Physics:Quantum Spectral lines and series - Revision history

Maintenance script: Add historical name link to William Hyde Wollaston

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	== Historical names ==		== Historical names ==
			* [[Biography:William Hyde Wollaston\|William Hyde Wollaston]] observed dark lines in the solar spectrum in 1802, before Fraunhofer mapped them systematically. These observations became part of the experimental history of spectroscopy and quantum atomic transitions.
	* [[Biography:Joseph von Fraunhofer\|Joseph von Fraunhofer]] mapped dark absorption lines in the solar spectrum. Fraunhofer lines became a key observational background for spectroscopy and the later quantum explanation of atomic transitions.		* [[Biography:Joseph von Fraunhofer\|Joseph von Fraunhofer]] mapped dark absorption lines in the solar spectrum. Fraunhofer lines became a key observational background for spectroscopy and the later quantum explanation of atomic transitions.

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	==References==		==References==
	{{reflist\|3}}		{{reflist\|3}}
			== Historical names ==
			* [[Biography:Joseph von Fraunhofer\|Joseph von Fraunhofer]] mapped dark absorption lines in the solar spectrum. Fraunhofer lines became a key observational background for spectroscopy and the later quantum explanation of atomic transitions.

	{{Author\|Harold Foppele}}		{{Author\|Harold Foppele}}

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	{{Short description\|Quantum Collection topic on Quantum Spectral lines and series}}		{{Short description\|Quantum Collection topic on Quantum Spectral lines and series}}

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	{{Quantum article nav\|previous=Physics:Quantum Stark effect\|previous label=Stark effect\|next=Physics:Quantum Selection rules\|next label=Selection rules}}		{{Quantum article nav\|previous=Physics:Quantum Stark effect\|previous label=Stark effect\|next=Physics:Quantum Selection rules\|next label=Selection rules}}

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	{{Short description\|Quantum Collection topic on Quantum Spectral lines and series}}~~Book I~~		{{Short description\|Quantum Collection topic on Quantum Spectral lines and series}}

	{{Quantum book backlink\|Atomic and spectroscopy}}		{{Quantum book backlink\|Atomic and spectroscopy}}

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	'''Spectral lines and series''' ~~is a Book I topic in the Quantum Collection. Spectral~~ lines are discrete wavelengths of light emitted or absorbed by atoms and molecules, arising from transitions between quantized energy levels, and they provided some of the earliest direct evidence for quantum theory. In quantum mechanics, electrons in atoms occupy discrete energy eigenstates. When an electron transitions between two states, a photon is emitted or absorbed with energy given by: * \nu is the frequency of the radiation * E_i, E_f are the initial and final energy levels This leads to sharply defined spectral lines rather than a continuous spectrum. The hydrogen atom provides the simplest and most important example of spectral line structure. Its energy levels are given by: Transitions between these levels produce series of spectral lines described by the Rydberg formula: This relation accurately predicts observed hydrogen spectral lines.		'''Spectral lines and series''' spectral lines are discrete wavelengths of light emitted or absorbed by atoms and molecules, arising from transitions between quantized energy levels, and they provided some of the earliest direct evidence for quantum theory. In quantum mechanics, electrons in atoms occupy discrete energy eigenstates. The hydrogen atom provides the simplest and most important example of spectral line structure. Its energy levels are given by: Transitions between these levels produce series of spectral lines described by the Rydberg formula: This relation accurately predicts observed hydrogen spectral lines. When an electron transitions between two states, a photon is emitted or absorbed with energy given by: This leads to sharply defined spectral lines rather than a continuous spectrum.
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Maintenance script: Clean Book I red links, intro, and image slots

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	'''Spectral lines''' are discrete wavelengths of light emitted or absorbed by atoms and molecules, arising from transitions between quantized energy levels, and they provided some of the earliest direct evidence for quantum theory.~~<ref>[https~~:~~//www~~.~~britannica~~.~~com/science/~~spectral~~-line Spectral line – Britannica]</ref>~~		'''Spectral lines and series''' is a Book I topic in the Quantum Collection. Spectral lines are discrete wavelengths of light emitted or absorbed by atoms and molecules, arising from transitions between quantized energy levels, and they provided some of the earliest direct evidence for quantum theory. In quantum mechanics, electrons in atoms occupy discrete energy eigenstates. When an electron transitions between two states, a photon is emitted or absorbed with energy given by: * \nu is the frequency of the radiation * E_i, E_f are the initial and final energy levels This leads to sharply defined spectral lines rather than a continuous spectrum. The hydrogen atom provides the simplest and most important example of spectral line structure. Its energy levels are given by: Transitions between these levels produce series of spectral lines described by the Rydberg formula: This relation accurately predicts observed hydrogen spectral lines.
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Maintenance script: Normalize Book I Quantum page structure

2026-05-19T22:48:59Z

Normalize Book I Quantum page structure

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	{{Author\|Harold Foppele}}		{{Author\|Harold Foppele}}

	{{Sourceattribution\|Quantum Spectral lines and series\|1}}		{{Sourceattribution\|Physics:Quantum Spectral lines and series\|1}}

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	{{Quantum article nav\|previous=Physics:Quantum Stark effect\|previous label=Stark effect\|next=Physics:Quantum Selection rules\|next label=Selection rules}}		{{Quantum article nav\|previous=Physics:Quantum Stark effect\|previous label=Stark effect\|next=Physics:Quantum Selection rules\|next label=Selection rules}}