Atomic Structure

Views:
 
Category: Entertainment
     
 

Presentation Description

No description available.

Comments

By: kevin_patel (18 month(s) ago)

download unavailable what is the use of it if you are not allowing others to see your creativity

By: neerajguglani12 (24 month(s) ago)

Nice Atomic structure

Presentation Transcript

Slide 1: 

Atomic Structure

Slide 2: 

All waves have a characteristic wavelength, l, and amplitude, A. Frequency, n, of a wave is the number of cycles which pass a point in one second. Speed of a wave, c, is given by its frequency multiplied by its wavelength: For light, speed = c = 3.00x108 m s-1 . A Brief History of Time The Wave Nature of Light

Slide 3: 

The Wave Nature of Light

Slide 4: 

The Wave Nature of Light

Slide 5: 

The Wave Nature of Light

Slide 6: 

Planck: energy can only be absorbed or released from atoms in certain amounts called quanta. The relationship between energy and frequency is where h is Planck’s constant ( 6.626  10-34 J s ) . Quantized Energy and Photons

Slide 7: 

The Photoelectric Effect and Photons Einstein assumed that light traveled in energy packets called photons. The energy of one photon is: Quantized Energy and Photons

Slide 8: 

Nature of Waves: Quantized Energy and Photons

Slide 9: 

Line Spectra Radiation composed of only one wavelength is called monochromatic. Radiation that spans a whole array of different wavelengths is called continuous. White light can be separated into a continuous spectrum of colors. Note that there are no dark spots on the continuous spectrum that would correspond to different lines. Line Spectra and the Bohr Model

Slide 11: 

Bohr Model Colors from excited gases arise because electrons move between energy states in the atom. (Electronic Transition) Line Spectra and the Bohr Model

Slide 12: 

Bohr Model Since the energy states are quantized, the light emitted from excited atoms must be quantized and appear as line spectra. After lots of math, Bohr showed that where n is the principal quantum number (i.e., n = 1, 2, 3, … and nothing else). Line Spectra and the Bohr Model

Slide 13: 

Bohr Model We can show that When ni > nf, energy is emitted. When nf > ni, energy is absorbed Line Spectra and the Bohr Model

Slide 14: 

Bohr Model Line Spectra and the Bohr Model CyberChem (Fireworks) video Mathcad (Balmer Series)

Slide 15: 

Line Spectra and the Bohr Model: Balmer Series Calculations

Slide 17: 

Limitations of the Bohr Model Can only explain the line spectrum of hydrogen adequately. Can only work for (at least) one electron atoms. Cannot explain multi-lines with each color. Electrons are not completely described as small particles. Electrons can have both wave and particle properties. Line Spectra and the Bohr Model

Slide 18: 

Knowing that light has a particle nature, it seems reasonable to ask if matter has a wave nature. Using Einstein’s and Planck’s equations, de Broglie showed: The momentum, mv, is a particle property, whereas  is a wave property. de Broglie summarized the concepts of waves and particles, with noticeable effects if the objects are small. The Wave Behavior of Matter

Slide 19: 

The Uncertainty Principle Heisenberg’s Uncertainty Principle: on the mass scale of atomic particles, we cannot determine exactly the position, direction of motion, and speed simultaneously. For electrons: we cannot determine their momentum and position simultaneously. If Dx is the uncertainty in position and Dmv is the uncertainty in momentum, then The Wave Behavior of Matter

Energy and Matter : 

Energy and Matter E = m c2

Slide 21: 

Schrödinger proposed an equation that contains both wave and particle terms. Solving the equation leads to wave functions. The wave function gives the shape of the electronic orbital. [“Shape” really refers to density of electronic charges.] The square of the wave function, gives the probability of finding the electron ( electron density ). Quantum Mechanics and Atomic Orbitals

Slide 22: 

Quantum Mechanics and Atomic Orbitals Solving Schrodinger’s Equation gives rise to ‘Orbitals.’ These orbitals provide the electron density distributed about the nucleus. Orbitals are described by quantum numbers.

Slide 23: 

Orbitals and Quantum Numbers Schrödinger’s equation requires 3 quantum numbers: Principal Quantum Number, n. This is the same as Bohr’s n. As n becomes larger, the atom becomes larger and the electron is further from the nucleus. ( n = 1 , 2 , 3 , 4 , …. ) Azimuthal Quantum Number, . This quantum number depends on the value of n. The values of  begin at 0 and increase to (n - 1). We usually use letters for  (s, p, d and f for  = 0, 1, 2, and 3). Usually we refer to the s, p, d and f-orbitals. Magnetic Quantum Number, m. This quantum number depends on  . The magnetic quantum number has integral values between -  and +  . Magnetic quantum numbers give the 3D orientation of each orbital. Quantum Mechanics and Atomic Orbitals

Quantum Numbers of Wavefuntions : 

Quantum Numbers of Wavefuntions

Quantum Mechanics and Atomic Orbitals : 

Quantum Mechanics and Atomic Orbitals

Slide 26: 

Orbitals and Quantum Numbers Quantum Mechanics and Atomic Orbitals

Slide 27: 

The s-Orbitals Representations of Orbitals

Slide 28: 

The p-Orbitals Representations of Orbitals

Slide 29: 

d-orbitals

Slide 30: 

Many-Electron Atoms Orbitals and Their Energies Orbitals CD

Slide 31: 

Electron Spin and the Pauli Exclusion Principle Many-Electron Atoms

Slide 32: 

Electron Spin and the Pauli Exclusion Principle Since electron spin is quantized, we define ms = spin quantum number =  ½. Pauli’s Exclusions Principle: no two electrons can have the same set of 4 quantum numbers. Therefore, two electrons in the same orbital must have opposite spins. Many-Electron Atoms

Slide 33: 

Figure 6.27 Figure 6.27 Orbitals CD

Slide 34: 

Figure 6.28 Orbitals CD

Slide 35: 

Many-Electron Atoms Orbitals and Their Energies Orbitals CD

Slide 36: 

Electron Configurations

Slide 37: 

Metals, Nonmetals, and Metalloids Metals Figure 7.14

Slide 38: 

Two Major Factors: principal quantum number, n, and the effective nuclear charge, Zeff. Periodic Trends

Slide 39: 

Figure 7.5: Radius video Clip

Slide 40: 

Figure 7.6

Slide 41: 

Figure 7.10 IE clip

Slide 42: 

Figure 7.9

Slide 43: 

Electron Affinities Electron affinity is the opposite of ionization energy. Electron affinity: the energy change when a gaseous atom gains an electron to form a gaseous ion: Cl(g) + e-  Cl-(g) Electron affinity can either be exothermic (as the above example) or endothermic: Ar(g) + e-  Ar-(g)

Slide 44: 

Figure 7.11: Electron Affinities

Slide 45: 

Group Trends for the Active Metals Group 1A: The Alkali Metals

Slide 46: 

Group Trends for the Active Metals Group 2A: The Alkaline Earth Metals

Slide 47: 

Group Trends for Selected Nonmetals Group 6A: The Oxygen Group

Slide 48: 

Group Trends for Selected Nonmetals Group 7A: The Halogens

Slide 49: 

Group Trends for the Active Metals Group 1A: The Alkali Metals Alkali metals are all soft. Chemistry dominated by the loss of their single s electron: M  M+ + e- Reactivity increases as we move down the group. Alkali metals react with water to form MOH and hydrogen gas: 2M(s) + 2H2O(l)  2MOH(aq) + H2(g)

Slide 50: 

Group Trends for the Active Metals Group 2A: The Alkaline Earth Metals Alkaline earth metals are harder and more dense than the alkali metals. The chemistry is dominated by the loss of two s electrons: M  M2+ + 2e-. Mg(s) + Cl2(g)  MgCl2(s) 2Mg(s) + O2(g)  2MgO(s) Be does not react with water. Mg will only react with steam. Ca onwards: Ca(s) + 2H2O(l)  Ca(OH)2(aq) + H2(g)

Slide 51: 

Atomic Structure