Hostname: page-component-848d4c4894-2pzkn Total loading time: 0 Render date: 2024-05-11T09:32:56.642Z Has data issue: false hasContentIssue false
  • English
  • Français

Evolution of the Solar Magnetic Activity over Time and Effects on Planetary Atmospheres

Published online by Cambridge University Press:  26 May 2016

Edward F. Guinan  and
Ignasi Ribas
Edward F. Guinan
Affiliation:
Dept. of Astronomy & Astrophysics, Villanova University, USA
Ignasi Ribas
Affiliation:
Dept. d'Astronomia i Meteorologia, Univ. Barcelona, Spain

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We report on the results of a multi-wavelength program (X-rays to the near IR) of solar analogs with ages covering ∼0.1—9 Gyr. The chief science goals are to study the solar magnetic dynamo and to determine the radiative and magnetic properties of the Sun during its evolution across the main sequence. The present paper focuses on the latter goal, which has the ultimate purpose of constructing spectral irradiance tables to be used to study and model planetary atmospheres. The results obtained thus far indicate that the young Sun was extremely active, with large flares, massive winds, and high-energy emissions up to 1000 times stronger than presently. The strong radiation and particle emissions inferred should have had major influences on the photochemistry and photo-ionization of paleo-planetary atmospheres and also played an important role in the development of primitive life in the Solar System. Some recent results of the effects of the young Sun's enhanced radiation and particle emissions on the early Solar System planets are discussed.

Type
Part 8: Stellar Analogues for Interaction and Evolution
Information
Symposium - International Astronomical Union , Volume 219: Stars as Suns : Activity, Evolution and Planets , 2004 , pp. 423 - 430
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Audard, M., Güdel, M., & Guinan, E. F. 1999, ApJ, 513, L53.Google Scholar
Ayres, T. R. 1997, JGR, 102, 1641.CrossRefGoogle Scholar
Cameron, A. G. W. 1985, Icarus, 64, 285.Google Scholar
Canuto, V. M., Levine, J. S., Augustsson, T. R., & Imhoff, C. L. 1982, Nature, 296, 816.CrossRefGoogle Scholar
Canuto, V. M., Levine, J. S., Augustsson, T. R., Imhoff, C. L., & Giampapa, M. S. 1983, Nature, 305, 281.Google Scholar
Guinan, E. F., Ribas, I., & Harper, G. M. 2003, ApJ, 594, 561.Google Scholar
Kasting, J. F., Whitmire, D. P., & Reynolds, R. T. 1993, Icarus, 101, 108.Google Scholar
Lammer, H., Tehrany, M. G., Hanslmeier, A., Ribas, I., Guinan, E. F., & Kolb, C. 2002, poster presented at the 2002 EGS meeting (Nice).Google Scholar
Lammer, H., Selsis, F., Ribas, I., Guinan, E. F., & Weiss, W. W. 2003a, ApJ, 598, L121.CrossRefGoogle Scholar
Lammer, H., Lichtenegger, H., Kolb, C., Ribas, I., Guinan, E. F., & Bauer, S. J. 2003b, Icarus, 165, 9.Google Scholar
Pavlov, A. A., Kasting, J. F., Brown, L. L., Rages, K. A., & Freedman, R. 2000, JGR, 105, 11981.Google Scholar
Rye, R., Kuo, P. H., & Holland, H. D. 1995, Nature, 378, 603.CrossRefGoogle Scholar
Sagan, C., & Mullen, G. 1972, Science, 177, 52.CrossRefGoogle Scholar
Sagan, C., & Chyba, C. 1997, Science, 276, 1217.CrossRefGoogle Scholar
Walker, A. R. 1981, MNRAS, 195, 1029.CrossRefGoogle Scholar
Wood, B. E., Müller, H.-R., Zank, G., & Linsky, J. L. 2002, ApJ, 574, 412.Google Scholar
Zahnle, K. J., & Walker, J. C. G. 1982, Rev. Geophys. Space Phys., 20, 280.Google Scholar