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Распространенность химических элементов.pptx

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Распространенность химических элементов Илья Векслер лекция в ПГНИУ, 7 октября 2013 Распространенность химических элементов Илья Векслер лекция в ПГНИУ, 7 октября 2013

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Michail Vasil‘evic LOMONOSOV 1711 - 1765 Student der Marburger Universität 1736 – 1739 «Везде Michail Vasil‘evic LOMONOSOV 1711 - 1765 Student der Marburger Universität 1736 – 1739 «Везде исследуйте всечасно Что есть велико и прекрасно Чего еще не видел свет»

Hydrogen atom Hydrogen atom

Helium (4 He) atom Helium (4 He) atom

4 He atom: Quantum model Atom mass: 6. 67 10 -27 kg (1 fm 4 He atom: Quantum model Atom mass: 6. 67 10 -27 kg (1 fm = 10 -15 m)

How did H and He atoms (= 99 % of all the atoms in How did H and He atoms (= 99 % of all the atoms in the Universe) form ?

Big Bang Big Bang

Cosmic microwave background radiation T = 3 °K NASA / WMAP Science Team 2012 Cosmic microwave background radiation T = 3 °K NASA / WMAP Science Team 2012

Today Atoms 4. 6% Dark matter 23% Dark energy 72% 13. 7 billion years Today Atoms 4. 6% Dark matter 23% Dark energy 72% 13. 7 billion years ago Dark matter 63% Neutrinos 10% Photons 15% Atoms 12% (Universe is 370, 000 years old)

“α-β-γ paper” Ralph Alpher 1921 - 2007 George Gamow 1904 - 1968 “α-β-γ paper” Ralph Alpher 1921 - 2007 George Gamow 1904 - 1968

? ? ? Gaps at masses 5 and 8 ? ? ? Only D, ? ? ? Gaps at masses 5 and 8 ? ? ? Only D, 3 He and 4 He were able to form by neutron capture!

Where do the heavy elements form ? Where do the heavy elements form ?

Fred Hoyle 1915 - 2001 Fred Hoyle 1915 - 2001

Our star - the Sun Our star - the Sun

Death of a Sunlike star Death of a Sunlike star

Supernova 1987 A Supernova 1987 A

Crab nebula resulted from the Supernova explosion 1054 A. D. Now 10 light years Crab nebula resulted from the Supernova explosion 1054 A. D. Now 10 light years in diameter, still expanding at about 680 km/s

10 Binding energy per barion, Me. V 56 Fe 16 O 12 C 8 10 Binding energy per barion, Me. V 56 Fe 16 O 12 C 8 4 He 11 B 6 9 Be 6 Li 4 fusion fission 3 He 2 D 0 0 20 40 60 80 100 Isotope mass, amu 120 140

10 Binding energy per barion, Me. V 56 Fe 16 O 12 C 8 10 Binding energy per barion, Me. V 56 Fe 16 O 12 C 8 4 He 11 B 6 9 Be 6 Li 4 Produced inside stars Produced in Supernova explosions 3 He 2 D 0 0 20 40 60 80 100 Isotope mass, amu 120 140

Element abundances in the Solar system 100000 1000 Atoms per 1 Si atom 100 Element abundances in the Solar system 100000 1000 Atoms per 1 Si atom 100 H He O 10 1 0. 01 0. 0001 1 E-05 1 E-06 1 E-07 1 E-08 Si Fe

Condensation: from gas to dust Condensation: from gas to dust

O’Neill & Palme, 1998 O’Neill & Palme, 1998

Allende meteorite (2 Feb 1969) 1 cm 3 Allende meteorite (2 Feb 1969) 1 cm 3

Allende meteorite (2 Feb 1969) CAI 1 cm 3 Allende meteorite (2 Feb 1969) CAI 1 cm 3

Accretion: from dust and gas to stars and planets Accretion: from dust and gas to stars and planets

The Solar system The Solar system

O’Neill & Palme, 1998 O’Neill & Palme, 1998

The Earth The Earth

Differentiation of the Earth Differentiation of the Earth

The birth of the Earth – the first 700 million years Halliday (2001) The birth of the Earth – the first 700 million years Halliday (2001)

O’Neill & Palme, 1998 O’Neill & Palme, 1998

Bulk Earth’s mantle Al Ca S Ni 1. 41 2. 9 1. 8 1. Bulk Earth’s mantle Al Ca S Ni 1. 41 2. 9 1. 8 1. 54 Fe 5. 8 O 30. 1 Fe 32. 1 Mg 13. 9 Si 15. 1 Mg 22. 8 Al Ca 2. 2 2. 3 Si 21. 5 O 44. 8

O’Neill & Palme, 1998 O’Neill & Palme, 1998

Composition of the crust Continental Oceanic Si. O 2 60. 2 48. 6 Al Composition of the crust Continental Oceanic Si. O 2 60. 2 48. 6 Al 2 O 3 15. 2 16. 5 Ca. O 5. 5 12. 3 Mg. O 3. 1 6. 8 Fe. O 3. 8 6. 2 Na 2 O 3 2. 6 K 2 O 2. 8 0. 4 Fe 2 O 3 2. 5 2. 3 H 2 O 1. 4 1. 1 CO 2 1. 4 Ti. O 2 0. 7 1. 4 P 2 O 5 0. 2 0. 3 Total 99. 6 99. 9 Ronov & Yaroshevsky (1969)

O’Neill & Palme, 1998 O’Neill & Palme, 1998