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Related Concept Videos

Heating and Cooling Curves02:44

Heating and Cooling Curves

When a substance—isolated from its environment—is subjected to heat changes, corresponding changes in temperature and phase of the substance is observed; this is graphically represented by heating and cooling curves.
For instance, the addition of heat raises the temperature of a solid; the amount of heat absorbed depends on the heat capacity of the solid (q = mcsolidΔT). According to thermochemistry, the relation between the amount of heat absorbed or released by a substance, q, and its...
Hess's Law03:40

Hess's Law

There are two ways to determine the amount of heat involved in a chemical change: measure it experimentally, or calculate it from other experimentally determined enthalpy changes. Some reactions are difficult, if not impossible, to investigate and make accurate measurements for experimentally. And even when a reaction is not hard to perform or measure, it is convenient to be able to determine the heat involved in a reaction without having to perform an experiment.
¹³C NMR: ¹H–¹³C Decoupling01:04

¹³C NMR: ¹H–¹³C Decoupling

The probability of having two carbon-13 atoms next to each other is negligible because of the low natural abundance of carbon-13. Consequently, peak splitting due to carbon-carbon spin-spin coupling is not observed in spectra. However, protons up to three sigma bonds away split the carbon signal according to the n+1 rule, resulting in complicated spectra.
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Atomic Spectroscopy: Effects of Temperature01:27

Atomic Spectroscopy: Effects of Temperature

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.
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Emission Spectra02:39

Emission Spectra

When solids, liquids, or condensed gases are heated sufficiently, they radiate some of the excess energy as light. Photons produced in this manner have a range of energies, and thereby produce a continuous spectrum in which an unbroken series of wavelengths is present.
Atomic Nuclei: Nuclear Spin State Population Distribution01:14

Atomic Nuclei: Nuclear Spin State Population Distribution

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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Related Experiment Video

Updated: May 9, 2026

Cooling an Optically Trapped Ultracold Fermi Gas by Periodical Driving
11:21

Cooling an Optically Trapped Ultracold Fermi Gas by Periodical Driving

Published on: March 30, 2017

Cooling by H3(+) emission.

Steve Miller1, Tom Stallard, Jonathan Tennyson

  • 1Department of Physics and Astronomy, University College London , London WC1E 6BT, U.K.

The Journal of Physical Chemistry. A
|July 18, 2013
PubMed
Summary
This summary is machine-generated.

New calculations show that the H3(+) ion significantly increases radiative cooling in exoplanetary atmospheres at high temperatures. Nonthermal effects are also crucial for understanding energy balance in these environments.

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Related Experiment Videos

Last Updated: May 9, 2026

Cooling an Optically Trapped Ultracold Fermi Gas by Periodical Driving
11:21

Cooling an Optically Trapped Ultracold Fermi Gas by Periodical Driving

Published on: March 30, 2017

High-resolution Thermal Micro-imaging Using Europium Chelate Luminescent Coatings
09:01

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Angle-resolved Photoemission Spectroscopy At Ultra-low Temperatures
08:53

Angle-resolved Photoemission Spectroscopy At Ultra-low Temperatures

Published on: October 9, 2012

Area of Science:

  • Astrophysics
  • Planetary Science
  • Physical Chemistry

Background:

  • The energy balance in exoplanetary atmospheres is influenced by molecular ion emissions.
  • The H3(+) molecular ion plays a role in astrophysical energy transfer processes.

Purpose of the Study:

  • To calculate a new cooling function for H3(+) emission.
  • To improve understanding of energy balance in exoplanetary atmospheres.

Main Methods:

  • Refitted partition functions for H3(+).
  • Recalculated total energy emitted by H3(+).
  • Consideration of nonthermal effects and departures from equilibrium.

Main Results:

  • A new cooling function for H3(+) was developed.
  • Significantly increased cooling observed at higher temperatures (e.g., gas giant atmospheres).
  • Nonthermal effects were found to be important.

Conclusions:

  • The new H3(+) cooling function enhances understanding of high-temperature exoplanetary atmospheres.
  • Nonthermal processes must be included for accurate energy balance calculations.
  • A web-based code is available for radiative cooling calculations in H2/H3(+) mixtures.