A comparison of solar p-mode parameters from MDI and GONG:: Mode frequencies and structure inversions

被引:24
作者
Basu, S
Christensen-Dalsgaard, J
Howe, R
Schou, J
Thompson, MJ
Hill, F
Komm, R
机构
[1] Yale Univ, Dept Astron, New Haven, CT 06520 USA
[2] Aarhus Univ, Inst Fys & Astron, DK-8000 Aarhus C, Denmark
[3] Danmarks Grundforskningsfond, Teoret Astrofys Ctr, Aarhus, Denmark
[4] Natl Solar Observ, Tucson, AZ 85719 USA
[5] Stanford Univ, Stanford, CA 94305 USA
[6] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Space & Atmospher Phys Grp, London SW7 2BW, England
关键词
methods : data analysis; Sun : helioseismology; Sun : interior; Sun : oscillations;
D O I
10.1086/375331
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Helioseismic analysis of solar global oscillations allows investigation of the internal structure of the Sun. One important test of the reliability of the inferences from helioseismology is that the results from independent sets of contemporaneous data are consistent with one another. Here we compare mode frequencies from the Global Oscillation Network Group and Michelson Doppler Imager on board SOHO and resulting inversion results on the Sun's internal structure. The average relative differences between the data sets are typically less than 1 x 10(-5), substantially smaller than the formal errors in the differences; however, in some cases the frequency differences show a systematic behavior that might nonetheless influence the inversion results. We find that the differences in frequencies are not a result of instrumental effects but are almost entirely related to the data pipeline software. Inversion of the frequencies shows that their differences do not result in any significant effects on the resulting inferences on solar structure. We have also experimented with fitting asymmetric profiles to the oscillation power spectra and find that, compared with the symmetric fits, this causes no significant change in the inversion results.
引用
收藏
页码:432 / 445
页数:14
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