The early faint sun paradox: Organic shielding of ultraviolet-labile greenhouse gases

Science

Volumn 276, Issue 5316, 1997, Pages 1217-1221

  Sagan, Carl ^a   Chyba, Christopher ^b  

^a Department of Obstetrics Gynecology   (United States)

^b UNIVERSITY OF ARIZONA   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

AIR ANALYSIS; AIR TEMPERATURE; ARTICLE; GAS ANALYSIS; GREENHOUSE EFFECT; PRIORITY JOURNAL; SOLAR ENERGY;

NASA DISCIPLINE EXOBIOLOGY; NON-NASA CENTER;

AMMONIA; ATMOSPHERE; CARBON DIOXIDE; EARTH (PLANET); EVOLUTION, PLANETARY; GREENHOUSE EFFECT; METHANE; MODELS, CHEMICAL; PHOTOLYSIS; SOLAR SYSTEM; ULTRAVIOLET RAYS;

EID: 0031001793     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.276.5316.1217     Document Type: Article

References (116)

1. S. L. Miller and H. C. Urey, Science 130, 245 (1959).
2. J. C. G. Walker, Evolution of the Atmosphere (Macmillan, New York, 1977); Nature 302, 518 (1983); Origins Life 16, 117 (1986).
3. J. C. G. Walker, Evolution of the Atmosphere (Macmillan, New York, 1977); Nature 302, 518 (1983); Origins Life 16, 117 (1986).
4. J. C. G. Walker, Evolution of the Atmosphere (Macmillan, New York, 1977); Nature 302, 518 (1983); Origins Life 16, 117 (1986).
5. D. J. Stevenson, Science 214, 611 (1981).
6. J. F. Kasting, in The Proterozoic Biosphere, J. W. Schopf and C. Klein, Eds. (Cambridge Univ. Press, Cambridge, 1992), pp. 165-168.
7. R. J. Arculus, Annu. Rev. Earth Planet. Sci. 13, 75 (1985). Some models admit reduced gases as minor constituents [J. F. Kasting, D. H. Eggler, S. P. Raeburn, J. Geol. 101, 245 (1993); D. L. Anderson, Science 261, 170 (1993)].
8. R. J. Arculus, Annu. Rev. Earth Planet. Sci. 13, 75 (1985). Some models admit reduced gases as minor constituents [J. F. Kasting, D. H. Eggler, S. P. Raeburn, J. Geol. 101, 245 (1993); D. L. Anderson, Science 261, 170 (1993)].
9. R. J. Arculus, Annu. Rev. Earth Planet. Sci. 13, 75 (1985). Some models admit reduced gases as minor constituents [J. F. Kasting, D. H. Eggler, S. P. Raeburn, J. Geol. 101, 245 (1993); D. L. Anderson, Science 261, 170 (1993)].
10. W. R. Kuhn and S. K. Atreya, Icarus 37, 207 (1979).
11. Y. L. Yung and J. P. Pinto, Nature 273, 730 (1978); J. F. Kasting, J. Geophys. Res. 87, 3091 (1982).
12. Y. L. Yung and J. P. Pinto, Nature 273, 730 (1978); J. F. Kasting, J. Geophys. Res. 87, 3091 (1982).
13. T. Owen, R. D. Cess, V. Ramanathan, Nature 277, 640 (1979).
14. J. S. Levine and T. R. Augustsson, Origins Life 15, 299 (1985).
15. P. H. Abelson, Proc. Natl. Acad. Sci. U.S.A. 55, 1365 (1966); S. L. Miller and G. Schlesinger, Origins Life 14, 83 (1984).
16. P. H. Abelson, Proc. Natl. Acad. Sci. U.S.A. 55, 1365 (1966); S. L. Miller and G. Schlesinger, Origins Life 14, 83 (1984).
17. C. F. Chyba and C. Sagan, Nature 355, 125 (1992); in Comets and the Origin and Evolution of Life, P. J. Thomas, C. F. Chyba, C. P. McKay, Eds. (Springer-Verlag, New York, 1997), pp. 147-173.
18. C. F. Chyba and C. Sagan, Nature 355, 125 (1992); in Comets and the Origin and Evolution of Life, P. J. Thomas, C. F. Chyba, C. P. McKay, Eds. (Springer-Verlag, New York, 1997), pp. 147-173.
19. M. J. Newman and R. T. Rood, Science 198, 1035 (1977); D. O. Gough, Sol. Phys. 74, 21 (1981).
20. M. J. Newman and R. T. Rood, Science 198, 1035 (1977); D. O. Gough, Sol. Phys. 74, 21 (1981).
21. C. Sagan and G. Mullen, Science 177, 52 (1972).
22. C. Sagan, Nature 269, 224 (1977).
23. J. B. Pollack, Icarus 37, 479 (1979).
24. G. R. North, J. Atmos. Sci. 32, 2033 (1975); W. C. Wang and P. H. Stoner, ibid. 37, 545 (1980).
25. G. R. North, J. Atmos. Sci. 32, 2033 (1975); W. C. Wang and P. H. Stoner, ibid. 37, 545 (1980).
26. An updating of this evidence includes (i) water-lain sediments 3.8 to 3.9 Ga [A. P. Nutman, J. H. Allaart, D. Bridgewater, E. Dimroth, M. Rosing, Precambrian Res. 25, 365 (1984)]; tidal or intertidal stromatolite fossils ≃3.5 Ga; (iii) pillow basalts, generated by underwater magma; (iv) alluvial detrital uraninite grains 3.0 to 2.3 Ga; and (v) turbidites and ripple marks 3.5 to 3.0 Ga [K. A. Eriksson, Tectonophysics 81, 179 (1982)].
27. An updating of this evidence includes (i) water-lain sediments 3.8 to 3.9 Ga [A. P. Nutman, J. H. Allaart, D. Bridgewater, E. Dimroth, M. Rosing, Precambrian Res. 25, 365 (1984)]; (ii) tidal or intertidal stromatolite fossils ≃3.5 Ga; (iii) pillow basalts, generated by underwater magma; (iv) alluvial detrital uraninite grains 3.0 to 2.3 Ga; and (v) turbidites and ripple marks 3.5 to 3.0 Ga [K. A. Eriksson, Tectonophysics 81, 179 (1982)].
28. S. J. Mojzsis et al., Nature 384, 55 (1996); J. M. Eiler, S. J. Mojzsis, G. Arrhenius, ibid. 386, 665 (1997).
29. S. J. Mojzsis et al., Nature 384, 55 (1996); J. M. Eiler, S. J. Mojzsis, G. Arrhenius, ibid. 386, 665 (1997).
30. 18O data between coexisting cherts and phosphates have suggested temperatures as high as 100°C at 3.8 Ga [J. Karhu and S. Epstein, ibid. 50, 1745 (1986)].
31. 18O data between coexisting cherts and phosphates have suggested temperatures as high as 100°C at 3.8 Ga [J. Karhu and S. Epstein, ibid. 50, 1745 (1986)].
32. 18O data between coexisting cherts and phosphates have suggested temperatures as high as 100°C at 3.8 Ga [J. Karhu and S. Epstein, ibid. 50, 1745 (1986)].
33. 18O data between coexisting cherts and phosphates have suggested temperatures as high as 100°C at 3.8 Ga [J. Karhu and S. Epstein, ibid. 50, 1745 (1986)].
34. 18O data between coexisting cherts and phosphates have suggested temperatures as high as 100°C at 3.8 Ga [J. Karhu and S. Epstein, ibid. 50, 1745 (1986)].
35. 18O data between coexisting cherts and phosphates have suggested temperatures as high as 100°C at 3.8 Ga [J. Karhu and S. Epstein, ibid. 50, 1745 (1986)].
36. 18O data between coexisting cherts and phosphates have suggested temperatures as high as 100°C at 3.8 Ga [J. Karhu and S. Epstein, ibid. 50, 1745 (1986)].
37. M. H. Carr, Water on Mars (Oxford Univ. Press, New York, 1996).
38. Sagan and Mullen (13) argued that on a much colder early Earth, the ice-albedo feedback (and the lower water vapor pressure) would more than compensate for any decreased cloudiness. The strength of this argument might be diminished on an all-ocean planet only a little above the freezing point [A. Henderson-Sellers, Nature 279, 786 (1979); W. B. Rossow, A. Henderson-Sellers, S. K. Weinreich, Science 217, 1245 (1982)]. On an Earth as warm as or warmer than today, cloud feedback effects do not seem to be the answer [J. F. Kasting and D. H. Grinspoon, in The Sun in Time, C. P. Sonett, M. S. Giampapa, M. S. Matthews, Eds. (Univ. of Arizona Press, Tucson, 1991), pp. 447-462].
39. Sagan and Mullen (13) argued that on a much colder early Earth, the ice-albedo feedback (and the lower water vapor pressure) would more than compensate for any decreased cloudiness. The strength of this argument might be diminished on an all-ocean planet only a little above the freezing point [A. Henderson-Sellers, Nature 279, 786 (1979); W. B. Rossow, A. Henderson-Sellers, S. K. Weinreich, Science 217, 1245 (1982)]. On an Earth as warm as or warmer than today, cloud feedback effects do not seem to be the answer [J. F. Kasting and D. H. Grinspoon, in The Sun in Time, C. P. Sonett, M. S. Giampapa, M. S. Matthews, Eds. (Univ. of Arizona Press, Tucson, 1991), pp. 447-462].
40. Sagan and Mullen (13) argued that on a much colder early Earth, the ice-albedo feedback (and the lower water vapor pressure) would more than compensate for any decreased cloudiness. The strength of this argument might be diminished on an all-ocean planet only a little above the freezing point [A. Henderson-Sellers, Nature 279, 786 (1979); W. B. Rossow, A. Henderson-Sellers, S. K. Weinreich, Science 217, 1245 (1982)]. On an Earth as warm as or warmer than today, cloud feedback effects do not seem to be the answer [J. F. Kasting and D. H. Grinspoon, in The Sun in Time, C. P. Sonett, M. S. Giampapa, M. S. Matthews, Eds. (Univ. of Arizona Press, Tucson, 1991), pp. 447-462].
41. G. S. Jenkins, H. G. Marshall, W. R. Kuhn, J. Geophys. Res. 98, 8785 (1993).
42. M. J. Holman and J. Wisdom, Astron. J. 105, 1987 (1993).
43. T. E. Graedel, I.-J. Sackmann, A. I. Boothroyd, Geophys. Res. Lett. 18, 1881 (1991); A. I. Boothroyd, I.-J. Sackmann, W. A. Fowler, Astrophys. J. 377, 318 (1991).
44. T. E. Graedel, I.-J. Sackmann, A. I. Boothroyd, Geophys. Res. Lett. 18, 1881 (1991); A. I. Boothroyd, I.-J. Sackmann, W. A. Fowler, Astrophys. J. 377, 318 (1991).
45. More extreme models propose that solar-type stars lose as much as half their original mass through an enhanced solar wind, implying an initial main-sequence luminosity for the sun ∼15 times the current value [J. A. Guzik, L. A. Willson, W. M. Brunish, Astrophys. J. 319, 957 (1987)]. The equilibrium temperature for Earth at 1 AU and no greenhouse effect for a luminosity 15 times that of the sun's present value is <450 K. These models typically decay to standard stellar evolution values in ∼0.2 billion years, providing no contradiction to terrestrial observations in the high-luminosity phase; but then they do not explain temperatures >0°C on Earth between 4.3 and 2.0 Ga.
46. E. Robinson and R. C. Bobbins, J. Air Pollut. Control Assoc. 20, 303 (1970); A. O. Langford and F. C. Fehsenfeld, Science 255, 581 (1992); P. K. Quinn, R. S. Charlson, T. S. Bates, Nature 335, 336 (1988).
47. E. Robinson and R. C. Bobbins, J. Air Pollut. Control Assoc. 20, 303 (1970); A. O. Langford and F. C. Fehsenfeld, Science 255, 581 (1992); P. K. Quinn, R. S. Charlson, T. S. Bates, Nature 335, 336 (1988).
48. E. Robinson and R. C. Bobbins, J. Air Pollut. Control Assoc. 20, 303 (1970); A. O. Langford and F. C. Fehsenfeld, Science 255, 581 (1992); P. K. Quinn, R. S. Charlson, T. S. Bates, Nature 335, 336 (1988).
49. J. S. Levine, T. R. Augustsson, J. M. Hoell, Geophys. Res. Lett. 7, 317 (1980).
50. J. L. Bada and S. L. Miller, Science 159, 423 (1968).
51. S. L. Miller and J. E. Van Trump, in Origin of Life, Y. Wolman, Ed. (Reidel, Boston, 1981), p. 135; H. D. Holland, The Chemical Evolution of the Atmosphere and Oceans (Princeton Univ. Press, Princeton, NJ, 1984).
52. S. L. Miller and J. E. Van Trump, in Origin of Life, Y. Wolman, Ed. (Reidel, Boston, 1981), p. 135; H. D. Holland, The Chemical Evolution of the Atmosphere and Oceans (Princeton Univ. Press, Princeton, NJ, 1984).
53. + is also deposited from the atmosphere [J. D. Tjepkama, R. J. Cartica, H. F. Hemond, Nature 294, 445 (1981)].
54. + is also deposited from the atmosphere [J. D. Tjepkama, R. J. Cartica, H. F. Hemond, Nature 294, 445 (1981)].
55. + is also deposited from the atmosphere [J. D. Tjepkama, R. J. Cartica, H. F. Hemond, Nature 294, 445 (1981)].
56. R. C. Burns and R. W. F. Hardy, Nitrogen Fixation in Bacteria and Higher Plants (Springer-Verlag, Berlin, 1975); J. A. Raven, B. Wollenweber, L. L. Handley, New Phytol. 121, 5 (1992).
57. R. C. Burns and R. W. F. Hardy, Nitrogen Fixation in Bacteria and Higher Plants (Springer-Verlag, Berlin, 1975); J. A. Raven, B. Wollenweber, L. L. Handley, New Phytol. 121, 5 (1992).
58. W. R. Kuhn and J. F. Kasting, Nature 301, 53 (1983); J. F. Kasting and T. P. Ackerman, Science 234, 1383 (1986).
59. W. R. Kuhn and J. F. Kasting, Nature 301, 53 (1983); J. F. Kasting and T. P. Ackerman, Science 234, 1383 (1986).
60. R. Rye, P. H. Kuo, H. D. Holland, Nature 378, 603 (1995).
61. J. Goldspiel and S. W. Squyres, Icarus 89, 392 (1991); T. J. Parker, D. S. Gorsline, R. S. Saunders, D. C. Pieri, D. M. Schneeberger, J. Geophys. Res. 98, 11061 (1993).
62. J. Goldspiel and S. W. Squyres, Icarus 89, 392 (1991); T. J. Parker, D. S. Gorsline, R. S. Saunders, D. C. Pieri, D. M. Schneeberger, J. Geophys. Res. 98, 11061 (1993).
63. V. R. Baker et al., Nature 352, 589 (1991); M. W. Schaefer, J. Geophys. Res. 95, 14291 (1990).
64. V. R. Baker et al., Nature 352, 589 (1991); M. W. Schaefer, J. Geophys. Res. 95, 14291 (1990).
65. J. B. Pollack, J. F. Kasting, S. M. Richardson, K. Poliakoff, Icarus 71, 203 (1987).
66. S. W. Squyres and J. F. Kasting, Science 265, 744 (1994).
67. J. F. Kasting, Icarus 94, 1 (1991).
68. 2 [C. Sagan, J. Geophys. Res. 78, 1250 (1973)].
69. 2 [C. Sagan, J. Geophys. Res. 78, 1250 (1973)].
70. 2 [C. Sagan, J. Geophys. Res. 78, 1250 (1973)].
71. A. C. Lasaga, H. D. Holland, M. J. Dwyer, Science 174, 53 (1971).
72. W. E. McGovern, J. Atmos. Sci. 26, 623 (1969).
73. K. J. Zahnle, J. Geophys. Res. 91, 2819 (1986).
74. 2 adds only ∼10% to τ at 1216 Å.
75. 3 atmospheres, organic solids are also plentifully produced, involving aldehydes, ketones, furans, and carboxylic acids as indications of oxygen chemistry [B. N. Khare, C. Sagan, J. E. Zumberge, D. S. Sklarew, B. Nagy. Icarus 48, 290 (1981)]. Similar results are found in UV irradiation experiments [K.-y. Hong, J.-H. Hong, R. S. Becker, Science 184, 984 (1974); B. N. Khare, C. Sagan, E. L. Bandurski, B. Nagy, ibid. 199, 1199 (1978)].
76. 3 atmospheres, organic solids are also plentifully produced, involving aldehydes, ketones, furans, and carboxylic acids as indications of oxygen chemistry [B. N. Khare, C. Sagan, J. E. Zumberge, D. S. Sklarew, B. Nagy. Icarus 48, 290 (1981)]. Similar results are found in UV irradiation experiments [K.-y. Hong, J.-H. Hong, R. S. Becker, Science 184, 984 (1974); B. N. Khare, C. Sagan, E. L. Bandurski, B. Nagy, ibid. 199, 1199 (1978)].
77. 3 atmospheres, organic solids are also plentifully produced, involving aldehydes, ketones, furans, and carboxylic acids as indications of oxygen chemistry [B. N. Khare, C. Sagan, J. E. Zumberge, D. S. Sklarew, B. Nagy. Icarus 48, 290 (1981)]. Similar results are found in UV irradiation experiments [K.-y. Hong, J.-H. Hong, R. S. Becker, Science 184, 984 (1974); B. N. Khare, C. Sagan, E. L. Bandurski, B. Nagy, ibid. 199, 1199 (1978)].
78. G. D. McDonald, W. R. Thompson, M. Heinrich, B. N. Khare, C. Sagan, Icarus 107, 137 (1994).
79. V. R. Oberbeck, C. P. McKay, T. W. Scattergood, G. C. Carle, J. R. Valentin, Origins Life 19, 39 (1989).
80. M. Ackerman, in Mesospheric Models and Related Experiments, G. Fiocco, Ed. (Reidel, Boston, 1971), pp. 149-159.
81. B. N. Khare et al., Icarus 60, 127 (1984).
82. C. Sagan and W. R. Thompson, ibid. 59, 133 (1984).
83. W. A. Noyes and P. A. Leighton, The Photochemistry of Gases (Reinhold, New York, 1941).
84. G. Toupance, A. Bossard, R. Raulin, Origins Life 8, 259 (1977).
85. This result derives from continuous-flow experiments, in which the mean free path is much less than the radius of the reaction tube, so wall effects should not be important [W. R. Thompson, G. D. McDonald, C. Sagan, Icarus 112, 376 (1994)].
86. K. J. Zahnle and J. C. G. Walker, Rev. Geophys. Space Phys. 20, 280 (1982).
87. 2: Natural Variations Archean to Present, E. T. Sundquist and W. S. Broecker, Eds. (American Geophysical Union, Washington, DC, 1985), pp. 602-611.
88. 4 supply provided <1% of the required flux.
89. C. F. Chyba, T. C. Owen, W.-H. Ip, in Hazards Due to Comets and Asteroids, T. Gehrels, Ed. (Univ. of Arizona Press, Tucson, 1994), pp. 9-58.
90. G. A. Dawson, J. Geophys. Res. 82, 3125 (1977); D. L. Baulch et al., J. Phys. Chem. Ref. Data 11 (suppl. 1), 327 (1982).
91. G. A. Dawson, J. Geophys. Res. 82, 3125 (1977); D. L. Baulch et al., J. Phys. Chem. Ref. Data 11 (suppl. 1), 327 (1982).
92. R. Stribling and S. L. Miller, Origins Life 17, 261 (1987).
93. D. M. Hunten and T. M. Donahue, Annu. Rev. Earth Planet. Sci. 4, 265 (1976).
94. S. C. Wofsy and M. B. McElroy, J. Geophys. Res. 78, 2619 (1973).
95. e = -[Kn(z)/H][f(z) - f(0) ≤ (K/H) f(0)n(z).
96. C. Sagan, B. N. Khare, J. Lewis, in Saturn, T. Gehrels and M. S. Matthews, Eds. (Univ. of Arizona Press, Tucson, 1984), pp. 788-807.
97. A. Henderson-Sellers and A. W. Schwartz, Nature 287, 526 (1980).
98. C. Sagan, J. Theor. Biol. 39, 195 (1973); J. F. Kasting, K. J. Zahnle, J. P. Pinto, A. T. Young, Origins Life 19, 95 (1989).
99. C. Sagan, J. Theor. Biol. 39, 195 (1973); J. F. Kasting, K. J. Zahnle, J. P. Pinto, A. T. Young, Origins Life 19, 95 (1989).
100. K. Rages and J. B. Pollack, Icarus 41, 119 (1980).
101. While completing this paper, we learned that related suggestions were made qualitatively by J. Kasting [J. Geophys. Res. 87, 3091 (1982)] and J. Lovelock [The Ages of Gaia (Norton, London, 1988), chap. 4].
102. While completing this paper, we learned that related suggestions were made qualitatively by J. Kasting [J. Geophys. Res. 87, 3091 (1982)] and J. Lovelock [The Ages of Gaia (Norton, London, 1988), chap. 4].
103. B. N. Khare et al., Icarus 103, 290 (1993).
104. P. Jenniskens, Astron. Astrophys. 272, 465 (1993).
105. G. Chlewicki and J. M. Greenberg, Astrophys. J. 365, 230 (1990).
106. J. M. Greenberg and J. I. Hage, ibid. 361, 260 (1990).
107. H. J. Hagemann, W. Gudat, C. Kunz, J. Opt. Soc. Am. 65, 742 (1975).
108. W. W. Duley, Astrophys. J. 287, 694 (1984).
109. E. Bussoletti, L. Colangeli, A. Borgnesi, V. Orofino, Astron. Astrophys. Suppl. Ser. 70, 257 (1987).
110. F. Rouleau and P. G. Martin, Astrophys. J. 377, 526 (1991).
111. E. T. Arakawa, S. M. Dolfini, J. C. Ashley, M. W. Williams, Phys. Rev. B 31, 8097 (1985).
112. D. A. Anderson, Philos. Mag. 35, 17 (1977).
113. S. C. Lee and C. L. Tien, Proceedings, Eighteenth Symposium (International) on Combustion (Combustion Institute, Pittsburgh, 1981), pp. 1159-1166.
114. W. R. Thompson, B. G. J. T. P. Murray, B. N. Khare, C. Sagan, J. Geophys. Res. 92, 14933 (1987); B. N. Khare, W. R. Thompson, B. G. J. T. P. Murray, C. F. Chyba, C. Sagan, Icarus 79, 350 (1989).
115. W. R. Thompson, B. G. J. T. P. Murray, B. N. Khare, C. Sagan, J. Geophys. Res. 92, 14933 (1987); B. N. Khare, W. R. Thompson, B. G. J. T. P. Murray, C. F. Chyba, C. Sagan, Icarus 79, 350 (1989).
116. This research was supported in part by NASA grants NAGW-3273, NAGW-1896, and NAGW-1870. We thank K. J. Zahnle, J. Bada, J. Kasting, W. R. Thompson, B. N. Khare, S. L. Miller, E. E. Salpeter, S. Epstein, J. W. Schopf, D. Layzell, D. Turpin, J. C. G. Walker, S. Soter, J. Goldspiel, P. Gogarten, L. A. Wilson, G. Bowen, C. de Ruiter, R. Margraves, and G. D. McDonald.