![]() Steenbock, W.: 1985, in Cool Stars with Excesses of Heavy Elements, M. (Eds.), University of Arizona press, Tucson, AZ, p. Spruit, H.C., Schüssler, M., and Solanki, S.K.: 1992, in Solar Interior and Atmosphere, A.N. Solanki, S.K., Zuffrey, D., Lin, H., Rüedi, I., and Kuhn, J.: 1996b, Astron. Solanki, S.K., Rüedi, I., Bianda, M., and Steffen, M.: 1996a, Astron. Schüssler, M.: 1992, in The Sun - a Laboratory for Astrophysics, J.T. Viotti (Ed.), Reidel, Dordrecht IAU Coll. Rutten, R.J.: 1988, in Physics of Formation of Fe II Lines Outside LTE, R. Rast, M.P., Nordlund, Å., Stein, R.F., and Toomre, J.: 1993, Astrophys. Nordlund, Å.: 1985, in Theoretical Problems in High Resolution Solar Physics, H.U. Keil (Ed.), National Solar Obs., Sunspot, NM, p. Nordlund, Å.: 1984, in Small-Scale Dynamical Processes in Quiet Stellar Atmospheres, S.L. Muller, R.: 1989, in Solar and Stellar Granulation, R.J. Meunier, N., Solanki, S.K., and Livingston, W.C.: 1998, Astron. Malagoli, A., Cattaneo, F., and Brumell, N.H.: 1990, Astrophys. Lites, B.W., Nordlund, Å., and Scharmer, G.B.: 1989, in Solar and Stellar Granulation, R.J. Kurucz, R.L.: 1991, in Precision Photometry: Astrophysics of the Galaxy, A.G. ![]() Komm, R., Mattig, W., and Ncsis, A.: 1990, Astron. Karpinsky, V.N.: 1990, in Solar Photosphere: Structure, Convection and Magnetic Fields, J.O. Holweger, H., Heise, C., and Kock, M.: 1990, Astron. Spite (Eds.), Kluwer, Dordrecht IAU Symp. Holweger, H.: 1988, in The Impact of Very High S/N Spectroscopy on Stellar Physics, G. Grevesse, N., and Sauval, A.J.: 1998, Space Sci. Gadun, A., Solanki, S.K., and Johannesson, A.: 1998, Astron. Gadun, A.S., Hanslmeier, A., and Pikalov, K.N.: 1997, Astron. 265, 257.įaurobert-School, M., Feautrier, N., Machefert, F., Petrovay, K., and Spielfiedel, A.: 1995, Astron. von der Lühe (Ed.), National Solar Observatory, Sunspot, NM, p. 23, 37.īonnacini, D.: 1989, in High Spatial Resolution Solar Observations, O. Lites (Ed.), National Solar Obs., Sunspot, NM, p. 339, 558.Īvrett, E.H.: 1985, in Chromospheric Diagnostics and Modelling, B.W. Animated explanation of the temperature of the Photosphere (University of South Wales).Anderson, L.S.: 1989, Astrophys.Animated explanation of the Photosphere (University of South Wales).Media related to Photosphere at Wikimedia Commons. ![]() "SP-402 A New Sun: The Solar Results From Skylab". Monthly Notices of the Royal Astronomical Society. "Heterogeneity of solid neutron-star matter: Transport coefficients and neutrino emissivity". "Nature of Fault Planes in Solid Neutron Star Matter". "Whole Earth Telescope observations of BPM 37093: A seismological test of crystallization theory in white dwarfs". ![]() These features are too fine to be directly observed on other stars however, sunspots have been indirectly observed, in which case they are referred to as starspots. Other magnetically-related phenomena in the Sun's photosphere include sunspots and solar faculae dispersed between granules. Grouping the typical granules are supergranules up to 30,000 kilometers (19,000 mi) in diameter with lifespans of up to 24 hours and flow speeds of about 500 meters per second (1,600 ft/s), carrying magnetic field bundles to the edges of the cells. Each granule has a lifespan of only about twenty minutes, resulting in a continually shifting "boiling" pattern. In the Sun's photosphere, the most ubiquitous phenomena are granules- convection cells of plasma each approximately 1,000 kilometers (620 mi) in diameter with hot rising plasma in the center and cooler plasma falling in the spaces between them, flowing at velocities of 7 kilometers per second (4.3 mi/s). ![]()
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