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Related Concept Videos

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The motion of molecules in a gas is random in magnitude and direction for individual molecules, but a gas of many molecules has a predictable distribution of molecular speeds. This predictable distribution of molecular speeds is known as the Maxwell-Boltzmann distribution. The distribution of molecular speeds in liquids is comparable to that of gases but not identical and can help to understand the phenomenon of the boiling and vapor pressure of a liquid. Consider that a molecule requires a...
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Atomic Emission Spectroscopy: Overview01:20

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AES is a powerful analytical technique, especially effective when used with plasma sources, producing abundant spectra in characteristic emission lines. The Inductively Coupled Plasma (ICP), in particular, yields superior quantitative analytical data due to its high stability, low noise, low background, and minimal interferences under optimal experimental conditions. However, newer air-operated microwave sources are emerging as promising alternatives that could be more cost-effective than...
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Although gaseous molecules travel at tremendous speeds (hundreds of meters per second), they collide with other gaseous molecules and travel in many different directions before reaching the desired target. At room temperature, a gaseous molecule will experience billions of collisions per second. The mean free path is the average distance a molecule travels between collisions. The mean free path increases with decreasing pressure; in general, the mean free path for a gaseous molecule will be...
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Outflows from the youngest stars are mostly molecular.

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Young stars expel matter via powerful jets. New James Webb Space Telescope observations reveal these jets are primarily composed of hot molecules, not atoms or ions, explaining previously observed

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Area of Science:

  • * Astrophysics
  • * Star Formation
  • * Planetary Science

Background:

  • * Star and planet formation involves both matter accretion and expulsion via supersonic jets.
  • * Young protostars exhibit the most powerful jets, but are obscured by dust, limiting observations.
  • * The hot, atomic, ionized, and molecular constituents forming the jet's backbone remain largely unobserved.

Purpose of the Study:

  • * To investigate the composition of young protostellar jets, particularly their hot constituents.
  • * To explain the origin of the 'green fuzzies' observed in protostellar outflows.
  • * To probe the earliest stages of jet evolution using infrared observations.

Main Methods:

  • * Near-infrared observations using the James Webb Space Telescope (JWST).
  • * Targeted observation of Herbig-Haro 211, an outflow from a young protostar.
  • * Analysis of emission from hot molecules, atomic, and ionized gases.

Main Results:

  • * Copious emission from hot molecules detected in the Herbig-Haro 211 outflow.
  • * The 'green fuzzies' are explained as emission from these hot molecules.
  • * The jet spine is found to be almost purely molecular, with minimal atomic or ionized emission.
  • * The outflow exhibits slower propagation compared to more evolved jets.

Conclusions:

  • * The backbone of young protostellar jets is predominantly molecular.
  • * JWST's infrared capabilities are crucial for observing obscured, hot components of protostellar outflows.
  • * This study provides new insights into the early stages of jet formation and evolution.