日震學：修订间差异

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2011年7月1日 (五) 11:02的版本

日震學是研究波振盪，特別是聲波壓力，在太陽上的傳播。不同於地球的地震波，太陽的波幾乎沒有剪力的成份 (S-波)。太陽壓力波被認為是接近太陽表面的對流層中的湍流生成的^[1]。有些頻率被建設性的干涉放大，換言之，太陽振盪的環像是一個鐘，聲波傳輸到太陽更表面的光球層，這是從太陽中心的核融合輻射出的能量經由吸收生成可見光，離開太陽表面的區域。這些振盪幾乎在任何時間序列的的太陽影像上都能檢測得到，但觀測到最好的影像是測量都卜勒位移的光球吸收譜線。經由太陽振盪波的傳播的變化，揭露了太陽內部的結構，並讓天文物理學家發展出太陽內部剖面極為詳細的設定條件。

日震學可以排除太陽微中子問題是由於太陽內部模型不正確的可能性^[2] 日震學揭示的特性包括外側的對流層和內側的輻射層以不同的速度旋轉，這引發太陽發電機產生磁場效應的想法^[3]^[4]，和在太陽表面對流層下的數千公里有電漿"噴流" (更明確的說，扭轉振盪) ^[5]。這些噴流從赤道廣泛的散播，在高緯度地區分解成小旋風的風暴。扭轉振盪是太陽較差自轉時間的變化，它們的交錯影響旋轉快與慢的帶。到目前為止，還沒有被普遍接受的理論能解釋，即使它們與太陽週期的密切關係很明顯，一樣有著11年的周期，而這是我們在1980年就已經發現的^[6]。

日枕學也可以用來生成從地球看在太陽背面，包括太陽黑子的影像^[7]。 including sunspots. In simple terms, sunspots absorb helioseismic waves. This sunspot absorption causes a seismic deficit that can be imaged at the antipode of the sunspot.^[8]。為方便太空氣象的預測，從2000年晚期，經由SOHO衛星就有部分太陽背面中央地區的日震影像圖不停的被產生，而從2001年起，全部的背面影像都被生成和進行資料分析。

請記住，不論名稱是如何，日震學是研究太陽的波動，而不是太陽的地震活動－沒有這一回事。名稱是源自類似研究地震波以確定地球內部的結構。在科學上可以和星震學對照，這是研究在恆星傳播的聲波。

太陽振盪的類型

參考資料

^ Goldreich, P.; Keeley, D.A. Solar seismology. II - The stochastic excitation of the solar p-modes by turbulent convection. Astrophysical Journal. February 1977, 212: 243–251. Bibcode:1977ApJ...212..243G. doi:10.1086/155043.
^ Bahcall, J.N.; Pinsonneault, M.H.; Basu, S.; Christensen-Dalsgaard, J. Are Standard Solar Models Reliable?. Physical Review Letters. January 1997, 78 (2): 171–174. Bibcode:1997PhRvL..78..171B. arXiv:astro-ph/9610250 . doi:10.1103/PhysRevLett.78.171.
^ Thompson, M.J.; Christensen-Dalsgaard, J.; Miesch, M.S.; Toomre, J. The Internal Rotation of the Sun. Annual Review of Astronomy & Astrophysics. 2003, 41 (1): 599–643. Bibcode:2003ARA&A..41..599T. doi:10.1146/annurev.astro.41.011802.094848.
^ Ossendrijver, M. The solar dynamo. The Astronomy and Astrophysics Review. 2003, 11 (4): 287–367. Bibcode:2003A&ARv..11..287O. doi:10.1007/s00159-003-0019-3.
^ Vorontsov, S.V.; Christensen-Dalsgaard, J.; Schou, J.; Strakhov, V.N.; Thompson, M.J. Helioseismic Measurement of Solar Torsional Oscillations. Science. April 2002, 296 (5565): 101–103. Bibcode:2002Sci...296..101V. PMID 11935019. doi:10.1126/science.1069190.
^ Howard, R.; Labonte, B.J. The sun is observed to be a torsional oscillator with a period of 11 years. Astrophysical Journal. July 1980, 239: L33–L36. Bibcode:1980ApJ...239L..33H. doi:10.1086/183286.
^ Braun, D.C.; Lindsey, C. Seismic Imaging of the Far Hemisphere of the Sun. The Astrophysical Journal. October 2001, 560 (2): L189–L192. Bibcode:2001ApJ...560L.189B. doi:10.1086/324323.
^ Lindsey, C.; Braun, D.C. Helioseismic imaging of sunspots at their antipodes. Solar Physics. March 1990, 126 (1): 101–115. Bibcode:1990SoPh..126..101L. doi:10.1007/BF00158301.

外部鏈結

Non-technical description of helio- and asteroseismology retrieved November 2009
Laurent Gizon and Aaron C. Birch, "Local Helioseismology", Living Rev. Solar Phys. 2 (2005) 6 online article
Scientists Issue Unprecedented Forecast of Next Sunspot Cycle National Science Foundation press release, March 6, 2006
Large-Scale Dynamics of the Convection Zone and Tachocline by Mark S. Miesch
European Helio- and Asteroseismology Network (HELAS)
Farside and Earthside images of the Sun
Living Reviews in Solar Physics

衛星的儀器

地面基地的儀器

BiSON
Mark-1
GONG
HiDHN

[Keeley1977-1] Goldreich, P.; Keeley, D.A. Solar seismology. II - The stochastic excitation of the solar p-modes by turbulent convection. Astrophysical Journal. February 1977, 212: 243–251. Bibcode:1977ApJ...212..243G. doi:10.1086/155043.

[Bahcall1997-2] Bahcall, J.N.; Pinsonneault, M.H.; Basu, S.; Christensen-Dalsgaard, J. Are Standard Solar Models Reliable?. Physical Review Letters. January 1997, 78 (2): 171–174. Bibcode:1997PhRvL..78..171B. arXiv:astro-ph/9610250 . doi:10.1103/PhysRevLett.78.171.

[Thompson2003-3] Thompson, M.J.; Christensen-Dalsgaard, J.; Miesch, M.S.; Toomre, J. The Internal Rotation of the Sun. Annual Review of Astronomy & Astrophysics. 2003, 41 (1): 599–643. Bibcode:2003ARA&A..41..599T. doi:10.1146/annurev.astro.41.011802.094848.

[4] Ossendrijver, M. The solar dynamo. The Astronomy and Astrophysics Review. 2003, 11 (4): 287–367. Bibcode:2003A&ARv..11..287O. doi:10.1007/s00159-003-0019-3.

[5] Vorontsov, S.V.; Christensen-Dalsgaard, J.; Schou, J.; Strakhov, V.N.; Thompson, M.J. Helioseismic Measurement of Solar Torsional Oscillations. Science. April 2002, 296 (5565): 101–103. Bibcode:2002Sci...296..101V. PMID 11935019. doi:10.1126/science.1069190.

[6] Howard, R.; Labonte, B.J. The sun is observed to be a torsional oscillator with a period of 11 years. Astrophysical Journal. July 1980, 239: L33–L36. Bibcode:1980ApJ...239L..33H. doi:10.1086/183286.

[Braun2001-7] Braun, D.C.; Lindsey, C. Seismic Imaging of the Far Hemisphere of the Sun. The Astrophysical Journal. October 2001, 560 (2): L189–L192. Bibcode:2001ApJ...560L.189B. doi:10.1086/324323.

[8] Lindsey, C.; Braun, D.C. Helioseismic imaging of sunspots at their antipodes. Solar Physics. March 1990, 126 (1): 101–115. Bibcode:1990SoPh..126..101L. doi:10.1007/BF00158301.

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