Encyclopedia of Astrobiology

Living Edition
| Editors: Muriel Gargaud, William M. Irvine, Ricardo Amils, Henderson James Cleaves, Daniele Pinti, José Cernicharo Quintanilla, Michel Viso

Hot Neptunes

  • David W. Latham
  • Nader Haghighipour
Living reference work entry
DOI: https://doi.org/10.1007/978-3-642-27833-4_739-2


Hot Neptune is a designation that is often assigned to planets with masses or radii similar to those of Neptune in short-period orbits around their parent stars. The characteristics of Hot Neptunes are not well defined, but the orbital period must be short enough (say less than 10 or 20 days) for the planet to be truly “hot,” and the mass must be substantially smaller than that of Saturn (say less than a tenth of a Jupiter mass). It is commonly accepted that Hot Neptunes originally form much farther from their host stars and then migrate inward either by interaction with the circumstellar disk from which they formed or by gravitational interactions with other planets in the system.

See Also


Orbital Period Bioorganic Chemistry Gravitational Interaction Giant Planet Circumstellar Disk 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

Copyright information

© Springer-Verlag Berlin Heidelberg 2014

Authors and Affiliations

  1. 1.Harvard-Smithsonian Center for AstrophysicsCambridgeUSA
  2. 2.Institute for Astronomy, University of Hawaii, University of Hawaii-ManoaHonoluluUSA