Physics
Scientific paper
Nov 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aps..ses.ja007m&link_type=abstract
American Physical Society, 71st Annual Meeting of the Southeastern Section, 11-13 November, 2004, Oak Ridge, TN. MEETING ID: S
Physics
Scientific paper
We present arguments that Sun's polar magnetic fields, near 1 gauss strength, ascend to photosphere in polar facular increments, in accord with Fig. 1, 1 thru secular meridional circulation of both 3,600 + 25 gauss mag. toroids (as obs. at upper level) of each hemisphere, reversing polarities every 11 yr. Having been submerged to just below lower mag. toroid and traveling slightly faster there in circulatory mer. motions of Sun, which drive toroids, incipient polar faculae do not ascend with toroid at 0c = 40¢ª, but continue to higher latitudes ¡A~ 50¢ª, and now having aged by as much as one solar cycle plus ¢« 3 yr., they begin their appearance at photosphere. Ascent to photosphere requires greater travel time the greater is their lat. of vertical ascent, owing to reduced mer. circulation velocity with inc. in lat. above 40¢ª (Confer sketch of fluid motions, Fig. 1.1) Thus, polar faculae reaching photosphere at 63¢ª, where surface density increases strongly and reaches an almost constant value at 0c = 70¢ª, and that possibly extends over whole polar cap when near polar facular max., would be expected to have been formed at 40¢ª or at lesser lat. as faculae in previous sunspot cycle and would thus possess a significantly reduced observed lifetime compared to faculae in photosphere newly found below 40¢ª. Sheeley2 has counted numbers of n., s. polar faculae for period 1935-1963, 1964-1975. He finds a min. value corresponding to sunspot max. years, and conversely, so that their numbers are approx. 180¢ª out of phase with time variation of sunspot numbers for whole disk. Faculae and plages have property of being any bright regions of Sun¡¯s photosphere, seen most easily near Sun¡¯s limb and occurring most often in neighborhood of sunspots, their incandescence resulting from slow collapse of their individual engulfing mag. fields; violent turbulent eddies excise portions of toroids, including their mag. fields and transport them laterally into regions where they decay slowly owing to high electrical resistivity of neighboring gas, in absence of sustaining amplification and regenerative feedback mechanisms present in mag. toroids; always associated with passage of high speed stream, usu. supersonic, thru breach in toroid, an M-region, turbulence thus produces faculae. Waldmeir3 obs. mean diameter of polar faculae to be 2,300 km and lifetimes ranged from a few minutes to many days, which is our best evidence of extreme age. Details.4 1 McDonald, K. L., Solar-Terrestrial Electromagnetic Phenomena; ¢«¢«¢«, Bul. No. 145, Utah Engin. Expt. Sta., Univ. Utah, May 1984; 135 pp. 2 Sheeley, N. R., Jr., Ap. J., 140, No. 2, 731-735 (1964); J. Geophys. Res., 81 (19), 3462-4 (1976). 3 Waldmeir, M., ¡°Polar Fackeln¡±, Zs. F. Ap., 38, 37-54 (1955-56). 4 Kiepenheur, K. O., ¡°Solar Activity¡±, 322, in The Sun, ed. By G. P. Kuiper (Univ. Chicago Press, Ill., 1953).
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Polar Faculae Are Faculae Of Old Age, Ascending To Photosphere From Sun's Upper Magnetic Toroid Levels, And Then Descending Near Equator by 105 Km, In Their Circulatory Motion, To Depths Slightly Below That of Lower Magnetic Toroid, And Then Ascending Agai does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
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