Exploring The Earth (PDF)

WHAT’S IN? Exploring the EARTH Prepared BY: Jennica Lyn n. bagang, lpt  PRAYER Lord Jesus, Please give me a good mind that I may do all my works well in such a way that I will make you happy. Help me to understand and remember all the things...

WHAT’S IN? Exploring the EARTH Prepared BY: Jennica Lyn n. bagang, lpt  PRAYER Lord Jesus, Please give me a good mind that I may do all my works well in such a way that I will make you happy. Help me to understand and remember all the things that I must learn. Help me to enjoy and be happy with the subject which I find so hard. Amen. REFRESHER DRILL: Don’t worry, this aims to make you recall your previous knowledge about chemistry and physics. TRUE OR FALSE 1. Elements are made up of subatomic particles called electron, proton and neutron 2. The identity of an element depends on how many neutron it has 3. Protons have a negative charge and electrons have a positive charge 4. Lithium is one of the elements formed during big bang nucleosynthesis 5. Nucleosynthesis combines nucleons (PROTONS AND NEUTRONS) to form elements 6. The big bang is an explosion 7. The universe was colder 13.8 billion years ago 8. The higher the energy of the particles in an object are, the higher the temperature of that object will be 9. Mass can be converted into energy 10. Gravitational force is what makes matter pull and clump together LESSON 1: FORMATION OF UNIVERSE Prepared BY: Jennica Lyn n. bagang, lpt Learning Objectives: Describe the formation of heavier elements during the formation and evolution of stars; Cite astronomical evidence which justifies the formation of elements during stellar formation and evolution; Appreciate the importance of the discovery of atomic number which led to the synthesis of new elements in the laboratory.  ASTROphysics The application of physics to the study of celestial objects cosmology The study of the origin and development of the universe How did the universe began? and when? 13.8 Billion years ago the universe was born  THE BIG BANG The leading theory of how the universe began What do you imagine when you hear the word “Big Bang”?  THE BIG BANG Common misconception: It is NOT an explosion STORY TIME... Imagine the moment before the universe began Nothingness  How did this happen? Time = 0  Just some energy The appearance of some energy from no energy is the thing that must be explained.  Just some energy The emergence of DUALITY. PLUS and MINUS POSITIVE and NEGATIVE  0 (s) The emergence of the simplest possible thing. Therefore, nothing is something.  0 10^(-43) (s) After bigbang, we get to 10 to the negative 43. This time, still not much is known.  0 10^(-43) (s) Planck Epoch 10^32 K Too hot for any matter to exist Planck Epoch Time when 4 fundamental forces of the universe were unified.  0 10^(-43) (s) Planck Epoch THEORY OF EVERYTHING  0 10^(-43) (s) Planck Epoch Until now, particle accelerators haven’t yet achieved this.  0 10^(-43) 10^(-36) (s) Planck Grand Unification Epoch Epoch Temperature cooled 10^29 K down Grand Unification Epoch Gravity separates, leaving the electroweak and strong nuclear forces together.  0 10^(-43) 10^(-36) (s) Planck Grand Unification Epoch Epoch ELECTRO STRONG FORCE  0 10^(-43) 10^(-36) (s) Planck Grand Unification Epoch Epoch GRAND UNIFIED THEORY - electromagnetic, weak, and strong forces are merged into a single force.  0 10^(-43) 10^(-36) (s) Planck Grand Unification Epoch Epoch SYMMETRY BREAKING occured when extreme temperatures cool below transition temperatures  0 10^(-43) 10^(-36) 10^(-32) (s) Planck Grand Unification Electroweak Epoch Epoch Epoch Cool to frosty 10^28 K temperature Electroweak Epoch Decoupling of the strong nuclear force from the electrostrong force leaving only the electromagnetic and weak force together.  0 10^(-43) 10^(-36) 10^(-32) (s) Planck Grand Unification Inflationary Epoch Epoch Epoch Inflationary Epoch the universe underwent an extremely rapid exponential expansion.  0 10^(-43) 10^(-36) 10^(-32) (s) Planck Grand Unification Inflationary Epoch Epoch Epoch Inflationary Epoch The universe suddenly expanded by 26 orders of magnitude. It was like going from the size of a molecule (less than a billionth of a meter) to an object that is ten light-years across (60 trillion miles)  0 10^(-43) 10^(-36) 10^(-32) (s) Planck Grand Unification Inflationary Epoch Epoch Epoch The released of potential energy produced and ultra-hot PLASMA This plasma contains: QUARK ANTIQUARK GLUON  0 10^(-43) 10^(-36) 10^(-32) 10^(-12) (s) Planck Grand Unification Electroweak Quark Epoch Epoch Epoch Epoch FINAL SYMMETRY BREAKING (10^12 K) decoupling of This plasma contains: electromagnetic QUARK force and weak ANTIQUARK force (resulted in 4 GLUON forces)  0 10^(-43) 10^(-36) 10^(-32) 10^(-12) (s) Planck Grand Unification Electroweak Quark Epoch Epoch Epoch Epoch Quark Epoch Still too hot for protons and neutrons to form The highest epoch that we can currently probe with particle accelerators (transition from theoretical cosmology to experimental)  0 10^(-43) 10^(-36) 10^(-32) 10^(-12) 10^(-6) 1 (s) Planck Grand Unification Electroweak Quark Hadron Epoch Epoch Epoch Epoch Epoch 10^28 K Things finally cool down enough to form HADRONS (particles made of quarks) Hadron Epoch Heavy materials were formed such as Baryons (Protons and Neutrons) 1 s Large Hadron Collider  0 10^(-43) 10^(-36) 10^(-32) 10^(-12) 10^(-6) 1 (s) Planck Grand Unification Electroweak Quark Hadron Epoch Epoch Epoch Epoch Epoch Look at how much has happened in a SINGLE SECOND!  1 10 s (s) s Lepton Epoch Lepton Epoch The majority of hadrons and anti-hadrons annihilate each other at the end of the hadron epoch, leaving leptons and anti-leptons dominating the mass of the universe. Leptons includes electrons, neutrinos and their antiparticles.  1s 10 s (s) Lepton Epoch Matter vs Antimatter Matter and antimatter annihilate each other on contact, and researchers believe such collisions destroyed almost all of the antimatter 1 s  1s 10 s 17 min (s) Lepton Epoch Photon Epoch Photon Epoch After most leptons and anti-leptons are annihilated at the end of the lepton epoch the energy of the universe is dominated by photons. 10^9 to 10^7 K Cool enough for baryons to be stable but also hot enough not to fuse.  1s 10 s 17 min (s) Photon Epoch Lepton Epoch Big bang Nucleosynthesis Big bang Nucleosynthesis the temperature of the universe falls to the point where atomic nuclei can begin to form. Protons (hydrogen ions) and neutrons begin to combine into atomic nuclei in the process of nuclear fusion.  1 Big bang Nucleosynthesis s Too hot temperature Proton + Neutron = collided and destroyed Enough temperature Proton + Neutron = collided and combined NEW ELEMENTS WERE FORMED 1 Big bang Nucleosynthesis s Proton + Neutron = DEUTERON DEUTERON – isotope of Hydrogen (H) that has 1 proton and 1 neutron Proton + Neutron + Neutron= TRITON TRITON – isotope of Hydrogen (H) that has 1 proton and 2 neutron Proton + Proton + Neutron + Neutron= HELIUM 1 Proton – Hydrogen 2 Proton - Helium  1s 10 s 17 min (s) Photon Epoch Lepton Epoch Big bang Nucleosynthesis Big bang Nucleosynthesis NUCLEAR FUSION: These consisted only of the nuclei of the simplest chemical elements: mostly hydrogen and helium and some lithium and beryllium 1 Big bang Nucleosynthesis s Helium-4 + Triton = LITHIUM Helium-4 = 2 Proton & 2 Neutron Triton = 1 Proton & 2 Neutron 1 Big bang Nucleosynthesis s Helium-4 + Helium-5 = BERYLLIUM Helium-4 = 2 Proton & 2 Neutron Helium-5 = 2 Proton & 3 Neutron  1s 10 s 17 min (s) Photon Epoch Lepton Epoch Big bang Nucleosynthesis After that, it gets too cold... 3:1 (by mass)  1s 10 s 17 min 377,000 yrs (s) Photon Epoch Lepton Epoch Photon Epoch Big bang (continued) Nucleosynthesi s due to gravity expansion H and He nuclei collect continues to form cloud of gas  1s 10 s 17 min 377,000 yrs (s) Photon Epoch Lepton Epoch Photon Epoch Big bang (continued) Recombination Nucleosynthesis Big bang Nucleosynthesis Electrons emit PHOTON for the first time PHOTON - tiny particle that comprises 4,000 K waves of electromagnetic radiation Cool enough for electrons to -light is made up of photon combine with nuclei to form neutral atoms for the first time  1s 10 s 17 min 377,000 yrs (s) Photon Epoch Lepton Epoch Photon Epoch Big bang (continued) Recombination Nucleosynthesis The universe become visible  1s 10 s 17 min 377,000 yrs 150 million yrs (s) Photon Epoch Lepton Epoch Photon Epoch Dark Ages Big bang (continued) Recombination Nucleosynthesis DARK AGES Hydrogen Helium NO STARS Photons  1s 10 s 17 min 377,000 yrs 150 million yrs (s) Photon Epoch Lepton Epoch Photon Epoch Dark Ages Big bang (continued) Recombination Nucleosynthesis 4,000 K to 3,000 K This temperature would allow water to exist  1s 10 s 17 min 377,000 yrs 150 million yrs (s) Photon Epoch Lepton Epoch Photon Epoch Dark Ages Big bang (continued) Recombination Nucleosynthesis 60 K This temperature is cold enough for human beings to exist  1s 10 s 17 min 377,000 yrs 150 million yrs (s) Photon Epoch Lepton Epoch Photon Epoch Dark Ages Big bang (continued) Recombination Nucleosynthesis Hydrogen and Helium continue to collect over million of years Forming atoms of gas of cloud  1s 10 s 17 min 377,000 yrs 150 million yrs (s) Photon Epoch Lepton Epoch Photon Epoch Dark Ages Big bang (continued) Recombination Nucleosynthesis Hydrogen and Helium continue to collect over million of years Forming atoms of gas of cloud  1s 10 s 17 min 377,000 yrs 150 million yrs (s) Photon Epoch Lepton Epoch Photon Epoch Dark Ages Big bang (continued) Recombination Nucleosynthesis What happened next? 1 s EARLIEST AND LIGHT ELEMENTS HYDROGEN HELIUM LITHIUM BERYLLIUM How does the heavier elements formed? 1 s Note: as the universe expands it cools down Atoms requires enough energy to combine and form new elements. The higher the temperature, the higher the energy What area in the universe where it is hot? 1 s SUN NOTE: Our sun is a star 1 s STAR FORMATION Between 100 million and 250 million years after the big bang, star were formed. 1 s STELLAR NUCLEOSYNTHESIS When elements are formed inside a star Consists of Hydrogen and Helium and other dust Where the stars are born CLOUD OF GAS OR STELLAR NEBULA  1 PROTON-PROTON CHAIN REACTION s DEUTERON HELIUM 1 MAIN SEQUENCE STAR s Temperature increases to 100 million Kelvin Hydrogen shell Due to thermal pressure, Helium gases pushes out causes core it to become a RED GIANT STAR 1 UNDER RED GIANT STAR s Triple Alpha Process He-4 + He-4 = Be-8 Be-8 + He-4 = C-12 1 s ALPHA LADDER Elements fused to create more elements all the way to Fe (iron) 1 s Lightest element = H, He, Li, Be Heavier than Be = B to Fe  1 ALPHA LADDER s + = Note: 12 – number of neutron 6 – number of proton 1 ALPHA LADDER s + = 1 s HEAVIER ELEMENTS THAN BERYLLIUM CARBON TO IRON How does the heavier elements than iron formed? 1 s SUPERNOVA NUCLEOSYNTHESIS As the red giant star exhausted the nuclear fuel of light elements, its core started to collapse that eventually led to explosion. This is called SUPERNOVA - it released a huge amount of nuclear energy and produced, through neutron capture and radioactive decay, other elements heavier than iron. 1 s GIVE THE THREE NUCLEOSYNTHESIS Big Bang Nucleosynthesis Stellar Nucleosynthesis Supernova Nucleosynthesis 1 s FORMATION OF PLANETS How do you think the planets we observed today came into existence? NEBULAR HYPOTHESIS the most accepted scientific explanation for the solar system's formation. 1 The Primordial Solar Nebula: s A giant cloud of gas and dust (primarily hydrogen and helium) began to collapse about 4.6 billion years ago. Trigger: Could have been a nearby supernova explosion or gravitational instabilities. 1 Formation of the Protosun: s As the nebula collapsed under gravity, it spun faster, forming a rotating disk. Most of the material condensed at the center, forming the protosun (the precursor to the Sun). Nuclear fusion ignited in the core, creating the Sun. 1 Formation of the Protoplanetary Disk: s Remaining material flattened into a disk orbiting the protosun. Dust particles collided and stuck together, forming planetesimals. 1 Accretion and Formation of Planets: s Planetesimals coalesced into larger bodies, forming protoplanets. Inner disk: Rocky materials dominated due to high temperatures (terrestrial planets like Earth and Mars). Outer disk: Cooler temperatures allowed gases and ices to form (gas giants like Jupiter and Saturn). 1 Formation of Other Solar System Objects s 1. Moons ✓ Some moons formed from debris ejected during collisions, such as Earth's Moon. ✓ Others, like the moons of Jupiter, formed from leftover material around the planet. 2. Asteroids and Comets ✓ Asteroids: Rocky remnants in the asteroid belt between Mars and Jupiter. ✓ Comets: Icy bodies from the outer solar system (Kuiper Belt and Oort Cloud). Key Processes in Solar System Formation 1.Gravity: ✓ Played a central role in condensing material and forming celestial bodies. 2.Collision and Accretion: ✓ Smaller particles clumped together, leading to larger planetary bodies. 3.Differentiation: ✓ Heavier elements sank to form planetary cores, while lighter materials formed crusts. Evidence Supporting the Nebular Hypothesis 1.Observation of Protoplanetary Disks: ✓ Similar disks have been observed around young stars in space. 2.Composition of the Solar System: ✓ The Sun contains most of the mass, with planets orbiting in nearly the same plane. 3.Dating of Meteorites: ✓ Radiometric dating places the age of the solar system at ~4.6 billion years. Thank you very much!