title: Coronal mass ejection (CME) activity of low mass M stars as an important factor for the habitability of terrestrial exoplanets. I. CME impact on expected magnetospheres of Earth-like exoplanets in close-in habitable zones.
abstract: Low mass M- and K-type stars are much more numerous in the solar neighborhood than solar-like G-type stars. Therefore, some of them may appear as interesting candidates for the target star lists of terrestrial exoplanet (i.e., planets with mass, radius, and internal parameters identical to Earth) search programs like Darwin (ESA) or the Terrestrial Planet Finder Coronagraph/Inferometer (NASA). The higher level of stellar activity of low mass M stars, as compared to solar-like G stars, as well as the closer orbital distances of their habitable zones (HZs), means that terrestrial-type exoplanets within HZs of these stars are more influenced by stellar activity than one would expect for a planet in an HZ of a solar-like star. Here we examine the influences of stellar coronal mass ejection (CME) activity on planetary environments and the role CMEs may play in the definition of habitability criterion for the terrestrial type exoplanets near M stars. We pay attention to the fact that exoplanets within HZs that are in close proximity to low mass M stars may become tidally locked, which, in turn, can result in relatively weak intrinsic planetary magnetic moments. Taking into account existing observational data and models that involve the Sun and related hypothetical parameters of extrasolar CMEs (density, velocity, size, and occurrence rate), we show that Earth-like exoplanets within close-in HZs should experience a continuous CME exposure over long periods of time. This fact, together with small magnetic moments of tidally locked exoplanets, may result in little or no magnetospheric protection of planetary atmospheres from a dense flow of CME plasma. Magnetospheric standoff distances of weakly magnetized Earth-like exoplanets at orbital distances <or=0.1 AU can be shrunk, under the action of CMEs, to altitudes of about 1,000 km above the planetary surface. Such compressed magnetospheres may have crucial consequences for atmospheric erosion processes.
authors.affiliation: Space Research Institute, Austrian Academy of Sciences, Graz, Austria. maxim.khodachenko@oeaw.ac.at
authors.forename: Maxim L
authors.initials: ML
authors.lastname: Khodachenko
authors.forename: Ignasi
authors.initials: I
authors.lastname: Ribas
authors.forename: Helmut
authors.initials: H
authors.lastname: Lammer
authors.forename: Jean-Mathias
authors.initials: JM
authors.lastname: Griessmeier
authors.forename: Martin
authors.initials: M
authors.lastname: Leitner
authors.forename: Franck
authors.initials: F
authors.lastname: Selsis
authors.forename: Carlos
authors.initials: C
authors.lastname: Eiroa
authors.forename: Arnold
authors.initials: A
authors.lastname: Hanslmeier
authors.forename: Helfried K
authors.initials: HK
authors.lastname: Biernat
authors.forename: Charles J
authors.initials: CJ
authors.lastname: Farrugia
authors.forename: Helmut O
authors.initials: HO
authors.lastname: Rucker
mesh_terms: D055580:Astronomical Phenomena; D001256:Astronomy; D019419:Evolution, Planetary; D018559:Exobiology; D005118:Extraterrestrial Environment; D008280:Magnetics; D016083:Planets; D018561:Space Simulation; D014867:Water
chemical_list: D014867:Water