Helium planet

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Helium planets would have a white or grey hue.
(artist concept).

A helium planet is a planet with a helium-dominated atmosphere. This is in contrast to ordinary gas giants such as Jupiter and Saturn, whose atmospheres consist primarily of hydrogen, with helium as a secondary component only. Helium planets might form in a variety of ways.

A helium planet may form via mass loss from a low-mass white dwarf depleted of hydrogen. Such a white dwarf can form from a star where all the hydrogen has been processed to helium or other heavier elements by nuclear fusion. Mass-loss from the white dwarf will transform it to a giant planet over time, and this planet will automatically be depleted of hydrogen.[clarification needed][1]

A helium planet might also form via hydrogen evaporation from a gaseous planet orbiting close to a star. The star will drive off lighter gases more effectively through evaporation than heavier gasses, and over time deplete the hydrogen, leaving a greater proportion of helium behind.[2]

Evaporated white dwarf[edit]

Origins[edit]

One scenario involves an AM CVn type of symbiotic binary star composed of two helium core white dwarfs surrounded by a circumbinary helium accretion disk formed during mass transfer from the less massive to the more massive white dwarf. After it loses most of its mass, the less massive white dwarf may approach planetary mass.[1]

Characteristics[edit]

Helium planets are predicted to have roughly the same diameter as hydrogen–helium planets of the same mass.[citation needed]

Evaporated hot Neptunes[edit]

Formation of a helium planet from a hot giant planet, possibly like Gliese 436 b.

Origins[edit]

A scenario for forming helium planets from regular giant planets, involves an ice giant in an orbit so close to its host star, that the hydrogen effectively boils out of the atmosphere, evaporating from and escaping the gravitational hold of the planet. The planets atmosphere will experience a large energy input and as lightweight gases are more readily evaporated than heavier gases, the helium proportion will steadily rise in the remaining atmosphere. Such a process will take some time to stabilize and completely drive out all the hydrogen, perhaps in the order of 10 billion years, depending on the precise physical conditions and the nature of the planet and the star. Hot Neptunes are candidates for such a scenario.

The loss of hydrogen also leads to a depletion of methane in the atmosphere. On ice giants, methane naturally forms a cycle of melting, evaporation, breakdown and subsequent recombination and condensation. But as hydrogen gets depleted, a fraction of the carbon atoms will not be able to recombine with free hydrogen in the atmosphere and over time this will lead to an overall loss of methane. With time, the methane in the atmospheres of hot ice giants, will also get depleted.[2]

Characteristics[edit]

These planets are expected to be distinguishable from regular hydrogen-dominated planets by strong evidence of carbon monoxide and carbon dioxide in the atmosphere. Due to hydrogen-depletion, the expected methane in the atmosphere cannot form as there is no hydrogen for the carbon to combine with, so carbon combines with oxygen instead, leading to CO and CO2. Due to the atmospheric composition, they are expected to be white or grey in appearance.[2] Such a signature can be found in GJ 436b, which has a predominance of carbon monoxide.[2]

See also[edit]

References[edit]

  1. ^ a b Seager, S.; M. Kuchner; C. Hier-Majumder; B. Militzer (2007). "Mass-Radius Relationships for Solid Exoplanets". ApJ 669: 1279. arXiv:0707.2895. Bibcode:2007ApJ...669.1279S. doi:10.1086/521346. 
  2. ^ a b c d "Helium-Shrouded Planets May Be Common in Our Galaxy". SpaceDaily. 16 June 2015. Retrieved 3 August 2015. 

External links[edit]