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Pu³tusk – Podróże Humboldta – Porowate Chondryty

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Pu³tusk – Podróże Humboldta – Porowate Chondryty KWARTALNIK MI£OŒNIKÓW METEORYTÓW METEORYTMETEORYT Nr 2 (50) Czerwiec 2004 ISSN 1642-588X W numerze: – Pu³tusk – podró¿e Humboldta – porowate chondryty – meteoryty w Smithsonian Institution – ping-pong w kosmosie Od redaktora: Meteoryt (ISSN 1642-588X) – biuletyn dla mi³oœników mete- Wszystkie pomys³y uczczenia wydania 50 numeru mia³y jedn¹ orytów wydawany przez Olsz- zasadnicz¹ wadê: wymaga³y wiêcej pracy. Niestety numer ukazuje siê tyñskie Planetarium i Obserwa- w porze najwiêkszego natê¿enia pracy zawodowej obu redaktorów torium Astronomiczne, Muzeum i wydanie normalnego numeru o tej porze roku wymaga du¿ego Miko³aja Kopernika we From- poœwiêcenia. Fajerwerków wiêc nie ma. borku i Pallasite Press – wydaw- Jednym z pomys³ów by³a wiêksza liczba artyku³ów polskich cê kwartalnika Meteorite, z któ- autorów. Pomys³ w zasadzie podoba³ siê paru osobom, do których rego pochodzi wiêksza czêœæ pu- blikowanych materia³ów. zwróci³em siê z tak¹ propozycj¹, ale gdy przysz³o do realizacji, to okaza³o siê, ¿e niemal ka¿dy ma wa¿niejsze obowi¹zki. Paradoksalnie Redaguje Andrzej S. Pilski sporo miejsca polskiemu meteorytowi poœwiêci³ O. Richard Norton. Sk³ad: Jacek Dr¹¿kowski S¹ wiêc w numerze dwa polskie meteoryty i to w kolorze. Druk: Jan, Lidzbark Warm. Chcia³bym zwróciæ uwagê na relacjê z Muzeum Przyrodniczego Adres redakcji: w Bernie, w Szwajcarii. Wytworzy³o siê ostatnio przeœwiadczenie, ¿e skr. poczt. 6 zinstytucjonalizowane poszukiwania meteorytów s¹ nieskuteczne 14-530 Frombork i nowe meteoryty odnajduje siê jedynie dziêki prywatnym tel. (0-55) 243-7218 w. 23 poszukiwaczom. Przyk³ad Muzeum z Berna pokazuje, ¿e mo¿e byæ e-mail: [email protected] inaczej. Kolejny raz przekonujemy siê, ¿e nie jest wa¿na forma lecz Biuletyn wydawany jest kwartal- treœæ. W ka¿dych warunkach organizacyjnych mo¿na dzia³aæ dobrze nie i dostêpny g³ównie w prenu- lub Ÿle. meracie. Roczna prenumerata Ze wzglêdów formalno-prawnych znikn¹³ na pewien czas wynosi w 2004 roku 32 z³. Zain- internetowy katalog meteorytów w zbiorach polskich. Ostatnio jego teresowanych prosimy o wp³ace- twórcy powiadomili, ¿e katalog ju¿ zaczyna dzia³aæ, ale trzeba go nie tej kwoty na konto Olsztyñ- szukaæ pod nowym adresem: http://meteoryty.sarrus-net.com lub po skiego Planetarium i Obserwato- rium Astronomicznego nr: prostu klikn¹æ na winietkê katalogu na stronie Polskiego Serwisu 88 1540 1072 2001 5000 3724 0002 Meteorytów. w BOŒ SA O/Olsztyn, Sytuacja ta uprzytomni³a fakt, ¿e katalog internetowy jest zaznaczaj¹c cel wp³aty i podaj¹c wprawdzie bardzo wygodny i ³atwy do aktualizowania, ale mo¿e czytelny adres. równie ³atwo znikn¹æ. Trzeba wiêc bêdzie chyba pomyœleæ o nowym Wczeœniejsze roczniki powielane wydaniu katalogu w formie ksi¹¿kowej tym bardziej, ¿e ostatnie s¹ na zamówienie za op³at¹ równ¹ wydanie powoli siê wyczerpuje. wysokoœci aktualnej prenumeraty. Andrzej S. Pilski Zapraszamy na strone, 200 lat figur Thomsona Polskiego Serwisu Meteorytowego: jba1.republika.pl Subscribe to METEORITE Pallasite Press P.O. Box 33-1218 Takapuna, Auckland NEW ZEALAND 4 issues per year $US30 (2nd class airmail) VISA & MasterCard accepted www.meteor.co.nz Canyon Diablo. Kolekcja Martina Altmanna. str. 2 METEORYT 2/2004 Pu³tusk i inne kawa³ki gruzu z planetoidy 6 Hebe Andrzej S. Pilski a aukcjach internetowych po- ale przewa¿nie nie s¹ one przeciête jawiaj¹ siê od czasu do czasu i niewiele jest okazji do zobaczenia ich Nfragmenty meteorytu Pu³tusk. struktury. Mimo to uda³o mi siê zoba- Ogl¹daj¹c je mo¿na odnieœæ wra¿enie, czyæ okazy o jednolitej budowie, ze s³a- ¿e pochodz¹ z zupe³nie ró¿nych mete- bo widocznymi chondrami, ¿y³kowa- orytów. Szczególnie p³ytki, które doœæ ne lub nie, takie w³aœnie, jakich regularnie oferuje Michael Farmer, fragmenty oferuje Farmer. Jego okazy przypominaj¹ wygl¹dem bardziej frag- pochodz¹ jednak z Naturhistorisches menty El Hammami ni¿ okaz, który Museum w Wiedniu. Widzia³em te¿ opisuje w tym numerze dr Jacek Sie- okazy zbrekcjowane z okruchami sza- Fot. 2. Zbrekcjowana p³ytka Pu³tuska z kolek- mi¹tkowski. Jak w³aœciwie powinien rymi i ¿ó³tawymi, przy czym ¿ó³tawe cji autora, z której wykonano szlif opisany przez wygl¹daæ ten meteoryt? zabarwienie wyraŸnie nie by³o wyni- dr Siemi¹tkowskiego. Wymiary 30×19 mm kiem wietrzenia. Napotka³em te¿ oka- stopniem zwietrzenia. Wymieni³em tyl- zy z doœæ grubymi ¿y³kami, a nawet ko najpopularniejsze, ale lista podob- natrafi³em w zbiorach Muzeum Wy- nych meteorytów jest d³uga. Wydaje siê dzia³u Geologii UW na ma³y okaz coraz bardziej prawdopodobne, ¿e Pu³tuska bêd¹cy w ca³oœci stopem po- wszystkie one pochodz¹ z jednej ma³ej zderzeniowym. Ciemna materia bez wi- planety. docznej struktury i bez œladu chondr, Fot. 3. (ok³adka) Piêtka Pu³tuska o brekcjowej jedynie z ziarenkami metalu, która zwy- budowie. U góry jasna ¿y³ka metalu. Na pozo- kle tworzy ¿y³ki, tutaj tworzy³a ca³y sta³ej czêœci przekroju metal jest ciemny. Wymiary Fot. 1. Fragment Pu³tuska o jednorodnej bu- meteoryt. Meteoryty pu³tuskie mog¹ 41×25 mm. dowie oferowany przez Farmera. Wymiary wiêc wygl¹daæ bardzo ró¿nie. Zdaniem naukowców najlepsz¹ 20×16 mm. Kolekcja Dariusza Tuzinowskiego. Statystyka wskazuje, ¿e co trzeci kandydatk¹ na macierzyst¹ planetkê Pytanie wydawa³oby siê retorycz- spadaj¹cy na Ziemiê meteoryt wygl¹- Pu³tuska jest planetoida 6 Hebe. Kr¹¿y ne. Pu³tusk jest brekcj¹ regolitow¹ da tak samo, jak Pu³tusk. Istotnie bar- ona wokó³ S³oñca w wewnêtrznej czê- zaliczan¹ do typu H5 wiêc powinien za- dzo podobne do meteorytów pu³tuskich œci pasa planetoid po lekko eliptycznej wieraæ doœæ du¿o ziaren metalu i niezbyt s¹ okazy z deszczów meteorytowych orbicie wchodz¹cej w obszar rezonan- du¿o chondr oraz powinien sk³adaæ siê Jilin, Juancheng, czy Zag, a tak¿e Gao- su 3:1 z Jowiszem i usytuowanej bar- ν z okruchów. Problem polega na tym, ¿e Guenie. Ten ostatni odró¿nia siê tylko dzo blisko rezonansu wiekowego 6. Jak te okruchy mog¹ byæ du¿e, a wiêkszoœæ prze- krojów Pu³tuska, jakie mo¿na zobaczyæ, jest ma³a. Nawet w przypad- ku okazu z Muzeum Mi- neralogicznego UJ w Krakowie nie ma pewno- œci, czy jest to fragment litej ska³y, na której osia- da³ gruz, czy te¿ frag- ment wyj¹tkowo du¿ego okruchu z gruzowiska. W chondrycie H5 Pla- inview zdarzaj¹ siê okru- chy o rozmiarach kilku- nastu centymetrów. W polskich zbio- rach zachowa³o siê doœæ Fot. 4. P³ytka Portales Valley. Przestrzeñ miêdzy okruchami wype³nia metal (na zdjêciu ciemny). Wymiary 62 x 43 du¿o okazów Pu³tuska, mm. Kolekcja Kazimierza Mazurka. METEORYT str. 3 wyliczono, wystarczy aby po zderze- niu od³amki uzyska³y prêdkoœæ 280 m/s i ju¿ wchodz¹ w obszar rezonansu, sk¹d po nieca³ym milionie lat trafiaj¹ na orbitê przecinaj¹c¹ orbitê Ziemi. Oceniono, ¿e od³amki ska³ z tej plane- toidy mog¹ stanowiæ nawet 10% stru- mienia meteoroidów zmierzaj¹cych ku Ziemi, wiêc 6 Hebe mo¿e byæ Ÿród³em jednej z wiêkszych grup chondrytów zwyczajnych. Dlaczego w³aœnie chondrytów zwyczajnych? Ten typ meteorytów sprawia najwiêcej k³opotu, gdy chce- my odnaleŸæ jego macierzyste plane- toidy. Istnieje spora grupa planetoid typu S, ale ich widmo odbiciowe ró¿- ni siê doœæ wyraŸnie od widma chon- Fot. 5. P³ytka chondrytu H5 Juancheng: scementowany gruz z powierzchni 6 Hebe. Wymiary drytów zwyczajnych. Z jednej strony 52×32 mm. Kolekcja autora. mamy wiêc du¿¹ grupê meteorytów, których widmo odbiciowe nie pasuje z czego wyci¹gniêto wniosek, ¿e ma krzepniêcia chondrytowej ska³y w wy- do ¿adnej planetoidy, a z drugiej spor¹ ona doœæ jednorodn¹ budowê, a wiêc niku uderzenia fragmentu innej plane- grupê planetoid, których widma nie najprawdopodobniej nie uleg³a dyferen- toidy. Jednym z mocnych argumentów pasuj¹ do ¿adnych meteorytów. Dopie- cjacji. Dla porównania widmo zdyfe- za takim pochodzeniem meteorytów ro niedawno obserwacje Erosa z bli- rencjowanej Westy zmienia siê doœæ ¿elaznych IIE jest ich wiek, m³odszy ska pokaza³y, ¿e jedn¹ z przyczyn tych znacznie w trakcie jej wirowania, po- od wiêkszoœci meteorytów ¿elaznych. rozbie¿noœci jest tak zwane wietrze- niewa¿ na dnie g³êbokich kraterów wi- Meteoryty IIE powstawa³y jeszcze wte- nie kosmiczne. Widmo odbiciowe daæ ska³y z g³êbszych warstw o odmien- dy, gdy na ma³ych planetach zakoñczy³a z okolicy œwie¿o utworzonych krate- nym sk³adzie. siê aktywnoœæ magmowa, a ich ¿elazne rów znacznie lepiej pasuje do widma Sk³ad chemiczny krzemianów na j¹dra zakrzep³y. chondrytów zwyczajnych ni¿ œrednie powierzchni 6 Hebe odpowiada krze- Mo¿emy wiêc sobie wyobraziæ, ¿e widmo planetoidy typu S. mianom z chondrytów H. Problemem uderzenia skalnych fragmentów w po- Planetoida 6 Hebe jest zaliczana do jest jednak wysoka zdolnoœæ odbijania wierzchniê 6 Hebe powoduj¹ powsta- typu S, ale jest nietypowa pod tym w³a- œwiat³a, wiêksza ni¿ w przypadku chon- wanie ma³ych i wiêkszych kraterków, œnie wzglêdem, ¿e jej widmo jest bar- drytów H. Œwiat³o odbija siê tak, jakby przy czym energia zderzenia powodu- dziej zbli¿one do widma chondrytów znaczna czêœæ powierzchni tej planeto- je stopienie ska³y i zebranie siê p³ynne- zwyczajnych ni¿ widmo przeciêtnej idy by³a obita blach¹. Z ró¿nych mode- go metalu na dnie krateru. Tworz¹ siê planetoidy tego typu. Ma ona œrednicê li budowy powierzchni tej planetoidy w ten sposób mniejsze i wiêksze blasz- 185 km i obraca siê z okresem 7,274 najlepsz¹ zgodnoœæ z obserwacjami ki o ró¿nej gruboœci. Kolejne zderze- godziny. Podczas wirowania jej jasnoœæ da³o po³¹czenie 60% gruboziarnistej nia rozbijaj¹ pokrywaj¹c¹ je warstwê i kszta³t widma niewiele siê zmienia, mieszaniny materii chondrytu H z 40% krzemianów, a wstrz¹sy regolitu wywo- metalicznego ¿elaza niklonoœnego. ³ane uderzeniami powoduj¹, ¿e te blasz- Niedu¿e blaszki metalu nie s¹ ki wêdruj¹ stopniowo ku powierzchni.
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