The solar acoustic spectrum and eigenmode parameters

Science

Volumn 272, Issue 5266, 1996, Pages 1292-1295

  Hill, F ^a   Stark, P B ^a   Stebbins, R T ^a   Anderson, E R ^a   Antia, H M ^a   Brown, T M ^a   Duvall Jr , T L ^a   Haber, D A ^a   Harvey, J W ^a   Hathaway, D H ^a   Howe, R ^a   Hubbard, R P ^a   Jones, H P ^a   Kennedy, J R ^a   Korzennik, S G ^a   Kosovichev, A G ^a   Leibacher, J W ^a   Libbrecht, K G ^a   Pintar, J A ^a   Rhodes Jr , E J ^a   Schou, J ^a   Thompson, M J ^a   Tomczyk, S ^a   Toner, C G ^a   Toussaint, R ^a   Williams, W E ^a   more..

^a NONE

Author keywords

[No Author keywords available]

Indexed keywords

ACOUSTIC SPECTRUM; GLOBAL OSCILLATION NETWORK GROUP; HELIOSEISMOLOGY;

SUN;

EID: 0029731277     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.272.5266.1292     Document Type: Article

References (32)

1. External sources include other solar velocity fields, attenuation of the oscillations in active regions, terrestrial atmospheric transparency variations (including birds and other opaque objects in the field of view), and seeing and atmospheric scattering.
2. Instrumental sources include prefilter nonlinearity and drift, image rotator encoder errors, spatial aliasing, spurious modulation, camera nonlinearity and zero-level variations, nonlinearity of velocity and intensity during integration, and image cache differences.
3. Data processing sources include calibration; image geometry determination; remapping of residuals from refraction, line-of-sight velocity projection, and pixellation; ephemeris errors; spherical harmonic approximation to true eigenfunctions; merging errors from MTF approximation and velocity scale factors; gap-filling; and peak fitting (leakage, parametric model, and algorithm).
4. E. Anderson, T. Duvall, S. Jefferies, Astrophys. J. 364,699 (1990). For other approaches to estimating mode parameters, see S. Korzennik, thesis, University of California at Los Angeles (1990); J. Schou, thesis, University of Aarhus (1992); J. Patron, thesis, Universidad de La Laguna (1994); and (12).
5. E. Anderson, T. Duvall, S. Jefferies, Astrophys. J. 364,699 (1990). For other approaches to estimating mode parameters, see S. Korzennik, thesis, University of California at Los Angeles (1990); J. Schou, thesis, University of Aarhus (1992); J. Patron, thesis, Universidad de La Laguna (1994); and (12).
6. E. Anderson, T. Duvall, S. Jefferies, Astrophys. J. 364,699 (1990). For other approaches to estimating mode parameters, see S. Korzennik, thesis, University of California at Los Angeles (1990); J. Schou, thesis, University of Aarhus (1992); J. Patron, thesis, Universidad de La Laguna (1994); and (12).
7. E. Anderson, T. Duvall, S. Jefferies, Astrophys. J. 364,699 (1990). For other approaches to estimating mode parameters, see S. Korzennik, thesis, University of California at Los Angeles (1990); J. Schou, thesis, University of Aarhus (1992); J. Patron, thesis, Universidad de La Laguna (1994); and (12).
8. M. J. Thompson et al., Science 272, 1300 (1996), and references therein.
9. D. O. Gough et al., ibid, p. 1296, and references therein.
10. Observations indicate substantial deviations of the line profile from a symmetrical Lorentzian shape. The line asymmetry is particularly pronounced for low- and high-frequency p modes. The degree of the asymmetry depends on the location of the excitation sources of oscillations relative to the mode resonant cavity [T. L. Duvall Jr. et al., Astrophys. J. 410, 829 (1993); M. Gabriel, Astron. Astrophys. 299, 245 (1995)].
11. Observations indicate substantial deviations of the line profile from a symmetrical Lorentzian shape. The line asymmetry is particularly pronounced for low- and high-frequency p modes. The degree of the asymmetry depends on the location of the excitation sources of oscillations relative to the mode resonant cavity [T. L. Duvall Jr. et al., Astrophys. J. 410, 829 (1993); M. Gabriel, Astron. Astrophys. 299, 245 (1995)].
12. Observational helioseismology has an extensive literature. A short list of representative papers from other observational efforts in the last decade is given. Big Bear Solar Observatory: (13); National Solar Observatory (NSO)-South Pole: T. L. Duvall Jr. et al., Astrophys. J. 324, 1158 (1988); Mount Wilson-Univ. ot Southern California (USC): (14); Birmingham Solar Oscillation Network (BiSON): Y. Elsworth et al., Astrophys. J. 434, 801 (1994); Université de Nice International Research on the Interior of the SUN (IRIS) Network: S. Loudagh et al., Astron. Astrophys. 275, L25 (1993); HAO Fourier Tachometer; K. T. Bachmann, J. Schou, T. Brown, Astrophys. J. 412, 870 (1993); NSO-High-t Helioseismometer: (12); Univ. of Hawaii Photometric Oscillations Imager: R. S. Ronan and B. J. LaBonte, Sol. Phys. 149, 1 (1994); Taiwanese Oscillations Network (TON): D.-Y. Chou et al., ibid. 160, 237 (1995); LOWL: (15).
13. Observational helioseismology has an extensive literature. A short list of representative papers from other observational efforts in the last decade is given. Big Bear Solar Observatory: (13); National Solar Observatory (NSO)-South Pole: T. L. Duvall Jr. et al., Astrophys. J. 324, 1158 (1988); Mount Wilson-Univ. ot Southern California (USC): (14); Birmingham Solar Oscillation Network (BiSON): Y. Elsworth et al., Astrophys. J. 434, 801 (1994); Université de Nice International Research on the Interior of the SUN (IRIS) Network: S. Loudagh et al., Astron. Astrophys. 275, L25 (1993); HAO Fourier Tachometer; K. T. Bachmann, J. Schou, T. Brown, Astrophys. J. 412, 870 (1993); NSO-High-t Helioseismometer: (12); Univ. of Hawaii Photometric Oscillations Imager: R. S. Ronan and B. J. LaBonte, Sol. Phys. 149, 1 (1994); Taiwanese Oscillations Network (TON): D.-Y. Chou et al., ibid. 160, 237 (1995); LOWL: (15).
14. Observational helioseismology has an extensive literature. A short list of representative papers from other observational efforts in the last decade is given. Big Bear Solar Observatory: (13); National Solar Observatory (NSO)-South Pole: T. L. Duvall Jr. et al., Astrophys. J. 324, 1158 (1988); Mount Wilson-Univ. ot Southern California (USC): (14); Birmingham Solar Oscillation Network (BiSON): Y. Elsworth et al., Astrophys. J. 434, 801 (1994); Université de Nice International Research on the Interior of the SUN (IRIS) Network: S. Loudagh et al., Astron. Astrophys. 275, L25 (1993); HAO Fourier Tachometer; K. T. Bachmann, J. Schou, T. Brown, Astrophys. J. 412, 870 (1993); NSO-High-t Helioseismometer: (12); Univ. of Hawaii Photometric Oscillations Imager: R. S. Ronan and B. J. LaBonte, Sol. Phys. 149, 1 (1994); Taiwanese Oscillations Network (TON): D.-Y. Chou et al., ibid. 160, 237 (1995); LOWL: (15).
15. Observational helioseismology has an extensive literature. A short list of representative papers from other observational efforts in the last decade is given. Big Bear Solar Observatory: (13); National Solar Observatory (NSO)-South Pole: T. L. Duvall Jr. et al., Astrophys. J. 324, 1158 (1988); Mount Wilson-Univ. ot Southern California (USC): (14); Birmingham Solar Oscillation Network (BiSON): Y. Elsworth et al., Astrophys. J. 434, 801 (1994); Université de Nice International Research on the Interior of the SUN (IRIS) Network: S. Loudagh et al., Astron. Astrophys. 275, L25 (1993); HAO Fourier Tachometer; K. T. Bachmann, J. Schou, T. Brown, Astrophys. J. 412, 870 (1993); NSO-High-t Helioseismometer: (12); Univ. of Hawaii Photometric Oscillations Imager: R. S. Ronan and B. J. LaBonte, Sol. Phys. 149, 1 (1994); Taiwanese Oscillations Network (TON): D.-Y. Chou et al., ibid. 160, 237 (1995); LOWL: (15).
16. Observational helioseismology has an extensive literature. A short list of representative papers from other observational efforts in the last decade is given. Big Bear Solar Observatory: (13); National Solar Observatory (NSO)-South Pole: T. L. Duvall Jr. et al., Astrophys. J. 324, 1158 (1988); Mount Wilson-Univ. ot Southern California (USC): (14); Birmingham Solar Oscillation Network (BiSON): Y. Elsworth et al., Astrophys. J. 434, 801 (1994); Université de Nice International Research on the Interior of the SUN (IRIS) Network: S. Loudagh et al., Astron. Astrophys. 275, L25 (1993); HAO Fourier Tachometer; K. T. Bachmann, J. Schou, T. Brown, Astrophys. J. 412, 870 (1993); NSO-High-t Helioseismometer: (12); Univ. of Hawaii Photometric Oscillations Imager: R. S. Ronan and B. J. LaBonte, Sol. Phys. 149, 1 (1994); Taiwanese Oscillations Network (TON): D.-Y. Chou et al., ibid. 160, 237 (1995); LOWL: (15).
17. Observational helioseismology has an extensive literature. A short list of representative papers from other observational efforts in the last decade is given. Big Bear Solar Observatory: (13); National Solar Observatory (NSO)-South Pole: T. L. Duvall Jr. et al., Astrophys. J. 324, 1158 (1988); Mount Wilson-Univ. ot Southern California (USC): (14); Birmingham Solar Oscillation Network (BiSON): Y. Elsworth et al., Astrophys. J. 434, 801 (1994); Université de Nice International Research on the Interior of the SUN (IRIS) Network: S. Loudagh et al., Astron. Astrophys. 275, L25 (1993); HAO Fourier Tachometer; K. T. Bachmann, J. Schou, T. Brown, Astrophys. J. 412, 870 (1993); NSO-High-t Helioseismometer: (12); Univ. of Hawaii Photometric Oscillations Imager: R. S. Ronan and B. J. LaBonte, Sol. Phys. 149, 1 (1994); Taiwanese Oscillations Network (TON): D.-Y. Chou et al., ibid. 160, 237 (1995); LOWL: (15).
18. Big Bear Solar Observatory: (13); LOWL: (15); Mount Wilson-USC: (14).
19. The frequencies of the p modes increase as the surface activity increases. The frequency shift depends on v and is about 0.4 μHz for v ≈ 3 mHz. The shift is thought to result from a combination of magnetic and temperature effects. Observational papers on the subject include M. F. Woodard and R. W. Noyes, Nature 318, 449 (1985); E. J. Rhodes Jr. et al., Astrophys. J. 326, 479 (1988); K. G. Libbrecht and M. F. Woodard, Nature 345, 779 (1990); Y. Elsworth et al., ibid., p. 322; M. Anguera Gubau et al., Astron. Astrophys. 255, 363 (1992); and K. T. Bachmann and T. M. Brown, Astrophys. J. 411, L45 (1993). There is also evidence for a solar cycle variation in Γ [S. M. Jefferies et al., Astrophys. J. 377, 330 (1991)] and in A (Y. Elsworth et al., Mon. Not. R Astron. Soc. 265, 888 (1993)].
20. The frequencies of the p modes increase as the surface activity increases. The frequency shift depends on v and is about 0.4 μHz for v ≈ 3 mHz. The shift is thought to result from a combination of magnetic and temperature effects. Observational papers on the subject include M. F. Woodard and R. W. Noyes, Nature 318, 449 (1985); E. J. Rhodes Jr. et al., Astrophys. J. 326, 479 (1988); K. G. Libbrecht and M. F. Woodard, Nature 345, 779 (1990); Y. Elsworth et al., ibid., p. 322; M. Anguera Gubau et al., Astron. Astrophys. 255, 363 (1992); and K. T. Bachmann and T. M. Brown, Astrophys. J. 411, L45 (1993). There is also evidence for a solar cycle variation in Γ [S. M. Jefferies et al., Astrophys. J. 377, 330 (1991)] and in A (Y. Elsworth et al., Mon. Not. R Astron. Soc. 265, 888 (1993)].
21. The frequencies of the p modes increase as the surface activity increases. The frequency shift depends on v and is about 0.4 μHz for v ≈ 3 mHz. The shift is thought to result from a combination of magnetic and temperature effects. Observational papers on the subject include M. F. Woodard and R. W. Noyes, Nature 318, 449 (1985); E. J. Rhodes Jr. et al., Astrophys. J. 326, 479 (1988); K. G. Libbrecht and M. F. Woodard, Nature 345, 779 (1990); Y. Elsworth et al., ibid., p. 322; M. Anguera Gubau et al., Astron. Astrophys. 255, 363 (1992); and K. T. Bachmann and T. M. Brown, Astrophys. J. 411, L45 (1993). There is also evidence for a solar cycle variation in Γ [S. M. Jefferies et al., Astrophys. J. 377, 330 (1991)] and in A (Y. Elsworth et al., Mon. Not. R Astron. Soc. 265, 888 (1993)].
22. The frequencies of the p modes increase as the surface activity increases. The frequency shift depends on v and is about 0.4 μHz for v ≈ 3 mHz. The shift is thought to result from a combination of magnetic and temperature effects. Observational papers on the subject include M. F. Woodard and R. W. Noyes, Nature 318, 449 (1985); E. J. Rhodes Jr. et al., Astrophys. J. 326, 479 (1988); K. G. Libbrecht and M. F. Woodard, Nature 345, 779 (1990); Y. Elsworth et al., ibid., p. 322; M. Anguera Gubau et al., Astron. Astrophys. 255, 363 (1992); and K. T. Bachmann and T. M. Brown, Astrophys. J. 411, L45 (1993). There is also evidence for a solar cycle variation in Γ [S. M. Jefferies et al., Astrophys. J. 377, 330 (1991)] and in A (Y. Elsworth et al., Mon. Not. R Astron. Soc. 265, 888 (1993)].
23. The frequencies of the p modes increase as the surface activity increases. The frequency shift depends on v and is about 0.4 μHz for v ≈ 3 mHz. The shift is thought to result from a combination of magnetic and temperature effects. Observational papers on the subject include M. F. Woodard and R. W. Noyes, Nature 318, 449 (1985); E. J. Rhodes Jr. et al., Astrophys. J. 326, 479 (1988); K. G. Libbrecht and M. F. Woodard, Nature 345, 779 (1990); Y. Elsworth et al., ibid., p. 322; M. Anguera Gubau et al., Astron. Astrophys. 255, 363 (1992); and K. T. Bachmann and T. M. Brown, Astrophys. J. 411, L45 (1993). There is also evidence for a solar cycle variation in Γ [S. M. Jefferies et al., Astrophys. J. 377, 330 (1991)] and in A (Y. Elsworth et al., Mon. Not. R Astron. Soc. 265, 888 (1993)].
24. The frequencies of the p modes increase as the surface activity increases. The frequency shift depends on v and is about 0.4 μHz for v ≈ 3 mHz. The shift is thought to result from a combination of magnetic and temperature effects. Observational papers on the subject include M. F. Woodard and R. W. Noyes, Nature 318, 449 (1985); E. J. Rhodes Jr. et al., Astrophys. J. 326, 479 (1988); K. G. Libbrecht and M. F. Woodard, Nature 345, 779 (1990); Y. Elsworth et al., ibid., p. 322; M. Anguera Gubau et al., Astron. Astrophys. 255, 363 (1992); and K. T. Bachmann and T. M. Brown, Astrophys. J. 411, L45 (1993). There is also evidence for a solar cycle variation in Γ [S. M. Jefferies et al., Astrophys. J. 377, 330 (1991)] and in A (Y. Elsworth et al., Mon. Not. R Astron. Soc. 265, 888 (1993)].
25. The frequencies of the p modes increase as the surface activity increases. The frequency shift depends on v and is about 0.4 μHz for v ≈ 3 mHz. The shift is thought to result from a combination of magnetic and temperature effects. Observational papers on the subject include M. F. Woodard and R. W. Noyes, Nature 318, 449 (1985); E. J. Rhodes Jr. et al., Astrophys. J. 326, 479 (1988); K. G. Libbrecht and M. F. Woodard, Nature 345, 779 (1990); Y. Elsworth et al., ibid., p. 322; M. Anguera Gubau et al., Astron. Astrophys. 255, 363 (1992); and K. T. Bachmann and T. M. Brown, Astrophys. J. 411, L45 (1993). There is also evidence for a solar cycle variation in Γ [S. M. Jefferies et al., Astrophys. J. 377, 330 (1991)] and in A (Y. Elsworth et al., Mon. Not. R Astron. Soc. 265, 888 (1993)].
26. The frequencies of the p modes increase as the surface activity increases. The frequency shift depends on v and is about 0.4 μHz for v ≈ 3 mHz. The shift is thought to result from a combination of magnetic and temperature effects. Observational papers on the subject include M. F. Woodard and R. W. Noyes, Nature 318, 449 (1985); E. J. Rhodes Jr. et al., Astrophys. J. 326, 479 (1988); K. G. Libbrecht and M. F. Woodard, Nature 345, 779 (1990); Y. Elsworth et al., ibid., p. 322; M. Anguera Gubau et al., Astron. Astrophys. 255, 363 (1992); and K. T. Bachmann and T. M. Brown, Astrophys. J. 411, L45 (1993). There is also evidence for a solar cycle variation in Γ [S. M. Jefferies et al., Astrophys. J. 377, 330 (1991)] and in A (Y. Elsworth et al., Mon. Not. R Astron. Soc. 265, 888 (1993)].
27. P. H. Scherrer et al., Sol. Phys. 162, 129 (1995).
28. K. T, Bachmann, T. L. Duvall Jr., J. W. Harvey, F. Hill, Astrophys. J. 443, 837 (1995).
29. K. G. Libbrecht, M. F. Woodard, J. M. Kaufman, Astrophys. J. Suppl. Ser. 74, 1129 (1990).
30. E. J. Rhodes Jr., A. Cacciani, S. G. Korzennik, Adv. Space Res. 11, 17 (1991).
31. S. Tomczyk et al., Sol. Phys. 159, 1 (1995).
32. The GONG project is managed by NSO, a division of the NOAO, which is operated by the Association of Universities for Research in Astronomy under a cooperative agreement with NSF. The data were acquired by instruments operated by Big Bear Solar Observatory, HAO, Learmouth Solar Observatory, Udaipur Solar Observatory, Instituto de Astrofisica de Canarias, and Cerro Tololo Interamerican Observatory.