It seems that all too frequently we read another exciting announcement that an extrasolar planet has been detected, one that is in the “habitable zone” and would likely be able to host life. The announcement is usually accompanied by an artist’s conception of the planet with oceans, continents, and an atmosphere with clouds that appear decidedly Earth-like.
Figure 1: Estimated habitable zones in the solar system compared to Kepler-452 and Kepler-186. Image credit: NASA
The circumstellar habitable zone (HZ) was given a rigorous definition in a 1993 paperby geoscientist James Kasting (Pennsylvania State University) and his team. This definition was then updated in 2013.1 As defined, an HZ has an inner edge where atmospheric water breaks down and hydrogen escapes. This results in a runaway greenhouse effect. At the outer edge, CO2 condenses into clouds and accelerates cooling, resulting in all surface water freezing. For the solar system, the HZ model has an inner edge at 0.99 astronomical units (AU) and an outer edge at 1.70 AU.2 Earth is just barely inside the inner edge, and Mars is just inside the outer edge at 1.52 AU.
Although often overlooked, the definition of an HZ is extremely dependent on the composition of an exoplanet’s atmosphere. Kasting’s model assumed not only an Earth-like atmosphere, but also a carbon-silicate feedback cycle that requires a fine-tuned mix of oceans, continents, plate tectonics, and steady volcanic outgassing of CO2. One exoplanet researcher notes, “Without knowledge of the major molecules of an exoplanet’s atmosphere, we can only speculate whether it resides in the habitable zone for liquid water.… Declaring a freshly detected exoplanet to be in the ‘habitable zone’ amounts to little more than media spin if its atmospheric composition is unknown.”3
How the Definition Is Changing
Recent studies demonstrate how fragile a planet’s atmosphere can be when subjected to steady stellar radiation and occasional coronal mass ejections. Several Earth-size exoplanets around M dwarf stars have been found in the classically defined HZ. However, the close orbits of these exoplanets lead to tidal locking, which results in the atmospheres being stripped over time by a constantly blowing stellar wind.4 NASA’s MAVEN spacecraft orbiting Mars indicates that the lack of a protective magnetic field may have resulted in a similar stripping of the planet’s atmosphere. Even planets like Venus that retain a dense atmosphere lose their water unless they have a strong magnetic field.
But how has Earth maintained its magnetic shield for billions of years? Recent work done by a French team informs us that complex gravitational interactions between the earth and the moon are responsible for the earth’s long-lasting geodynamo and protective magnetic shield. The team writes (emphasis added):