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Escape Velocity01:26

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The escape velocity of an object is defined as the minimum initial velocity that it requires to escape the surface of another object to which it is gravitationally bound and never to return. For example, what would be the minimum velocity at which a satellite should be launched from the Earth's surface such that it just escapes the Earth's gravitational field?
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The gravitational acceleration of an object near the Earth's surface is called the acceleration due to gravity. It can be measured by conducting simple experiments on Earth. However, such an experiment is impossible to conduct on the surface of other planets.
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No object with a finite mass can travel faster than the speed of light in a vacuum. This fact has an interesting consequence in the domain of extremely high gravitational fields.
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To escape the Earth's gravity, an object near the top of the atmosphere at an altitude of 100 km must travel away from Earth at 11.1 km/s. This speed is called the escape velocity. The temperature at which gas molecules attain the rms speed, which is equal to the escape velocity, can be estimated by using the equation for the average kinetic energy of the gas molecules. According to the kinetic theory of gas, the average kinetic energy of the gas molecules is proportional to its...
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Thermal escape from extrasolar giant planets.

Tommi T Koskinen1, Panayotis Lavvas, Matthew J Harris

  • 1Lunar and Planetary Laboratory, University of Arizona, , 1629 E. University Boulevard, Tucson, AZ 85721-0092, USA.

Philosophical Transactions. Series A, Mathematical, Physical, and Engineering Sciences
|March 26, 2014
PubMed
Summary
This summary is machine-generated.

Close-in giant planets have hot, escaping atmospheres, but not all are the same. This study reveals two distinct thermal escape regimes, impacting mass loss and detectability.

Keywords:
atmospheric physicsextrasolar planetshydrodynamics

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Area of Science:

  • Exoplanetary Science
  • Atmospheric Physics
  • Stellar Astrophysics

Background:

  • Hot atomic hydrogen and heavy elements detected at high altitudes of close-in giant planets suggest escaping atmospheres.
  • These atmospheric escape characteristics are not universal across all close-in giant planets.

Purpose of the Study:

  • To investigate how photochemistry and radiative transfer, driven by stellar UV radiation, influence thermal escape and mass loss rates.
  • To explore these processes across giant planets with varying characteristics and irradiation levels.

Main Methods:

  • Simulating atmospheric escape under different irradiation levels.
  • Analyzing the interplay between photochemistry and radiative transfer.

Main Results:

  • Confirmation of two distinct regimes of thermal atmospheric escape from extrasolar giant planets.
  • Identification of a relatively sharp transition between these escape regimes.

Conclusions:

  • The findings have significant implications for understanding thermal mass loss rates in extrasolar giant planets.
  • Discusses the detectability of upper atmospheres in currently known extrasolar giant planets based on these escape mechanisms.