Thermodynamic Limits Around M-dwarf Stars: Orbital Distances and Incident Spectral Fluxes

:::info (1) Samir Chitnavis, School of Biological and Behavioural Sciences, Queen Mary University of London, Mile End, London E1 4NS, UK & Digital Environment Research Institute, Queen Mary University of London, Empire House, Whitechapel E1 1HH, UK;

(2) Thomas J. Haworth, Astronomy Unit, Queen Mary University of London, Mile End Road, London E1 4NS, UK;

(3) Edward Gillen, Astronomy Unit, Queen Mary University of London, Mile End Road, London E1 4NS, UK;

(4) Conrad W. Mullineaux, School of Biological and Behavioural Sciences, Queen Mary University of London, Mile End, London E1 4NS, UK;

(5) Christopher D. P. Duffy, School of Biological and Behavioural Sciences, Queen Mary University of London, Mile End, London E1 4NS, UK & Digital Environment Research Institute, Queen Mary University of London, Empire House, Whitechapel E1 1HH, UK (Email: [email protected]).

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• Abstract and Introduction
• 2 Methodology
• 2.1 Local spectral irradiance as a function of stellar temperature
• 2.2 Thermodynamic model of an oxygenic light-harvesting system
• 2.3 Lattice model of an oxygenic light-harvesting system
• 3 Results
• 3.1 Orbital distances and incident spectral fluxes
• 3.2 Thermodynamic antenna model: Increasing antenna size in limited PAR
• 3.3 Lattice antenna model: Increasing the size of a “flat” antenna in limited PAR
• 3.4 Lattice antenna model: Improving antenna efficiency with an energetic ’funnel’
• 4 Discussion
• Acknowledgements, Author Contribution Statement, Authors disclosure statement and References

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:::info This paper is available on arxiv under CC 4.0 license.

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