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Science - Coggle Diagram

- - - - F = ma
        
        The second law explains how the velocity of an object changes when it is subjected to an external force. The law defines a force to be equal to change in momentum (mass times velocity) per change in time
    - - For every action there is an equal and opposite reaction.
    - - An object that is in motion or staying still will continue in that state until force opposes or acts upon it.
        
        Newton's first law states that every object will remain at rest or in uniform motion in a straight line unless compelled to change its state by the action of an external force. This is normally taken as the definition of inertia.
  - - - Standard method of measuring matter.(Kilogram ,Gram, Tonnes)
    - - How fast a given object it moving.(m/s)
        
        s = d/t
    - - The length of a given path.(m, km, cm)
  - - - The energy an object has when above the ground or currently falling.
      - Formula: m = mass, g = gravity, h = height
        
        Ep = mgh
    - - The energy gathered when an object is in motion.
      - Formula
        
        Ek = 1/2mv^2
  - - - The mass of an object with gravitational factors (varies from planet to planet due to difference in gravity).(Kilogram, gram, tonnes)
    - - The direct distance from point a to be regardless of the path with a direction.(Km, m, cm/N, E, S, W)
    - - The speed and direction of a given object.(m/s/N, E, S, W)
        
        v = S/t
  - - - In physics, power is the amount of energy transferred or converted per unit time. In the International System of Units, the unit of power is the watt, equal to one joule per second. In older works, power is sometimes called activity. Power is a scalar quantity.
    - - Work, in physics, measure of energy transfer that occurs when an object is moved over a distance by an external force at least part of which is applied in the direction of the displacement.
- - - - The path of the planets about the sun is elliptical in shape, with the center of the sun being located at one focus. (The Law of Ellipses)
    - - The ratio of the squares of the periods of any two planets is equal to the ratio of the cubes of their average distances from the sun. (The Law of Harmonies)
    - - An imaginary line drawn from the center of the sun to the center of the planet will sweep out equal areas in equal intervals of time. (The Law of Equal Areas)
  - - - CMBR
        
        The cosmic microwave background (CMB) is thought to be leftover radiation from the Big Bang, or the time when the universe began. As the theory goes, when the universe was born it underwent a rapid inflation and expansion. The CMB represents the heat left over from the Big Bang.
      - Creation of Light Elements
        
        Since the universe first started the atoms combined into very simple elements such as hydrogen and helium.
      - Expansion
        
        The idea that everything is getting pushed a way from each other when the force of expansion overcomes the gravitational pull together
      - Formation of galaxies
        
        This proves gravity as masses of stars and dust combined to forma galaxies and nebulae.
    - - The Stages after the big bang in the first few seconds to millions of years. Archie says 'Cameron yours has nothing pfft' ill just kick you or i just wont organise it into dot points u can do that hoe
        
        Quark
        
        Quark Epoch, from 10–12 seconds to 10–6 seconds:
        Quarks, electrons and neutrinos form in large numbers as the universe cools off to below 10 quadrillion degrees, and the four fundamental forces assume their present forms. Quarks and antiquarks annihilate each other upon contact, but, in a process known as baryogenesis, a surplus of quarks (about one for every billion pairs) survives, which will ultimately combine to form matter.
        
        Hadron
        
        Hadron Epoch, from 10–6 seconds to 1 second:
        The temperature of the universe cools to about a trillion degrees, cool enough to allow quarks to combine to form hadrons (like protons and neutrons). Electrons colliding with protons in the extreme conditions of the Hadron Epoch fuse to form neutrons and give off massless neutrinos, which continue to travel freely through space today, at or near to the speed of light. Some neutrons and neutrinos re-combine into new proton-electron pairs. The only rules governing all this apparently random combining and re-combining are that the overall charge and energy (including mass-energy) be conserved.
        
        Inflationary
        
        Inflationary Epoch, from 10–36 seconds to 10–32 seconds:
        Triggered by the separation of the strong nuclear force, the universe undergoes an extremely rapid exponential expansion, known as cosmic inflation. The linear dimensions of the early universe increases during this period of a tiny fraction of a second by a factor of at least 1026 to around 10 centimeters (about the size of a grapefruit). The elementary particles remaining from the Grand Unification Epoch (a hot, dense quark-gluon plasma, sometimes known as “quark soup”) become distributed very thinly across the universe.
        
        Nucleosynthesis
        
        Nucleosynthesis, from 3 minutes to 20 minutes:
        The temperature of the universe falls to the point (about a billion degrees) where atomic nuclei can begin to form as protons and neutrons combine through nuclear fusion to form the nuclei of the simple elements of hydrogen, helium and lithium. After about 20 minutes, the temperature and density of the universe has fallen to the point where nuclear fusion cannot continue.
        
        Plank
        
        Planck Epoch (or Planck Era), from zero to approximately 10-43 seconds (1 Planck Time):
        This is the closest that current physics can get to the absolute beginning of time, and very little can be known about this period. General relativity proposes a gravitational singularity before this time (although even that may break down due to quantum effects), and it is hypothesized that the four fundamental forces (electromagnetism, weak nuclear force, strong nuclear force and gravity) all have the same strength, and are possibly even unified into one fundamental force, held together by a perfect symmetry which some have likened to a sharpened pencil standing on its point (i.e. too symmetrical to last). At this point, the universe spans a region of only 10-35 meters (1 Planck Length), and has a temperature of over 1032°C (the Planck Temperature).
        
        Dark
        
        Dark Age (or Dark Era), from 300,000 to 150 million years:
        The period after the formation of the first atoms and before the first stars is sometimes referred to as the Dark Age. Although photons exist, the universe at this time is literally dark, with no stars having formed to give off light. With only very diffuse matter remaining, activity in the universe has tailed off dramatically, with very low energy levels and very large time scales. Little of note happens during this period, and the universe is dominated by mysterious “dark matter”.
    - - Steady-state theory, in cosmology, a view that the universe is always expanding but maintaining a constant average density, with matter being continuously created to form new stars and galaxies at the same rate that old ones become observable as a consequence of their increasing distance and velocity of recession.
    - - The Big Bang Theory is the leading explanation about how the universe began. At its simplest, it says the universe as we know it started with a small singularity, then inflated over the next 13.8 billion years to the cosmos that we know today.
  - - - A celestial object that is much smaller than a normal star and has insufficient mass to sustain nuclear fusion but that is hot enough to radiate energy especially at infrared wavelengths
    - - A Stellar nebula
        A star forms from massive clouds of dust and gas in space, also known as a nebula. Nebulae are mostly composed of hydrogen.
        Gravity begins to pull the dust and gas together.
        
        Protostar
        As the mass falls together it gets hot. A star is formed when it is hot enough for the hydrogen nuclei to fuse together to make helium. The fusion process releases energy, which keeps the core of the star hot.
        
        Massive Stars:
        Massive stars are born, just like average stars, out of clouds of dust called nebulae. When a nebula collects enough mass, it begins to collapse under its own gravity. The internal pressure created by this collapse is enough to trigger fusion of hydrogen deep in its core. When nuclear fusion begins, a star is born. If the cloud of dust is large, it will create a massive star. A star is considered massive if it is at least eight times more massive than our Sun.
        
        A red supergiant is an aging giant star that has consumed its core's supply of hydrogen fuel. Helium has accumulated in the core, and hydrogen is now undergoing nuclear fusion in the outer shells. These shells then expand, and the now cooler star takes on a red color. They are the largest known stars.
        
        Supernova
        A larger star with more mass will go on making nuclear reactions, getting hotter and expanding until it explodes as a supernova. An exploding supernova throws hot gas into space.
        
        Neutron star or black hole
        Depending on the mass at the start of its life, a supernova will leave behind either a neutron star or a black hole.
        
        Main sequence star
        During this stable phase in the life of a star, the force of gravity holding the star together is balanced by higher pressure due to the high temperatures. The Sun is at this stable phase in its life.
        
        Red giant star
        When all the hydrogen has been used up in the fusion process, larger nuclei begin to form and the star may expand to become a red giant.
        
        White dwarf
        When all the nuclear reactions are over, a small star like the Sun may begin to contract under the pull of gravity. In this instance, the star becomes a white dwarf which fades and changes colour as it cools.
- - - - Protons, Neutrons and Electrons make up the atom with Protons and Neutrons Being the the Nucleus and the Electrons orbiting it in the electron cloud
    - - The Atomic number states that amount of protons in the nucleus of an atom, it also tells us where on the periodic table it is.
    - - The Atomic Mass is equal to the amount of protons and neutrons added together, we usually don't however include the electrons because they at extremely small and don't way much.
    - - Atoms are made of protons(positive charge) neutrons(neutral charge) and electrons(negative charge)
      - The Nucleus
        
        The nucleus is made up of Protons and Neutrons. The amount of protons are equal to the Atomic Number, and you can find the number of neutrons by subtracting the amount of protons from the Atomic Mass.
    - - Cations
        
        Cations are the opposite of Anions as they are positively charged ions which have lost an electron to be like their closest Nobel Gas and be stable.
      - Nobel Gasses
        
        The Nobel Gasses have a complete electron cloud and their valence electrons fill the outermost layer, this means that are stable.
      - Anions
        
        Anions are negatively charged ions that have gained an electron to be like the closest Nobel Gas to become stable
  - - - How the same amount of valence electrons(electrons in the outermost shell)
    - - Elements with the same charge meaning they react similarly and have similar properties
    - - Alkali Earth Music - Group 2
      - Transitions Metals - GRoup 3 - 12
      - Alkali Metals - Group 1
      - Nobel Gasses - Stable gasses as all there outer shells are filled and complete
      - Halogens - Group 17
  - - - Acid + Base --> Salt+ Water
      - Acid + Metal --> Salt+ Hydrogen Gas
      - Acid + Carbonate --> Carbon Dioxide + Water + Salt
  - - - Ionic bonding is a type of chemical bonding that involves the electrostatic attraction between oppositely charged ions, and is the primary interaction occurring in ionic compounds. It is one of the main types of bonding along with covalent bonding and metallic bonding.
    - - A covalent bond, also called a molecular bond, is a chemical bond that involves the sharing of electron pairs between atoms. These electron pairs are known as shared pairs or bonding pairs, and the stable balance of attractive and repulsive forces between atoms, when they share electrons, is known as covalent bonding.
    - - Metallic bonding is a type of chemical bonding that rises from the electrostatic attractive force between conduction electrons and positively charged metal ions. It may be described as the sharing of free electrons among a structure of positively charged ions.