Elements of Life Flashcards

1
Q

Isotope

A

Atoms of the same element (thus containing the same number of protons) with a different number of neutrons

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2
Q

Nuclear fission

A

A large nucleus (such as the Lanthanides and Actinides) splits into smaller nuclei, e.g. fission process used in nuclear power plants

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3
Q

Nuclear fusion

A

Smaller nuclei (such as hydrogen and helium) fuse to form a larger nucleus, e.g. creation of elements in stars

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4
Q

Alpha (α) radiation

A

A strongly ionising helium nucleus (2+ charge) with a short range (a few centimetres in air) in air. Very little deflection by a magnetic field; stopped by a sheet of paper

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5
Q

Beta (ß) radiation

A

Weakly ionising electrons (1- charge) emitted from the nucleus when a neutron decays into a proton and an electron. Travel a few metres in air; high deflection by a magnetic field; stopped by aluminium foil

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6
Q

Gamma (Ɣ)

A

Non-ionising electromagnetic radiation with a very long range in air. Not deflected by a magnetic field; stopped by a sheet of lead or several metres of concrete

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7
Q

α particle

A

4/2 He

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8
Q

ß particle

A

0/-1 e

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9
Q

Ɣ particle

A

Photons of high frequency electromagnetic radiation

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10
Q

Hydrogen fusion

A

The means by which stars release energy; in the early universe “clouds” of hydrogen nuclei fused together under a high temperature and pressure to form stars; continued fusion formed the “light” elements (up to iron). Heavier elements were formed in supernovae under conditions of huge temperature and pressure

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11
Q

Absorption and emission spectra

A

Under certain conditions elements emit or absorb electromagnetic radiation in a characteristic way. Absorption spectra appear as black lines on a bright background, while emission spectra are the inverse of this

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12
Q

Balmer series

A

A diagram showing how outermost electrons can be excited to unstable higher levels, only to emit photons to get back to ground level

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13
Q

Star structure

A

The photosphere, the glowing surface of a star that emits visible light, is surrounded by atoms and ions that absorb light from the photosphere, producing absorption spectra. The corona, an area of high temperature surrounds the star and contains ions such as Mg 11+ and Fe 15+

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14
Q

Light emission

A

The outermost electrons of an atom start in a stable “ground state”, and when heat, light or energy is applied the molecules transition into a higher, unstable state. When the electron goes back to ground state it emits energy as a photon of light or electromagnetic radiation

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15
Q

Wave-particle duality

A

Light can be imagined with two models: as a wave, equation c = f ƛ; and as a particle, equation E = h f. The energy of the light is a function of it’s wavelength, E = c h / ƛ

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16
Q

Bohr’s Theory

A

Atomic spectra are caused by electrons in atoms moving between different energy levels (shells and sub-shells)

17
Q

Electron shells

A

Electrons are arranged in principal energy levels which contain overlapping sub shells

18
Q

Electron sub-shells

A

S-orbital contains one orbital with two electrons; P-orbital contains three orbitals with six electrons; D-orbital contains five orbitals with ten electrons

19
Q

Sub-shell order

A

1s2, 2s2, 2p6, 3s2, 3p6, 4s2, 3d10

20
Q

Electron configuration rules

A

The lowest energy sub-levels are occupied first (the Aufbau principle); single electrons fill empty orbitals before forming pairs (Hund’s rule); each orbital contains a maximum of two electrons (the Pauli exclusion principle)

21
Q

Dative covalent bonds

A

In a dative covalent bond, one atom contributes both electrons to the covalent bond. The bond line is replaced by an arrow, demonstrating where the electrons come from

22
Q

Electron Pair Repulsion theory

A

Areas of electron density repel each other as they are negatively charged, so they move as far apart as possible to reduce the repulsions