Abstract
We present a model of the solar atmosphere in the optical depth range from τ5000 = 10−8 to 25. It combines an improved model of the photosphere that incorporates recent EUV observations with a new model of the quiet lower chromosphere. The latter is based on OSO 4 observations of the Lyman continuum, on infrared observations, and on eclipse electron densities.
Our model differs from the Bilderberg Continuum Atmosphere (BCA) in the low chromosphere (τ5000 < 10−4), where deviations from local thermodynamic equilibrium in hydrogen and carbon have been taken into account. It also differs in the transition region between the chromosphere and the photosphere (10−4 < τ5000 < 10−2), where the temperature is lower than in the BCA, and in the convective region (τ5000 ≳ 2), where the temperature is higher than in the BCA.
Article PDF
Similar content being viewed by others
Avoid common mistakes on your manuscript.
References
Athay, R. G.: 1969, Solar Phys. 9, 51.
Bonnet, R. M.: 1968, Ann. Astrophys. 31, 597.
Bötticher, W.: 1958, Z. Physik 150, 336.
Carbon, D. F. and Gingerich, O.: 1969, in Theory and Observations of Normal Stellar Atmospheres (ed. by O. Gingerich), Massachusetts Institute of Technology Press, Cambridge, p. 377.
Carbon, D. F., Gingerich, O., and Kurucz, R.: 1968, Solar Phys. 3, 55.
Conneely, M. J., Smith, K., and Lipsky, L.: 1970, J. Phys. B 3, 493.
Cuny, Y.: 1969, in Theory and Observations of Normal Stellar Atmospheres (ed. by O. Gingerich), Massachusetts Institute of Technology Press, Cambridge, p. 173.
Cuny, Y.: 1971, Solar Phys. 16, 293.
Doyle, R. O.: 1968, Astrophys. J. 153, 987.
Eddy, J. A., Léna, P. J., and MacQueen, R. M.: 1969a, Bull. Am. Astron. Soc. 1, 275.
Eddy, J. A., Léna, P. J., and MacQueen, R. M.: 1969b, Solar Phys. 10, 330.
Elste, G.: 1968, Solar Phys. 3, 106.
Garz, T., Holweger, H., Kock, M., and Richter, J.: 1969, Astron. Astrophys. 2, 446.
Gay, J.: 1970, Astron. Astrophys. 6, 327.
Gingerich, O.: 1970, in L. Houziaux and H. E. Butler (eds.), ‘Ultraviolet Stellar Spectra and Related Ground-Based Observations’, IAU Symp. 36, 140.
Gingerich, O. and de Jager, C.: 1968, Solar Phys. 3, 5.
Goldberg, L., Noyes, R. W., Parkinson, W. H., Reeves, E. M., and Withbroe, G. L.: 1968, Science 162, 95.
Henze, Jr., W.: 1969, Solar Phys. 9, 65.
Holweger, H.: 1970, Astron. Astrophys. 4, 11.
Houtgast, J.: 1968, Solar Phys. 3, 47.
Koutchmy, S. and Peyturaux, R.: 1968, Compt. Rend. 267, 905.
Kozlov, M. G. and Startsev, G. P.: 1969, Opt. Spectrosc. 27, 383.
Labs, D. and Neckel, H.: 1968, Z. Astrophys. 69, 1.
Labs, D. and Neckel, H.: 1970, Solar Phys. 15, 79.
Lambert, D. L. and Warner, B.: 1968, Monthly Notices Roy. Astron. Soc. London 138, 181.
Léna, P. J.: 1970, Astron. Astrophys. 4, 207.
Linsky, J. and Avrett, E. H.: 1970, Publ. Astron. Soc. Pacific 82, 169.
Mankin, W. G.: 1969, Ph.D. Thesis, Johns Hopkins University, Baltimore, Md.
Mankin, W. G. and Strong, J.: 1969, Bull. Am. Astron. Soc. 1, 200.
McGuire, E. J.: 1968, Phys. Rev. 175, 20.
Noyes, R. W. and Kalkofen, W.: 1970, Solar Phys. 15, 120.
Parkinson, W. H. and Reeves, E. M.: 1969, Solar Phys. 10, 342.
Parkinson, W. H. and Reeves, E. M.: 1970, Personal communication.
Peach, G.: 1967, Mem. Roy. Astron. Soc. 71, 29.
Saiedy, F.: 1960, Monthly Notices Roy. Astron. Soc. London 121, 483.
Sando, K.: 1969, Personal communication (see Table III).
Sando, K., Doyle, R. O., and Dalgarno, A.: 1969, Astrophys. J. 157, L143.
Tousey, R.: 1963, Space Sci. Rev. 2, 3.
Widing, K. G., Purcell, J. D., and Sandlin, G. D.: 1970, Solar Phys. 12, 52.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Gingerich, O., Noyes, R.W., Kalkofen, W. et al. The Harvard-Smithsonian reference atmosphere. Sol Phys 18, 347–365 (1971). https://doi.org/10.1007/BF00149057
Received:
Issue Date:
DOI: https://doi.org/10.1007/BF00149057