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Equilibrium temperatures of porous spheres and their relevance to astrobiology

Published online by Cambridge University Press:  21 August 2007

S.G. Coulson  and
N.C. Wickramasinghe
S.G. Coulson
Affiliation:
Centre for Astrobiology, School of Mathematics, Cardiff University, 2 North Road, Cardiff CF10 3DY, UK e-mail: coulson@aldpartners.com; wickramasinghe@cf.ac.uk
N.C. Wickramasinghe
Affiliation:
Centre for Astrobiology, School of Mathematics, Cardiff University, 2 North Road, Cardiff CF10 3DY, UK e-mail: coulson@aldpartners.com; wickramasinghe@cf.ac.uk
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Abstract

Equilibrium temperatures are calculated for porous, organic spheres at a Solar distance of around 1 AU. It is found that the equilibrium temperature of porous grains is highly sensitive to their composition and radius. For porous organic grains of radius 0.1 μm the temperature ranges from 355 to 386 K as the porosity (vacuum volume fraction) increases from 0 to 0.9; for organic grains of radius 0.1 μm with 10% charring the corresponding range is from 448 to 431 K. Such superheated submicron grains, porous or otherwise, may have only a limited role as transporters of fragile biomolecules. Clumps of biological particles with radii in excess of 5 μm are, however, at low enough temperatures to permit such transport at 1 AU.

Keywords

OrganicsradiationMaxwell–Garnettpanspermia
Type
Research Article
Information
International Journal of Astrobiology , Volume 6 , Issue 4 , October 2007 , pp. 263 - 266
Copyright
Copyright © Cambridge University Press 2007

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References

Abadi, H. & Wickramasinghe, N.C. (1976). Astrophys. Space Sci. 39, L31–L32.CrossRefGoogle Scholar
Blanco, A. & Bussoletti, E. (1980). Astrophys. Space Sci. 67, 105–110.CrossRefGoogle Scholar
Bohren, C.F. & Huffman, D.R. (1983). Absorption and Scattering of Light by Small Particles. Wiley, New York.Google Scholar
Bohren, C.F. & Wickramasinghe, N.C. (1977). Astrophys. Space Sci. 50, 461–472.CrossRefGoogle Scholar
Coulson, S.G. (2004) Int. J. Astrobiol. 3(2), 151–156.CrossRefGoogle Scholar
Coulson, S.G. & Wickramasinghe, N.C. (2003). Mon. Notices R. Astron. Soc. 343, 1123–1130.CrossRefGoogle Scholar
Millman, P.M. (1972). The meteoritic complex. In From Plasma to Planet, Proc. 21st Nobel Symposium, Saltsjöbaden, Sweden, 6–10 September, 1971, ed. Elvius, A.Wiley, New York.Google Scholar
Hoyle, F. & Wickramasinghe, N.C. (1979). Astrophys. Space Sci. 66(1), 77–90.CrossRefGoogle Scholar
Taft, E.A. & Philipp, H.R. (1965). Phys. Rev. A 138, 197.CrossRefGoogle Scholar
Van de Hulst, H.C. (1957). Light Scattering by Small Particles. Wiley, New York.CrossRefGoogle Scholar
Wainwright, M. et al. (2004). Int. J. Astrobiol. 3(1), 13–15.CrossRefGoogle Scholar
Wallis, M.K., Rabilizirov, R. & Wickramasinghe, N.C. (1987). Astron. Astrophys. 187, 801.Google Scholar
Wickramasinghe, N.C. (1973). Light Scattering by Small Particles with Applications in Astronomy. Adam Hilger, London.Google Scholar