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This study evaluates the probability of carbon-based life emerging around different types of stars by analyzing how stellar UV radiation drives the formation and stability of organic molecules through photochemical processes. Using thermodynamic models, researchers found that F-, G-, and K-type stars provide optimal conditions for creating high concentrations of life's building blocks within weeks to months, while M-dwarf stars produce extremely low molecular concentrations requiring years to accumulate. The analysis suggests that Earth-like life is most probable around sun-like G-type stars, with M-dwarfs being unlikely hosts unless life arrives through panspermia.
Why it matters
These findings could significantly refine the search for extraterrestrial life by identifying which stellar systems are most promising targets for biosignature detection and potentially habitable exoplanets. The work provides a thermodynamic framework for prioritizing astronomical observations and SETI efforts toward stars most likely to support complex, carbon-based life.
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⚠️ Preprint – Noch nicht peer-reviewed
Dieser Artikel wurde noch nicht von unabhängigen Experten begutachtet. Die Ergebnisse sind vorläufig und sollten mit Vorsicht interpretiert werden.
Abstract: From the non-equilibrium thermodynamic perspective of the origin of life as a photochemical dissipative structuring (entropy driven) process, we assess the probability of carbon-based life arising on Earth-like analogues orbiting different main-sequence stellar types (O7 V to M2 V). Using black-body spectra normalized to Earth’s solar constant, we calculate surface photon fluxes for an atmosphere like early Archean Earth’s in the productive dissipative structuring (P, soft UV-C + UV-B, 205-320 nm) and destructive ionization (D, hard UV-C + EUV, <205 nm) regions. Stationary concentrations of fundamental molecules and times to reach 99% of these are computed for different chemical degradation (e.g., deamination, hydrolysis, oxidation, etc.) rate constants of k = 10^{-7}, 10^{-6}, and 10^{-5} s^{-1}. For a nominal chemical degradation rate constant of k = 10^{-6} s^{-1} (t_{1/2}= 8 days), results show F-, G-, and K-type stars provide the highest stationary concentrations of fundamental molecules and short rise times (weeks to months), while quiescent M-type stars yield extremely low concentrations (~10^{-7} relative to G stars) and require years to reach even these values. Flaring M stars improve stationary concentrations by about an order of magnitude (~10^{-6} relative to G stars) but produce adverse planet surface environments for complex evolution through dissipative structuring. From this non-equilibrium thermodynamic perspective, carbon-based life like Earth's is to be found most probably on F-, G-, and high-mass K-type stars, with intelligent life arising only on G-type stars. Low mass K- and M-dwarfs are highly unlikely to harbor life unless seeded via panspermia. Biosignatures related to the thermodynamic imperative of photon dissipation are proposed.
Source: Abiogenesis on Different Star Types; a Dissipative Photochemical Perspective