<p>Despite decades of observations, the physical processes governing mass loss from small bodies beyond our Solar System remain poorly constrained. These “exocomets” are often treated as analogs of Solar System comet, yet the stellar environments they inhabit spans a wide range in terms of luminosity, stellar wind intensity, and evolutionary stage, leading to potentially very diverse physical behaviors. Within our Solar System, small bodies lose gas and dust through a range of mechanisms, including sublimation, desorption, impacts, and/or sputtering. Once released, the composition and dynamics of the ejecta are then altered by additional processes, such as dust sublimation, ionization, and radiation pressure. In extrasolar systems, these mechanisms unfold under vastly different radiative and plasma conditions, leading to a rich diversity of mass-loss pathways and observable signatures. This work reviews our understanding of the mechanisms driving mass loss from small bodies and the subsequent evolution of ejecta in diverse stellar environments. We compare the physical and chemical mechanisms that drive gas and dust production, such as sublimation, thermal and photon desorption, and investigate how they scale with stellar luminosity, temperature, and activity. We then examine the processes that modify the composition of the ejecta (e.g., dust sublimation, dissociation, or ionisation) and its dynamics (e.g., radiation pressure or stellar winds). To illustrate how these processes vary across different stellar environments, we use four well-studied planetary systems as case studies: the Sun, <InlineEquation ID="IEq1"> <EquationSource Format="MATHML"><math> <mi mathvariant="normal">β</mi> </math></EquationSource> <EquationSource Format="TEX">$\upbeta $</EquationSource> </InlineEquation> Pictoris, AU Microscopii, and WD 1145+017. By exploring how cometary tails behave under such diverse conditions, this work provides a physical framework for interpreting exocometary activity and sheds light on why A-type stars, such as the famous <InlineEquation ID="IEq2"> <EquationSource Format="MATHML"><math> <mi mathvariant="normal">β</mi> </math></EquationSource> <EquationSource Format="TEX">$\upbeta $</EquationSource> </InlineEquation>-Pictoris, are over-represented in the population of exocomet-hosting stars.</p>

Exocometary Physics: Material Release and Tails

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2026年3月23日

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Théo Vrignaud,
Dennis Bodewits,
Jake Hanlon,
Matthew M. Knight,
Tim D. Pearce,
Daryl Z. Zeligman,
Dimitri Veras,
Geraint H. Jones

摘要

Despite decades of observations, the physical processes governing mass loss from small bodies beyond our Solar System remain poorly constrained. These “exocomets” are often treated as analogs of Solar System comet, yet the stellar environments they inhabit spans a wide range in terms of luminosity, stellar wind intensity, and evolutionary stage, leading to potentially very diverse physical behaviors. Within our Solar System, small bodies lose gas and dust through a range of mechanisms, including sublimation, desorption, impacts, and/or sputtering. Once released, the composition and dynamics of the ejecta are then altered by additional processes, such as dust sublimation, ionization, and radiation pressure. In extrasolar systems, these mechanisms unfold under vastly different radiative and plasma conditions, leading to a rich diversity of mass-loss pathways and observable signatures. This work reviews our understanding of the mechanisms driving mass loss from small bodies and the subsequent evolution of ejecta in diverse stellar environments. We compare the physical and chemical mechanisms that drive gas and dust production, such as sublimation, thermal and photon desorption, and investigate how they scale with stellar luminosity, temperature, and activity. We then examine the processes that modify the composition of the ejecta (e.g., dust sublimation, dissociation, or ionisation) and its dynamics (e.g., radiation pressure or stellar winds). To illustrate how these processes vary across different stellar environments, we use four well-studied planetary systems as case studies: the Sun, $β$ $\upbeta $ Pictoris, AU Microscopii, and WD 1145+017. By exploring how cometary tails behave under such diverse conditions, this work provides a physical framework for interpreting exocometary activity and sheds light on why A-type stars, such as the famous $β$ $\upbeta $ -Pictoris, are over-represented in the population of exocomet-hosting stars.