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Related Concept Videos

Atomic Spectroscopy: Effects of Temperature01:27

Atomic Spectroscopy: Effects of Temperature

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Atomization, converting samples into gas-phase atoms and ions, is essential for atomic spectroscopy. The flame temperature required for atomization affects the efficiency of the atomic spectroscopic methods by increasing the atomization efficiency and the relative population of the excited and ground states.
At thermal equilibrium, the relative populations of excited and ground state atoms can be estimated using the Maxwell–Boltzmann distribution. For example, an increase in temperature...
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Fermi Level Dynamics01:12

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The vacuum level denotes the energy threshold required for an electron to escape from a material surface. It is usually positioned above the conduction band of a semiconductor and acts as a benchmark for comparing electron energies within various materials.
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The number of independent ways a gas molecule can move along straight line, rotate, and vibrate is called its degrees of freedom. Supposing d represents the number of degrees of freedom of an ideal gas, the molar heat capacity at constant volume of an ideal gas in terms of d is
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Heat Capacities of an Ideal Gas II01:23

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For a system that undergoes a thermodynamic process at a constant volume condition, the heat absorbed is used only to increase the system's internal energy and not for doing any kind of work. While for a system undergoing a thermodynamic process under a constant pressure condition, the amount of heat absorbed is used not only for increasing the internal energy (as a function of temperature) but also for doing some work. The molar heat capacity is the amount of heat required to increase the...
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Atomic Nuclei: Nuclear Spin State Population Distribution01:14

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Near absolute zero temperatures, in the presence of a magnetic field, the majority of nuclei prefer the lower energy spin-up state to the higher energy spin-down state. As temperatures increase, the energy from thermal collisions distributes the spins more equally between the two states. The Boltzmann distribution equation gives the ratio of the number of spins predicted in the spin −½ (N−) and spin +½ (N+) states.
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Methods of Ex Situ and In Situ Investigations of Structural Transformations: The Case of Crystallization of Metallic Glasses
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Nucleation at Finite Temperature: A Gauge-Invariant Perturbative Framework.

Johan Löfgren1, Michael J Ramsey-Musolf2,3,4,5, Philipp Schicho6

  • 1Department of Physics and Astronomy, Uppsala University, Box 516, SE-751 20 Uppsala, Sweden.

Physical Review Letters
|July 7, 2023
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We developed a gauge-invariant method to calculate bubble nucleation rates in high-temperature theories. This framework aids in understanding electroweak baryogenesis and cosmic phase transitions for gravitational wave signals.

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Area of Science:

  • Theoretical Physics
  • Cosmology
  • Particle Physics

Background:

  • Radiative symmetry breaking at high temperatures is crucial for early universe cosmology.
  • Calculating bubble nucleation rates is essential for understanding phase transitions.
  • Existing methods often lack gauge invariance, complicating theoretical predictions.

Purpose of the Study:

  • To present a novel gauge-invariant framework for computing bubble nucleation rates.
  • To establish a practical perturbative method for high-temperature expansions.
  • To enable accurate predictions for cosmological phenomena.

Main Methods:

  • Developed a gauge-invariant perturbative framework.
  • Applied consistent power counting in the high-temperature expansion.
  • Focused on leading-order nucleation rate calculations.

Main Results:

  • Established a practical, gauge-invariant method for calculating nucleation rates.
  • The framework is based on a consistent high-temperature expansion.
  • Provides a reliable tool for theoretical computations.

Conclusions:

  • The presented framework offers a significant advancement in calculating bubble nucleation.
  • It has direct applications in electroweak baryogenesis and gravitational wave signal predictions.
  • Facilitates more accurate modeling of cosmic phase transitions.