2009 Annual Science Report

VPL at University of Washington Reporting  |  JUL 2008 – AUG 2009

Stellar Effects on Planetary Habitability

Project Summary

Habitable environments are most likely to exist in close proximity to a star, and hence a detailed and comprehensive understanding of the effect of the star on planetary habitability is crucial in the pursuit of an inhabited world. We model how stars with different masses, temperatures and flare activity affect the habitability of planets. We also address the effect that tides between a star and a planet have on planetary habitability, including the power to turn potentially habitable planets like Earth into extremely volcanically active bodies like Io.

4 Institutions
3 Teams
4 Publications
0 Field Sites
Field Sites

Project Progress

We studied the impact of a large flare from the M dwarf, AD Leonis (AD Leo), on the atmospheric chemistry of a hypothetical, Earth-like planet located within its habitable zone. The AD Leo flare of 1985 April 12 emitted a total energy of ~10^34 ergs. The simulations were performed using a 1-D photochemical model coupled to a 1-D radiative/convective model. Our results indicate that the ultraviolet radiation emitted during the flare does not produce a significant change in the ozone column depth or the UV flux reaching the surface of the planet, and so such flares may not present a direct hazard for life on the surface of an orbiting habitable planet. Given that AD Leo is one of the most magnetically active M dwarfs known, this conclusion should apply to planets around other M dwarfs with lower chromospheric activity (Walkowicz et al., 2009; Segura et al., 2009)

We have explored how tidal effects can alter the surface properties of planets. We considered the specific case of HD 40307 and showed which regions of observationally-permitted parameter space led to tidal heating rates larger than on Io on HD 40307 b. We also considered the range of tidal heating that is possible in the habitable zones of low-mass stars. We proposed that one may make a second cut on planetary habitability based in the level of tidal heating: The heat flux must be less than that on Io, and more than the minimum for plate tectonics (Barnes et al., 2009)

The blue region is the “classic” habitable zone derived from estimates of stellar flux and assuming an Earth-like atmosphere (see Selsis et al. 2007). Yellow regions represent regions in which tidal heating of a 10 Earth mass terrestrial planet is favorable for habitability, the left strip assumes an orbital eccentricity of 0.01, the right 0.5. Green represents the overlap of the two types of habitability.

We also explored the statistical probability of detrimental effects on habitability due to astrospheric collapse for stars of different mass (Smith & Scalo, 2009) An “astrosphere” is the plasma cocoon carved out of the interstellar medium by a stellar wind. In dense interstellar clouds, the resulting pressure can collapse the astrosphere, resulting in exposure of the habitable zone to enhanced amounts of cosmic ray flux, dust and gas. We find that ISM encounters resulting in astrosphere collapse are unlikely to occur for K and M stars, but could be as frequent at 1-10 every billion years for solar mass stars or larger.

  • PROJECT INVESTIGATORS:
  • PROJECT MEMBERS:
    Victoria Meadows
    Project Investigator

    John Armstrong
    Co-Investigator

    James Kasting
    Co-Investigator

    Thomas Quinn
    Co-Investigator

    John Scalo
    Co-Investigator

    Antigona Segura-Peralta
    Co-Investigator

    Rory Barnes
    Postdoc

    Mark Claire
    Postdoc

    Ravi Kopparapu
    Postdoc

    Sean Raymond
    Postdoc

    Lucianne Walkowicz
    Postdoc

    Kristina Mullins
    Undergraduate Student

  • RELATED OBJECTIVES:
    Objective 1.1
    Formation and evolution of habitable planets.

    Objective 1.2
    Indirect and direct astronomical observations of extrasolar habitable planets.

    Objective 2.1
    Mars exploration.

    Objective 2.2
    Outer Solar System exploration

    Objective 4.1
    Earth's early biosphere.

    Objective 4.3
    Effects of extraterrestrial events upon the biosphere

    Objective 5.3
    Biochemical adaptation to extreme environments

    Objective 6.1
    Effects of environmental changes on microbial ecosystems

    Objective 7.2
    Biosignatures to be sought in nearby planetary systems