The Global Oscillation Network Group (GONG) project

Science

Volumn 272, Issue 5266, 1996, Pages 1284-1286

  Harvey, J W ^a   Hill, F ^a   Hubbard, R P ^a   Kennedy, J R ^a   Leibacher, J W ^a   Pintar, J A ^a   Gilman, P A ^b   Noyes, R W ^c   Title, A M ^d   Toomre, J ^e   Ulrich, R K ^f   Bhatnagar, A ^g   Kennewell, J A ^h   Marquette, W ^i,j   Patron J ^k   Saa O ^l   Yasukawa, E ^b,m  

^a NATIONAL SOLAR OBSERVATORY   (United States)

^b NATIONAL CENTER FOR ATMOSPHERIC RESEARCH   (United States)

^c SMITHSONIAN ASTROPHYSICAL OBSERVATORY   (United States)

^d LOCKHEED MARTIN   (United States)

^e UNIVERSITY OF COLORADO   (United States)

^f UNIVERSITY OF CALIFORNIA   (United States)

^g PHYSICAL RESEARCH LABORATORY   (India)

^h BUREAU OF METEOROLOGY   (Australia)

ⁱ NEW JERSEY INSTITUTE OF TECHNOLOGY   (United States)

^j CALIFORNIA INSTITUTE OF TECHNOLOGY   (United States)

^k INSTITUTO DE ASTROFÍSICA DE CANARIAS   (Spain)

^l CERRO TOLOLO INTER AMERICAN OBSERVATORY   (Chile)

^m Mauna Loa Observatory   (United States)

more..

Author keywords

[No Author keywords available]

Indexed keywords

GLOBAL OSCILLATION NETWORK GROUP; HELIOSEISMOLOGY; SOLAR SURFACE; STELLAR STRUCTURE;

SUN;

EID: 0029751637     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.272.5266.1284     Document Type: Article

References (27)

1. The original papers providing the theoretical under-pinnings of the oscillations are R. Ulrich, Astrophys. J. 162, 993 (1970); J. W. Leibacher and R, F. Stein, Astrophys. Lett. 7, 191 (1971); C. L. Wolff, Astrophys. J. 177, L87 (1972). For more recent reviews of the subject, see D. O. Gough and J. Toomre, Annu. Rev. Astron. Astrophys. 29, 627 (1991); A. N. Cox, W. C. Livingston, M. S. Matthews, Eds., Solar Interior and Atmosphere (Univ. of Arizona Press, Tucson, 1991), pp. 329-660; W. Unno, Y.Osaki, H. Ando, H. Saio, H. Shibahashi, Nonradial Oscillations of Stars (Univ. of Tokyo Press, Tokyo, 1989).
2. The original papers providing the theoretical under-pinnings of the oscillations are R. Ulrich, Astrophys. J. 162, 993 (1970); J. W. Leibacher and R, F. Stein, Astrophys. Lett. 7, 191 (1971); C. L. Wolff, Astrophys. J. 177, L87 (1972). For more recent reviews of the subject, see D. O. Gough and J. Toomre, Annu. Rev. Astron. Astrophys. 29, 627 (1991); A. N. Cox, W. C. Livingston, M. S. Matthews, Eds., Solar Interior and Atmosphere (Univ. of Arizona Press, Tucson, 1991), pp. 329-660; W. Unno, Y.Osaki, H. Ando, H. Saio, H. Shibahashi, Nonradial Oscillations of Stars (Univ. of Tokyo Press, Tokyo, 1989).
3. The original papers providing the theoretical under-pinnings of the oscillations are R. Ulrich, Astrophys. J. 162, 993 (1970); J. W. Leibacher and R, F. Stein, Astrophys. Lett. 7, 191 (1971); C. L. Wolff, Astrophys. J. 177, L87 (1972). For more recent reviews of the subject, see D. O. Gough and J. Toomre, Annu. Rev. Astron. Astrophys. 29, 627 (1991); A. N. Cox, W. C. Livingston, M. S. Matthews, Eds., Solar Interior and Atmosphere (Univ. of Arizona Press, Tucson, 1991), pp. 329-660; W. Unno, Y.Osaki, H. Ando, H. Saio, H. Shibahashi, Nonradial Oscillations of Stars (Univ. of Tokyo Press, Tokyo, 1989).
4. The original papers providing the theoretical under-pinnings of the oscillations are R. Ulrich, Astrophys. J. 162, 993 (1970); J. W. Leibacher and R, F. Stein, Astrophys. Lett. 7, 191 (1971); C. L. Wolff, Astrophys. J. 177, L87 (1972). For more recent reviews of the subject, see D. O. Gough and J. Toomre, Annu. Rev. Astron. Astrophys. 29, 627 (1991); A. N. Cox, W. C. Livingston, M. S. Matthews, Eds., Solar Interior and Atmosphere (Univ. of Arizona Press, Tucson, 1991), pp. 329-660; W. Unno, Y.Osaki, H. Ando, H. Saio, H. Shibahashi, Nonradial Oscillations of Stars (Univ. of Tokyo Press, Tokyo, 1989).
5. The original papers providing the theoretical under-pinnings of the oscillations are R. Ulrich, Astrophys. J. 162, 993 (1970); J. W. Leibacher and R, F. Stein, Astrophys. Lett. 7, 191 (1971); C. L. Wolff, Astrophys. J. 177, L87 (1972). For more recent reviews of the subject, see D. O. Gough and J. Toomre, Annu. Rev. Astron. Astrophys. 29, 627 (1991); A. N. Cox, W. C. Livingston, M. S. Matthews, Eds., Solar Interior and Atmosphere (Univ. of Arizona Press, Tucson, 1991), pp. 329-660; W. Unno, Y.Osaki, H. Ando, H. Saio, H. Shibahashi, Nonradial Oscillations of Stars (Univ. of Tokyo Press, Tokyo, 1989).
6. The original papers providing the theoretical under-pinnings of the oscillations are R. Ulrich, Astrophys. J. 162, 993 (1970); J. W. Leibacher and R, F. Stein, Astrophys. Lett. 7, 191 (1971); C. L. Wolff, Astrophys. J. 177, L87 (1972). For more recent reviews of the subject, see D. O. Gough and J. Toomre, Annu. Rev. Astron. Astrophys. 29, 627 (1991); A. N. Cox, W. C. Livingston, M. S. Matthews, Eds., Solar Interior and Atmosphere (Univ. of Arizona Press, Tucson, 1991), pp. 329-660; W. Unno, Y.Osaki, H. Ando, H. Saio, H. Shibahashi, Nonradial Oscillations of Stars (Univ. of Tokyo Press, Tokyo, 1989).
7. J. W. Harvey, AIP Conf. Proc. 189, 227 (1989).
8. P. H. Scherrer et al., Sol. Phys. 162, 129 (1995).
9. Y. Elsworth et al., Astron. Soc. Pac. Conf. Ser. 76, 392 (1995).
10. E. Fossat, Sol. Phys. 133, 1 (1991).
11. D. Y. Chou et al., ibid. 160, 237 (1995).
12. E. J. Rhodes Jr. et al., Astron. Soc. Pac. Conf. Ser. 76, 398 (1995).
13. F. Hill and G. Newkirk Jr., Sol. Phys. 95, 201 (1985).
14. F. Hill et al., ibid. 152, 321 (1994); ibid., p. 351.
15. F. Hill et al., ibid. 152, 321 (1994); ibid., p. 351.
16. J. W. Harvey et al., in preparation.
17. J. Beckers and T. M. Brown, Oss. Mem. Oss. Astrofis. Arcetri 106, 189, (1978).
18. F. Hill et al., in preparation.
19. R. Toussaint, J. W. Harvey, R. P. Hubbard, Astron. Soc. Pac. Conf. Ser. 76, 532 (1995).
20. T. Brown, in Advances in Helio- and Asteroseismology, J. Christensen-Dalsgaard and S. Frandsen, Eds. (Reidel, Dordrecht, 1988), pp. 453-465.
21. The time series from each site-day, scaled to compensate for variations in image resolution from seeing and other effects, are merged to form a longer, more nearly continuous time series. The uncertainty in the scaling estimate is used as a measure of data quality to weight the time series [W. Williams, F. Hill, C. Toner, T. Brown, Astron. Soc. Pac. Conf. Ser. 42, 441 (1993); W. Williams, F. Hill, C. Toner, ibid. 52, 494 (1993); W. Williams, C. Toner, F. Hill, ibid. 76, 500 (1995); in Fourth SOHO Workshop: Helioseismology Volume 2, J, T. Hoeksema, V. Domingo, B. Fleck, B. Battrick, Eds. (European Space AgencyPubl. Div., Noordwijk aan Zee, Netherlands. 1995), pp. 185-189]. Merging algorithms have also been developed in the context of nonimaged helioseismology for the IRIS network [E. Fossat, Astron. Astrophys. 263, 443 (1992)].
22. The time series from each site-day, scaled to compensate for variations in image resolution from seeing and other effects, are merged to form a longer, more nearly continuous time series. The uncertainty in the scaling estimate is used as a measure of data quality to weight the time series [W. Williams, F. Hill, C. Toner, T. Brown, Astron. Soc. Pac. Conf. Ser. 42, 441 (1993); W. Williams, F. Hill, C. Toner, ibid. 52, 494 (1993); W. Williams, C. Toner, F. Hill, ibid. 76, 500 (1995); in Fourth SOHO Workshop: Helioseismology Volume 2, J, T. Hoeksema, V. Domingo, B. Fleck, B. Battrick, Eds. (European Space AgencyPubl. Div., Noordwijk aan Zee, Netherlands. 1995), pp. 185-189]. Merging algorithms have also been developed in the context of nonimaged helioseismology for the IRIS network [E. Fossat, Astron. Astrophys. 263, 443 (1992)].
23. The time series from each site-day, scaled to compensate for variations in image resolution from seeing and other effects, are merged to form a longer, more nearly continuous time series. The uncertainty in the scaling estimate is used as a measure of data quality to weight the time series [W. Williams, F. Hill, C. Toner, T. Brown, Astron. Soc. Pac. Conf. Ser. 42, 441 (1993); W. Williams, F. Hill, C. Toner, ibid. 52, 494 (1993); W. Williams, C. Toner, F. Hill, ibid. 76, 500 (1995); in Fourth SOHO Workshop: Helioseismology Volume 2, J, T. Hoeksema, V. Domingo, B. Fleck, B. Battrick, Eds. (European Space AgencyPubl. Div., Noordwijk aan Zee, Netherlands. 1995), pp. 185-189]. Merging algorithms have also been developed in the context of nonimaged helioseismology for the IRIS network [E. Fossat, Astron. Astrophys. 263, 443 (1992)].
24. The time series from each site-day, scaled to compensate for variations in image resolution from seeing and other effects, are merged to form a longer, more nearly continuous time series. The uncertainty in the scaling estimate is used as a measure of data quality to weight the time series [W. Williams, F. Hill, C. Toner, T. Brown, Astron. Soc. Pac. Conf. Ser. 42, 441 (1993); W. Williams, F. Hill, C. Toner, ibid. 52, 494 (1993); W. Williams, C. Toner, F. Hill, ibid. 76, 500 (1995); in Fourth SOHO Workshop: Helioseismology Volume 2, J, T. Hoeksema, V. Domingo, B. Fleck, B. Battrick, Eds. (European Space AgencyPubl. Div., Noordwijk aan Zee, Netherlands. 1995), pp. 185-189]. Merging algorithms have also been developed in the context of nonimaged helioseismology for the IRIS network [E. Fossat, Astron. Astrophys. 263, 443 (1992)].
25. The time series from each site-day, scaled to compensate for variations in image resolution from seeing and other effects, are merged to form a longer, more nearly continuous time series. The uncertainty in the scaling estimate is used as a measure of data quality to weight the time series [W. Williams, F. Hill, C. Toner, T. Brown, Astron. Soc. Pac. Conf. Ser. 42, 441 (1993); W. Williams, F. Hill, C. Toner, ibid. 52, 494 (1993); W. Williams, C. Toner, F. Hill, ibid. 76, 500 (1995); in Fourth SOHO Workshop: Helioseismology Volume 2, J, T. Hoeksema, V. Domingo, B. Fleck, B. Battrick, Eds. (European Space AgencyPubl. Div., Noordwijk aan Zee, Netherlands. 1995), pp. 185-189]. Merging algorithms have also been developed in the context of nonimaged helioseismology for the IRIS network [E. Fossat, Astron. Astrophys. 263, 443 (1992)].
26. F. Hill et al., Science 272, 1292 (1996).
27. The GONG project is managed by the National Solar Observatory, a Division of the National Optical Astronomy Observatories, which is operated by the Association of Universities for Research in Astronomy under a cooperative agreement with NSF.