This video is an introduction to Bohr's planetary model and emission spectra, explaining various aspects of Bohr's model, including orbits, discrete energy levels, electrons changing energy and the resulting emission of light, ground state versus excited state electrons, the electromagnetic spectrum and visible light, emission spectra, in particular of hydrogen, and the connection of Bohr's model to the atomic emission spectra of hydrogen in particular and of other elements as well.
Check out other CC Academy videos on this channel:
Stoichiometry Tutorial, step by step
Types of Chemical Reactions: How to classify five basic reaction types
Solution Stoichiometry
Orbitals the Basics: Atomic Orbitals Tutorial
Hybrid Orbitals Explained
Polar Molecules Tutorial: How to determine polarity in a molecule
Metallic Bonding and Metallic Properties Explained
Covalent Bonding Tutorial
Ionic Bonds, Ionic Compounds: What is an ionic bond and how do ionic compounds form
Electronegativity and bond character (bond type): non-polar covalent, polar, ionic
Metric Unit Prefix Conversions: How to Convert Metric System Prefixes
Metric unit conversions shortcut: fast, easy how-to with examples
Mole Conversions Tutorial: how to convert mole - mass, mole - particle, mass - particle problems
Frequency, Wavelength, and the Speed of Light
The Bohr Model of the Atom and Atomic Emission Spectra
What is Heat: A brief introduction at the particle level
Rutherford's Gold Foil Experiment
Unit Conversion Using Dimensional Analysis Tutorial
What is Fire: Combustion Reaction Tutorial
Quantum Numbers Tutorial
Electron Configurations Tutorial and How to Derive Electron Configurations from the Periodic Table
Concentration and Molarity Explained
Heating Curves Tutorial
Naming Ionic Compounds
Limiting Reactant Tutorial
PV=nRT The Ideal Gas Law: What is it, What is R, Four practice problems solved including molar mass
Gas density and PV=nRT, the ideal gas law
Surface Tension - What is it, how does it form, what properties does it impart
The Bohr Model, Wikipedia, 2020:
In atomic physics, the Bohr model or Rutherford-Bohr model, presented by Niels Bohr and Ernest Rutherford in 1913, is a system consisting of a small, dense nucleus surrounded by orbiting electrons-similar to the structure of the Solar System, but with attraction provided by electrostatic forces in place of gravity. After the cubical model (1902), the plum pudding model (1904), the Saturnian model (1904), and the Rutherford model (1911) came the Rutherford-Bohr model or just Bohr model for short (1913). The improvement over the 1911 Rutherford model mainly concerned the new quantum physical interpretation.
The model's key success lay in explaining the Rydberg formula for the spectral emission lines of atomic hydrogen. While the Rydberg formula had been known experimentally, it did not gain a theoretical underpinning until the Bohr model was introduced. Not only did the Bohr model explain the reasons for the structure of the Rydberg formula, it also provided a justification for the fundamental physical constants that make up the formula's empirical results.
The Bohr model is a relatively primitive model of the hydrogen atom, compared to the valence shell atom model. As a theory, it can be derived as a first-order approximation of the hydrogen atom using the broader and much more accurate quantum mechanics and thus may be considered to be an obsolete scientific theory. However, because of its simplicity, and its correct results for selected systems (see below for application), the Bohr model is still commonly taught to introduce students to quantum mechanics or energy level diagrams before moving on to the more accurate, but more complex, valence shell atom. A related model was originally proposed by Arthur Erich Haas in 1910 but was rejected. The quantum theory of the period between Planck's discovery of the quantum (1900) and the advent of a mature quantum mechanics (1925) is often referred to as the old quantum theory.
In the early 20th century, experiments by Ernest Rutherford established that atoms consisted of a diffuse cloud of negatively charged electrons surrounding a small, dense, positively charged nucleus.[2] Given this experimental data, Rutherford naturally considered a planetary model of the atom, the Rutherford model of 1911. This had electrons orbiting a solar nucleus, but involved a technical difficulty: the laws of classical mechanics (i.e. the Larmor formula) predict that the electron will release electromagnetic radiation while orbiting a nucleus. Because the electron would lose energy, it would rapidly spiral inwards, collapsing into the nucleus on a timescale of around 16 picoseconds. This atom model is disastrous because it predicts that all atoms are unstable.[4] Also, as the electron spirals inward, the emission would rapidly increase in frequency as the orbit got smaller and faster. This would cause a continuous stream of electromagnetic radiation.