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9 - The model photosphere

David F. Gray
David F. Gray
Affiliation:
University of Western Ontario
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Summary

What is a model photosphere, and why build one? It would seem logical to take our stellar observations and deduce from them the physical conditions existing in the atmosphere of the star – somewhat like a parallax measurement yields the distance to a star. Alas, the formation of the stellar spectrum involves many physical variables, and a rigorous deductive interpretation cannot generally be made. Instead we hypothesize a model through which we organize and relate the information conveyed in the starlight. The model resembles a scientific theory in that it is constructed on the basis of our observations and known physical laws. We may then gather additional observations to test our model much like we would test a theory. The model is modified and improved as information is added. When our model closely reproduces all the available observations, we begin to feel that our model is worthy of some trust. Then properties associated with the model, or deduced from further application of the model, are associated with the star, properties such as effective temperature, surface gravity, radius, chemical composition, or rate of rotation.

The model photosphere consists of a table of numbers giving the source function and the pressure as a function of optical depth for an assumed chemical composition. Additional columns may be added to the table depending on the use intended for the model.

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The Observation and Analysis of Stellar Photospheres , pp. 170 - 203
Publisher: Cambridge University Press
Print publication year: 2005

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References

Abbott, D.C. & D.G., Hummer 1985. Ap. J. 294, 286.CrossRef
Allende Preito, C., I., Hubeny, & D.L., Lambert 2003. Ap. J. 591, 1192.CrossRef
Anderson, L.S. 1989. Ap. J. 339, 558.CrossRef
Athay, R.G. & A., Skumanich 1969. Ap. J. 155, 273.CrossRef
Auer, L.H. & D., Mihalas 1969. Ap. J. 158, 641.CrossRef
Avrett, E.H. & M., Krook 1963a. Ap. J. 137, 874.CrossRef
Avrett, E.H. & M., Krook 1963b. J. Quant. Spectr. Rad. Trans. 3, 107.CrossRef
Ayres, T.R. 1981. Ap. J. 244, 1064.CrossRef
Ayres, T.R. & L., Testerman 1981. Ap. J. 245, 1124.CrossRef
Ayres, T.R. & G.R., Wiedeman 1989. Ap. J. 338, 1033.CrossRef
Bell, R.A., J., Eriksson, B., Gustafsson, & Å., Norlund 1976. Ast. Ap. Suppl. 23, 37.
Bessell, M., J.M., Brett, M., Scholz, & P. R., Wood 1989. Ast. Ap. 213, 209.
Bohannan, B., D.C., Abbott, S.A., Voels, & D.C., Hummer 1986. Ap. J. 308, 728.CrossRef
Böhm, K.H. 1966. J. Quant. Spectr. Rad. Trans. 6, 534.
Cannon, C.J. 1973a. J. Quant. Spectr. Rad. Trans. 13, 627.CrossRef
Cannon, C.J. 1973b. Ap. J. 185, 621.CrossRef
Carbon, D.F. 1979. Ann. Rev. Ast. Ap. 17, 513.CrossRef
Carbon, D.F. & O., Gingerich 1969. Theory and Observation of Normal Stellar Atmospheres, ed. O., Gingerich. (Cambridge: MIT), p. 377.Google Scholar
Decin, L., B., Vandenbussche, C., Waelkens, et al. 2003. Ast. Ap. 400, 709.
Drake, J.J. & G., Smith 1991. Mon. Not. Roy. Ast. Soc. 250, 89.CrossRef
Edmonds, F.N. Jr. 1969. J. Quant. Spectr. Rad. Trans. 9, 1427.CrossRef
Elste, G.H.E. 1967. Ap. J. 148, 857.CrossRef
Elste, G.H.E. 1985. Theoretical Problems in High Resolution Solar Physics, ed. H. U., Schmidt. (München: Max Planck Inst. Ap.), p. 185.Google Scholar
Ferguson, J.W., D.R., Alexander, F., Allard, & P., Hauschildt 2001. Ap. J. 557, 798.CrossRef
Gingerich, O., D.W., Latham, J., Linsky, & S.S., Kumar 1966. Coll. on Late-Type Stars, ed. M., Hack. (Trieste: Osservatorio Astronomico), p. 291.Google Scholar
Gray, D.F. 1984. Ap. J. 281, 719.CrossRef
Gray, D.F. 1989. Ap. J . 347, 1021.CrossRef
Groth, H.G. 1961. Z.f. Ap. 51, 231.
Gustafsson, B., R. A., Bell, J., Eriksson, & Å., Nordlund 1975. Ast. Ap. 42, 407.
Heasley, J.N., S.T., Ridgway, D.F., Carbon, R. W., Milkey, & D. N., Hall 1978. Ap. J. 219, 970.CrossRef
Holweger, H. & E.A., Müller 1974. Solar Phys. 39, 19.CrossRef
Johnson, H.R., A.P., Bernat, & B.M., Krupp 1980. Ap. J. Suppl. 42, 501.CrossRef
Jorgenson, U.G., H.R., Johnson, & Å., Nordlund 1992. Ast. Ap. 261, 263.
Kalkofen, W. 1987. Numerical Radiative Transfer. (Cambridge: Cambridge University press).Google Scholar
Kurucz, R.L. 1979. Ap. J. Suppl. 40, 1.CrossRef
Lester, J.B., M.C., Lane, & R.L., Kurucz 1982. Ap. J. 260, 272.CrossRef
Maltby, P., E.H., Avrett, M., Carlsson, O., Kjeldseth-Moe, R.L., Kurucz, & R., Loeser 1986. Ap. J. 306, 284.CrossRef
Mihalas, D. 1966. Ap. J. Suppl. 13, 1.CrossRef
Mihalas, D. 1967. Ap. J. 149, 169.CrossRef
Mihalas, D. 1972. Ap. J. 176, 139.CrossRef
Mihalas, D.M. & W.R., Luebke 1971. Mon. Not. Roy. Ast. Soc. 153, 229.CrossRef
Mitchell, W.E. Jr. 1959. Ap. J. 129, 93.CrossRef
Muchmore, D. 1986. Ast. Ap. 155, 172.
Nordlund, Å. 1985. Theoretical Problems in High Resolution Solar Physics, ed. H.U., Schmidt. (München: Max Planck Inst. Ap.), p. 19.Google Scholar
Osmer, P.S. 1972. Ap. J. Suppl. 24, 255.CrossRef
Parsons, S.B. 1969. Ap. J. Suppl. 18, 127.CrossRef
Pecker, J.C. 1973. Problems of Calibration of Absolute Magnitudes and Temperature of Stars, IAU Symp. 54, ed. B., Hauck & B. E., Westerlund. (Dordrecht: Reidel), p. 173.CrossRefGoogle Scholar
Pierce, A.K. 2000. Allen's Astrophysical Quantites, 4th edn, ed. A.N., Cox. (London: Athlone), p. 355.Google Scholar
Pierce, A.K. & J.H., Waddell 1961. Mem. Roy. Ast. Soc. 68, 89.
Plez, B., J.M., Brett, & Å., Nordlund 1992. Ast. Ap. 256, 551.
Ruck, M.J. & G., Smith 1995. Ast. Ap. 304, 449.
Ruland, F.D.Biehl, H. Holweger, R., Griffin, & R., Griffin 1980. Ast. Ap. 92, 70.
Rutten, R.J. 1990. Cool Stars, Stellar Systems, and the Sun, 6th Cambridge Workshop, ed. G., Wallerstein. (San Francisco: Ast. Soc. Pacific), p. 91.Google Scholar
Scharmer, G.B. 1981. Ap. J. 249, 720.CrossRef
Schmid-Burgk, J., M., Scholz, & R., Wehrse 1981. Mon. Not. Roy. Ast. Soc. 194, 383.CrossRef
Scholz, M. 1985. Ast. Ap. 145, 251.
Smith, M.A. & S. E., Strom 1969. Ap. J. 158, 1161.CrossRef
Strom, S.E. & W., Kalkofen 1966. Ap. J. 144, 76.CrossRef
Tripicchio, A., G., Severino, E., Covino, L., Terranegra, & R.J. Garcia, Lopez 1997. Ast. Ap. 327, 681.
Tsuji, T. 1966. Colloquium on Late-Type Stars, ed. M., Hack. (Trieste: Osservatorio Ast.), p. 260.Google Scholar
Tsuji, T. 1978. Ast. Ap. 62, 29.
Underhill, A. B. 1968. Bull. Ast. Inst. Netherlands 19, 500.
Werner, K. 1988. Ast. Ap. 204, 159.
Wesemael, F., H.M., van Horn, M.P., Savedoff, & L.H., Auer 1980. Ap. J. Suppl. 43, 159.CrossRef

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  • The model photosphere
  • David F. Gray, University of Western Ontario
  • Book: The Observation and Analysis of Stellar Photospheres
  • Online publication: 05 March 2015
  • Chapter DOI: https://doi.org/10.1017/CBO9781316036570.012
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  • The model photosphere
  • David F. Gray, University of Western Ontario
  • Book: The Observation and Analysis of Stellar Photospheres
  • Online publication: 05 March 2015
  • Chapter DOI: https://doi.org/10.1017/CBO9781316036570.012
Available formats
×

Save book to Google Drive

To save content items to your account, please confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your account. Find out more about saving content to Google Drive.

  • The model photosphere
  • David F. Gray, University of Western Ontario
  • Book: The Observation and Analysis of Stellar Photospheres
  • Online publication: 05 March 2015
  • Chapter DOI: https://doi.org/10.1017/CBO9781316036570.012
Available formats
×