Интенсивность эмиссионных линий короны спокойного солнца: сравнение расчетных и наблюдательных данных

Интенсивность эмиссионных линий короны спокойного солнца: сравнение расчетных и наблюдательных данных

Автор: Криссинель Б.Б.

Журнал: Солнечно-земная физика @solnechno-zemnaya-fizika

Статья в выпуске: 1 т.4, 2018 года.

Бесплатный доступ

Приведены результаты расчета центр-лимб интенсивности оптически тонких линий УФ-диапазона волн многокомпонентной модели спокойной короны Солнца. Модель представляет собой совокупность ранжированных по размерам петель, спикул и свободного (межпетельного) вещества. Теоретические значения интенсивности находятся по вероятностям встречи по линии зрения участков петель с учетом вероятности отсутствия при этом других компонент короны. В модели используются 12 петель размерами от 3200 км до 210 000 км, с различными величинами коэффициента заполнения и давления в основании и в вершине петли. Температура вершин петель - 1 400 000 K. При расчетах использована база данных CHIANTI. Сравнение теоретических и экспериментальных значений интенсивности корональных линий, а также линий переходной зоны, полученных на телескопах SUMER, CDS и EIS, показало достаточно удовлетворительное согласие их, особенно для данных центра диска Солнца. Для данных над лимбом повышенные значения расхождений в результате анализа объясняются погрешностями измерений спектрометра EIS.

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Солнце, корона, уф-излучение, атомные данные

Короткий адрес: https://sciup.org/142220272

IDR: 142220272   |   DOI: 10.12737/szf-41201802

Список литературы Интенсивность эмиссионных линий короны спокойного солнца: сравнение расчетных и наблюдательных данных

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  • DOI: :10.1051/0004-6361:20010255
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  • Brooks D.H., Warren H.P. The intercalibration of SOHO EIT, CDS-NIS, and TRACE. Astrophys. J. Suppl. Ser. 2006, vol. 164, no. 1, pp. 202-214.
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  • DOI: :10.1088/0004-637X/705/2/1522
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  • DOI: 10.1088/0004-637X/691/2/1540
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  • Doschek E.E., Laming G.A., Doschek G.A., Feldman V., Wilhelm K. A comparison of measurements of solar extreme-ultraviolet spectral line intensities emitted by C, N, O, and S ions with theoretical calculations. Astrophys. J. 1999. vol. 518, no. 2. pp. 909-917.
  • Erdely R., Doyle J.G., Perez M.E., Wilhelm K. Center-to-limb width measurements of solar chromospheric, transition region and coronal lines. Astron. Astrophys. 1998, vol. 337, pp. 287-293.
  • Feldman U. Elemental abundances in the upper solar atmosphere. Physica Scripta. 1992, vol. 46, pp. 202-220.
  • Feldman U., Mandelbaum P., Seely J.L., Doschek G.A., Gursky H. The potential for plasma diagnostics from stellar extreme-ultraviolet observations. Astron. Astrophys. Suppl. Ser. 1992, vol. 81, pp. 387-408.
  • Feldman U., Schühle U., Widing K.G., Laming J.M. Coronal composition above the solar equator and the north pole as determined from spectra acquired by the SUMER instrument on SOHO. Astrophys. J. 1998, vol. 505, no. 2, pp. 99-1006.
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  • Feldman U., Warren H.P., Brown C.M., Doschek G.A. Can then composition of the solar corona be derived from HINODE/extreme-ultraviolet imaging spectrometer spectra. Astrophys. J. 2009, vol. 695, no. 1, pp. 36-45. 10.1088/0004-637X/695/1/36
  • DOI: :10.1088/0004-637X/695/1/36
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  • Hassler D.M., Rottman G.J., Shoub E.C., Holzer T.E. Line broadening of Mg X λλ609 and 625 coronal emission lines observed above the solar limb. Astrophys. J. 1990, vol. 348, no. 1, pp. L77-L80.
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  • Krissinel B.B. Modeling of the structure of quiescent areas of the solar atmosphere emitting at 1-100 cm. Astron. Rep. 2015, vol. 59, no. 1, pp. 58-71. 10.1134/S1063772915010060
  • DOI: :10.1134/S1063772915010060
  • Laming J.M., Feldman U., Schühle U., Lemaire P., Curdt W., Wilhelm K. Electron density diagnostic for solar upper atmosphere from spectra obtained by SUMER/SOHO. Astrophys. J. 1997, vol. 485, pp. 911-919.
  • Landi E., Feldman U., Dere K.P. CHIANTI -an atomic database for emission lines. V. Comparison with an isothermal spectrum observed with SUMER. Astrophys. J. Suppl. Ser. 2002a, vol. 139, no. 1, pp. 281-296.
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  • Landi E., Feldman U. Propeerties of solar plasmas near solar maximum above two quiet regions at distance of 1.02 -1.34 Ro. Astrophys. J. 2003, vol. 592, no. 1, pp. 607-619.
  • Landi E., Del Zanna G., Young P.R., Dere K.P., Mason H.E. CHIANTI -an atomic database for emission lines. XII, Version 7 for database. Astrophys. J. 2012, vol. 744, no. 2, p. 99
  • DOI: 10.1088/0004-637X/778/1/29
  • Lantos P., Kundu M.R. The quiet Sun brightness distributions at millimeter wavelenghts and chrospheric inhomogeneties. Astron. Astrophys. 1972, vol. 21, pp. 119-124.
  • Lee H., Yun H.S., Chae J. Nonthermal broadening of UV lines observed at the limb of the quiet SUN. J. Kor. Astron. Soc. 2000, vol. 33, pp. 57-37.
  • Mariska J.T., Feldman U., Doschek G.A. Measurements of extreme-ultraviolet emission-line profilies near the solar limb. Astrophys. J. 1978, vol. 226, pp. 698-705.
  • Mariska J.T., Feldman U., Doschek G.A. Nonthermal broadening of extreme ultraviolet emission lines near Solar limb. Astron. Astrophys. 1979, vol. 73, pp. 361-363.
  • Mason H.E., Monsignori Fossi B.C. Spectroscopic diagnostic in the VUW for solar and stellar plasmas. Astron. Astrophys. Rev. 1994, vol. 6, pp. 123-173.
  • Mohan A., Landi E., Dwivedeli B.N. On the extreme-ultraviolet/ultraviolet plasma diagnostics for nitrogen-like ions from spectra obtained by SOHO/SUMER. Astrophys. J. 2003, vol. 582, no. 1, pp. 1162-1171.
  • Parenti S., Landi E., Bromage B.J.I. SOHO-ULYSSES spring 2000 quadrature: coronal diagnostic spectrometer and SUMER results. Astrophys. J. 2003, vol. 590, no. 1, pp. 519-532.
  • Peter H. Analysis of transition-region emission-line profiles from full-disk scans of the Sun using the SUMER instrument on SOHO. Astrophys. J. 1999, vol. 516, no. 1, pp. 490-504.
  • Schmelz J.T., Reames D.V., von Steiger R., Basu S. Composition of the solar corona, solar wind, and solar energetic particles. Astrophys. J. 2012, vol. 755, no. 1, p. 33-40
  • DOI: 10.1088/0004-637X/755/1/33
  • Warren H.P. Measuring the physical properties of the solar corona: results from SUMER/SOHO and TRACE. Sol. Phys. 1999, vol. 190, pp. 363-377.
  • Warren H.P., Warshall A.D. Temperature and density measurements in a quiet coronal streamer. Astrophys. J. 2002, vol. 571, no. 1, pp. 999-1007.
  • Warren H.P. A solar minimum irradiance spectrum for wavelengths below 1200Ǻ. Astrophys. J. Suppl. Ser. 2005, vol. 157, no. 1, pp. 147-173.
  • Warren H.P., Brooks D.H. The temperature and density structure of the solar corona. I. Observations of the quiet Sun with the EUV imaging spectrometer on Hinode. Astrophys. J. 2009, vol. 700, no. 2, p. 762-773
  • DOI: 10.1088/0004-637X/700/1/762
  • Wilhelm K., Lemaire P., Dammasch I.E., et al. Solar irradiances and radiances of UV and EUV lines during the minimum sunspot activity in 1996. Astron. Astrophys. 1998, vol. 334, p. 685-702.
  • Young P.R., Landi E., Thomas R.J. CHIANTI: an atomic database for emission lines. II. Comparison with the SERTS-89 active region spectrum. Astron. Astrophys. 1998, vol. 329, p. 291-314.
  • Young P.R., Del Zanna G., Mason H.E., Dere K.P., Landi E., Landini M., Doschek G.A., Brown Ch.M., Culhane L., Harra L.K., Watanabe T., Hara H. EUV emission lines and diagnostics observed with Hinode/EIS. Publ. Astron. Soc. Japan. 2007, vol. 59, p. S857-S864.
  • Zirin H., Baument B.M., Hurford G.J. The microwave brightness temperature spectrum of the quiet Sun. Astrophys. J. 1991, vol. 370, no. 1, p. 779-783.
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