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Comets have been invoked in numerous studies as a potentially importantsource of dust and gas around stars, but none has studied the thermo-physicalevolution, out-gassing rate, and dust ejection of these objects in such stellarsystems. We investigate the thermo-physical evolution of comets inexo-planetary systems in order to provide valuable theoretical data required tointerpret observations of gas and dust. We use a quasi 3D model of cometarynucleus to study the thermo-physical evolution of comets evolving around asingle star from 0.1 to 50 AU, whose homogeneous luminosity varies from 0.1 to70 solar luminosities. This paper provides mass ejection, lifetimes, and therate of dust and water gas mass productions for comets as a function of thedistance to the star and stellar luminosity. Results show significant physicalchanges to comets at high stellar luminosities. The models are presented insuch a manner that they can be readily applied to any planetary system. Byconsidering the examples of the Solar System, Vega and HD 69830, we show thatdust grains released from sublimating comets have the potential to create theobserved (exo)zodiacal emission. We show that observations can be reproduced by1 to 2 massive comets or by a large number of comets whose orbits approachclose to the star. Our conclusions depend on the stellar luminosity and theuncertain lifetime of the dust grains. We find, as in previous studies, thatexozodiacal dust disks can only survive if replenished by a population oftypically sized comets renewed from a large and cold reservoir of cometarybodies beyond the water ice line. These comets could reach the inner regions ofthe planetary system following scattering by a (giant) planet.

Extrasolar comets : the origin of dust in exozodiacal disks?