6 × 1012 kanye no-9.6 × 1011 cm-2 s-1, ngokulandelana, ukuze kutholwe okuqukethwe kwe-Mg, Al, Ca, Ti, V kanye ne-Mn.Amakhemikhali afana ne-MgO (99.99% purity, Soekawa Chemical), Al (99.9% purity, Soekawa Chemical), kanye ne-Si metal (99.999% purity, FUJIFILM Wako Pure Chemical) nawo afakwe imisebe ukuze alungise ukuphazamisa ukusebenza kwenuzi okufana no-(n, n).Isampula iphinde i-radiated ne-sodium chloride (i-99.99% ubumsulwa; i-MANAC) ukulungisa izinguquko ku-neutron flux.
Ngemva kokukhanya kwe-neutron, ishidi le-polyethylene langaphandle lathathelwa indawo elisha, futhi imisebe ye-gamma ekhishwa isampula nereferensi yalinganiswa ngokushesha ngomtshina we-Ge.Amasampula afanayo aphinde afakwe imisebe amahora angu-4 kuthubhu ye-pneumatic irradiation.I-2 ine-neutron fluxes eshisayo nesheshayo engu-5.6 1012 kanye no-1.2 1012 cm-2 s-1, ngokulandelana, ukuze kutholakale i-Na, K, Ca, Sc, Cr, Fe, Co, Ni, Zn, Ga, As, Content Se, Sb, Os, Ir kanye ne-Au.Amasampuli okulawula we-Ga, As, Se, Sb, Os, Ir, kanye ne-Au afakwe imisebe ngokusebenzisa amanani afanelekile (kusuka ku-10 kuye ku-50 μg) wezixazululo ezijwayelekile zokugxilisa okwaziwayo kwalezi zakhi ezicushweni ezimbili zephepha lokuhlunga, okulandelwa ukushiswa kwamasampula.Ukubalwa kwe-gamma ray kwenziwa e-Institute of Integrated Radiation and Nuclear Sciences, Kyoto University kanye naseRI Research Centre, Tokyo Metropolitan University.Izinqubo zokuhlaziya nezinto eziyisethenjwa zokunqunywa kobuningi bezinto ze-INAA ziyafana nalezo ezichazwe emsebenzini wethu wangaphambilini.
I-X-ray diffractometer (Rigaku SmartLab) yasetshenziselwa ukuqoqa amaphethini okushintshashintsha amasampula e-Ryugu A0029 (<1 mg), A0037 (≪1 mg) kanye ne-C0087 (<1 mg) ku-NIPR. I-X-ray diffractometer (Rigaku SmartLab) yasetshenziselwa ukuqoqa amaphethini okushintshashintsha amasampula e-Ryugu A0029 (<1 mg), A0037 (≪1 mg) kanye ne-C0087 (<1 mg) ku-NIPR. Рентгеновский дифрактометр (Rigaku SmartLab) использовали для сбора дифракционных картин образцов Ryugu A0029 (<1 мг), A0037 (≤037) (≪1 мг) и 1 мг. I-X-ray diffractometer (Rigaku SmartLab) isetshenziselwe ukuqoqa amaphethini e-diffraction e-Ryugu A0029 (<1 mg), A0037 (≪1 mg), ne-C0087 (<1 mg) amasampuli ku-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) kanye C0087 (<1 мг) были получены в NIPR с использованием рентгеновгенгей ренгеного в NIPR с использованием рентгеновгенов рентгеновгенов ренгеновгенов ренгеного длучены в NIPR). Amaphethini we-X-ray diffraction wamasampuli Ryugu A0029 (<1 mg), A0037 (<1 mg) kanye ne-C0087 (<1 mg) atholwe e-NIPR kusetshenziswa i-X-ray diffractometer (Rigaku SmartLab).Wonke amasampula agaywa aba impushana ecwebezelayo kusinkwa esiyisicwecwana se-silicon esingabukisi kusetshenziswa ipuleti lengilazi yesafire abese asatshalaliswa ngokulinganayo ku-silicone wafer engabukisi ngaphandle kwanoma yiluphi uketshezi (amanzi noma utshwala).Izimo zokulinganisa zimi kanje: Imisebe ye-Cu Kα X-ray ikhiqizwa ku-voltage yeshubhu engu-40 kV kanye neshubhu lamanje elingu-40 mA, ubude bomkhawulo obunqunyiwe bungu-10 mm, i-divergence angle ingu-(1/6)°, isivinini sokuzungeza esindizeni singu-20 rpm, futhi ububanzi buthatha amahora angu-2θ (0 0 kabili kuya ku-3)° i-engeli ye-Brauble engu-3.Kwasetshenziswa iBragg Brentano Optics.Umtshina ungumtshina we-silicon semiconductor one-dimensional one-dimensional (D/teX Ultra 250).Ama-X-ray e-Cu Kβ akhishwe kusetshenziswa isihlungi se-Ni.Kusetshenziswa amasampula atholakalayo, izilinganiso ze-synthetic magnesian saponite (JCSS-3501, Kunimine Industries CO. Ltd), inyoka (leaf serpentine, Miyazu, Nikka) kanye ne-pyrrhotite (monoclinic 4C, Chihua, Mexico Watts) ziqhathaniswe ukuze kuhlonzwe iziqongo kanye nokusetshenziswa kwedatha yedatha ye-PDF Diffraction1 idatha yedatha ye-PDF. 071-1662) kanye ne-magnetite (PDF 00-019-0629).Idatha ye-Diffraction evela ku-Ryugu iphinde yaqhathaniswa nedatha ye-hydroaltered carbonaceous chondrites, i-Orgueil CI, Y-791198 CM2.4, kanye ne-Y 980115 CY (isigaba sokushisa III, 500–750°C).Ukuqhathanisa kubonise ukufana ne-Orgueil, kodwa hhayi nge-Y-791198 kanye ne-Y 980115.
I-spectra ye-NEXAFS ene-carbon edge K yezingxenye ze-ultrathin zamasampuli enziwe kusukela ku-FIB zikalwa kusetshenziswa isiteshi se-STXM BL4U esikhungweni se-UVSOR synchrotron e-Institute of Molecular Sciences (Okazaki, Japan).Usayizi wendawo we-beam ogxile ngokubonakalayo nge-Fresnel zone plate cishe u-50 nm.Isinyathelo samandla singu-0.1 eV ngesakhiwo esihle sesifunda sonqenqema (283.6–292.0 eV) kanye no-0.5 eV (280.0–283.5 eV kanye no-292.5–300.0 eV) ezifundeni ngaphambili nangemuva.isikhathi sephikseli yesithombe ngasinye sasisethwe ukuze sibe ngu-2 ms.Ngemva kokuphuma, igumbi lokuhlaziya le-STXM lagcwaliswa nge-helium ngengcindezi engaba ngu-20 mbar.Lokhu kusiza ekunciphiseni ukukhukhuleka okushisayo kwemishini ye-X-ray optics ekamelweni nesibambi sesampula, kanye nokunciphisa umonakalo wesampula kanye/noma ukukhishwa kwe-oxidation.I-NEXAFS K-edge carbon spectra yenziwe ngedatha estakiwe kusetshenziswa isofthiwe ye-aXis2000 kanye nesofthiwe yokuphathelene yokucubungula idatha ye-STXM.Qaphela ukuthi isampula yekesi lokudlulisa kanye nebhokisi legilavu ​​kusetshenziselwa ukugwema isampula ye-oxidation nokungcoliswa.
Kulandela ukuhlaziywa kwe-STXM-NEXAFS, ukwakheka kwe-isotopic ye-hydrogen, i-carbon, ne-nitrogen yezingcezu ze-Ryugu FIB kwahlaziywa kusetshenziswa isithombe se-isotope nge-JAMSTEC NanoSIMS 50L.I-Cs+ primary beam egxilile engaba ngu-2 pA yokuhlaziywa kwe-carbon ne-nitrogen isotope kanye ne-13 pA yokuhlaziywa kwe-hydrogen isotope ihlelwa kabusha endaweni engaba ngu-24 × 24 µm2 kuya ku-30 ​​× 30 µm2 kusampula.Ngemva kokufafazwa kusengaphambili kwemizuzu emi-3 endaweni eqinile yensimbi eyisisekelo, ukuhlaziya ngakunye kwaqalwa ngemva kokuqiniswa kokuqina kwensimbi yesibili.Ukuze kuhlaziywe ama-isotopes ekhabhoni ne-nitrogen, izithombe ze-12C–, 13C–, 16O–, 12C14N– kanye ne-12C15N– zitholwe kanyekanye kusetshenziswa ukutholwa kwama-electron ayisikhombisa okuphindaphindeka kwe-multiplex ene-mass resolution cishe engu-9000, eyanele ukuhlukanisa zonke izinhlanganisela ze-isotopic ezifanele.ukuphazamiseka (okungukuthi 12C1H ku-13C kanye ne-13C14N ku-12C15N).Ukuze kuhlaziywe ama-isotopes e-hydrogen, izithombe ze-1H-, 2D- kanye ne-12C- zitholwe ngokulungiswa kwesisindo esingaba ngu-3000 ngokutholwa okuningi kusetshenziswa iziphindaphinda ezintathu zama-electron.Ukuhlaziya ngakunye kuqukethe izithombe eziskeniwe ezingu-30 zendawo efanayo, nesithombe esisodwa esinamaphikseli angu-256 × 256 wokuhlaziywa kwe-carbon ne-nitrogen isotope kanye namaphikiseli angu-128 × 128 wokuhlaziywa kwe-hydrogen isotope.Isikhathi sokulibaziseka singu-3000 µs ngephikseli ngayinye yokuhlaziywa kwe-carbon ne-nitrogen isotope kanye no-5000 µs ngephikseli ngayinye yokuhlaziywa kwe-hydrogen isotope.Sisebenzise i-1-hydroxybenzotriazole hydrate njengezindinganiso ze-hydrogen, carbon kanye ne-nitrogen isotope ukuze silinganise ukuhlukaniswa kwensimbi yensimbi45.
Ukunquma ukwakheka kwe-silicon isotopic ye-presolar graphite kuphrofayela ye-FIB C0068-25, sisebenzise iziphindaphinda zama-electron eziyisithupha ezinokulungiswa kwesisindo okungaba ngu-9000. Izithombe ziqukethe amaphikseli angu-256 × 256 nesikhathi sokulibaziseka esingu-3000 µs ngephikseli ngayinye.Silinganise ithuluzi lokuhlukanisa ngobuningi sisebenzisa ama-silicon wafers njengamazinga e-hydrogen, carbon, kanye ne-silicon isotope.
Izithombe ze-Isotope zacutshungulwa kusetshenziswa isofthiwe ye-NASA ye-NanoSIMS45 imaging.Idatha yalungiselelwa isikhathi esifile sokuphindaphinda ama-electron (44 ns) kanye nemiphumela yokufika ngesikhathi esisodwa.Ukuqondanisa okuhlukile kokuskena kwesithombe ngasinye ukuze kulungiswe ukukhukhuleka kwesithombe ngesikhathi sokutholwa.Isithombe sokugcina se-isotopu senziwa ngokungeza ama-ion esibili esithombeni ngasinye kuphikseli ngayinye yokuskena.
Ngemva kokuhlaziywa kwe-STXM-NEXAFS ne-NanoSIMS, izigaba ze-FIB ezifanayo zahlolwa kusetshenziswa isibonakhulu se-electron yokudlulisela (JEOL JEM-ARM200F) ku-voltage esheshayo engu-200 kV e-Kochi, e-JAMSTEC.I-microstructure ibonwe kusetshenziswa i-TEM yensimu ekhanyayo kanye ne-TEM yokuskena ephezulu endaweni emnyama.Izigaba zamaminerali zihlonzwe nge-spot electron diffraction kanye ne-lattice band imaging, futhi ukuhlaziya amakhemikhali kwenziwa yi-EDS ngomtshina we-silicon drift 100 mm2 kanye nesofthiwe ye-JEOL Analysis Station 4.30.Ukuze uthole ukuhlaziya ubuningi, ubukhulu be-X-ray besici be-elementi ngayinye bulinganiswe ngemodi yokuskena ye-TEM ngesikhathi esinqunyiwe sokutholwa kwedatha esingu-30 s, indawo yokuskena ye-~100 × 100 nm2, kanye ne-beam current engu-50 pA.Isilinganiso (Si + Al)-Mg-Fe kumasilicate anengqimba sanqunywa kusetshenziswa i-coefficient k yokuhlola, elungiselwe ukujiya, etholwe ezingeni le-pyropagarnet yemvelo.
Zonke izithombe nokuhlaziya okusetshenziswe kulolu cwaningo kuyatholakala ku-JAXA Data Archiving and Communication System (DARTS) https://www.darts.isas.jaxa.jp/curation/hayabusa2.Lesi sihloko sinikeza idatha yangempela.
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