Title: A Volcanic Hydrogen Habitable Zone,
Abstract: The classical habitable zone is the circular region around a star in which
liquid water could exist on the surface of a rocky planet. The outer edge of
the traditional N2-CO2-H2O habitable zone (HZ) extends out to nearly 1.7 AU in
our Solar System, beyond which condensation and scattering by CO2 outstrips its
greenhouse capacity. Here, we show that volcanic outgassing of atmospheric H2
on a planet near the outer edge can extend the habitable zone out to ~2.4 AU in
our solar system. This wider volcanic hydrogen habitable zone (N2-CO2-H2O-H2)
can be sustained as long as volcanic H2 output offsets its escape from the top
of the atmosphere. We use a single-column radiative-convective climate model to
compute the HZ limits of this volcanic hydrogen habitable zone for hydrogen
concentrations between 1% and 50%, assuming diffusion-limited atmospheric
escape. At a hydrogen concentration of 50%, the effective stellar flux required
to support the outer edge decreases by ~35% to 60% for M to A stars. The
corresponding orbital distances increase by ~30% to 60%. The inner edge of this
HZ only moves out by ~0.1 to 4% relative to the classical HZ because H2 warming
is reduced in dense H2O atmospheres. The atmospheric scale heights of such
volcanic H2 atmospheres near the outer edge of the HZ also increase,
facilitating remote detection of atmospheric signatures.