Tri-phonic helioseismology: Comparison of solar p modes observed by the helioseismology instruments aboard SOHO

T. Toutain; T. Appourchaux; F. Baudin; C. Fröhlich; A. Gabriel; P. Scherrer; B. N. Andersen; R. Bogart; R. Bush; W. Finsterle; R. A. García; G. Grec; C. J. Henney; J. T. Hoeksema; A. Jiménez; A. Kosovichev; T. Roca Cortés; S. Turck-Chièze; R. Ulrich; C. Wehrli

doi:10.1023/A:1004949832159

Tri-phonic helioseismology: Comparison of solar p modes observed by the helioseismology instruments aboard SOHO

T. Toutain
, T. Appourchaux
, F. Baudin
, C. Fröhlich
, A. Gabriel
, P. Scherrer
, B. N. Andersen
, R. Bogart
, R. Bush
, W. Finsterle
, R. A. García
, G. Grec
, C. J. Henney
, J. T. Hoeksema
, A. Jiménez
, A. Kosovichev
, T. Roca Cortés
, S. Turck-Chièze
, R. Ulrich
, C. Wehrli

Research output: Contribution to journal › Article › peer-review

41 Scopus citations

Abstract

The three helioseismology instruments aboard SOHO observe solar p modes in velocity (GOLF and MDI) and in intensity (VIRGO and MDI). Time series of two months duration are compared and confirm that the instruments indeed observe the same Sun to a high degree of precision. Power spectra of 108 days are compared showing systematic differences between mode frequencies measured in intensity and in velocity. Data coverage exceeds 97% for all the instruments during this interval. The weighted mean differences (V - I) are -0.1 μHz for l = 0, and -0.16 μHz for l = 1. The source of this systematic difference may be due to an asymmetry effect that is stronger for modes seen in intensity. Wavelet analysis is also used to compare the shape of the forcing functions. In these data sets nearly all of the variations in mode amplitude are of solar origin. Some implications for structure inversions are discussed.

Original language	English (US)
Pages (from-to)	311-328
Number of pages	18
Journal	Solar Physics
Volume	175
Issue number	2
DOIs	https://doi.org/10.1023/A:1004949832159
State	Published - 1997
Externally published	Yes

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.1023/A:1004949832159

Cite this

Toutain, T., Appourchaux, T., Baudin, F., Fröhlich, C., Gabriel, A., Scherrer, P., Andersen, B. N., Bogart, R., Bush, R., Finsterle, W., García, R. A., Grec, G., Henney, C. J., Hoeksema, J. T., Jiménez, A., Kosovichev, A., Roca Cortés, T., Turck-Chièze, S., Ulrich, R., & Wehrli, C. (1997). Tri-phonic helioseismology: Comparison of solar p modes observed by the helioseismology instruments aboard SOHO. Solar Physics, 175(2), 311-328. https://doi.org/10.1023/A:1004949832159

@article{f23987cfda0f47ecafa8f7f9c5d65a2c,

title = "Tri-phonic helioseismology: Comparison of solar p modes observed by the helioseismology instruments aboard SOHO",

abstract = "The three helioseismology instruments aboard SOHO observe solar p modes in velocity (GOLF and MDI) and in intensity (VIRGO and MDI). Time series of two months duration are compared and confirm that the instruments indeed observe the same Sun to a high degree of precision. Power spectra of 108 days are compared showing systematic differences between mode frequencies measured in intensity and in velocity. Data coverage exceeds 97\% for all the instruments during this interval. The weighted mean differences (V - I) are -0.1 μHz for l = 0, and -0.16 μHz for l = 1. The source of this systematic difference may be due to an asymmetry effect that is stronger for modes seen in intensity. Wavelet analysis is also used to compare the shape of the forcing functions. In these data sets nearly all of the variations in mode amplitude are of solar origin. Some implications for structure inversions are discussed.",

author = "T. Toutain and T. Appourchaux and F. Baudin and C. Fr{\"o}hlich and A. Gabriel and P. Scherrer and Andersen, \{B. N.\} and R. Bogart and R. Bush and W. Finsterle and Garc{\'i}a, \{R. A.\} and G. Grec and Henney, \{C. J.\} and Hoeksema, \{J. T.\} and A. Jim{\'e}nez and A. Kosovichev and \{Roca Cort{\'e}s\}, T. and S. Turck-Chi{\`e}ze and R. Ulrich and C. Wehrli",

note = "Funding Information: VIRGO is a cooperative effort of many individual scientists and engineers at several institutes in Europe and U.S.A. The VIRGO team has been supported by several national and international funding agencies which are gratefully acknowledged: the PMOD/WRC by the Swiss National Science Foundation and PRODEX, the IRMB by the Fonds de la Recherche Fondamentale Collection d{\textquoteright}initiative min-ist{\'e}rielle and PRODEX, the SSD/ESA by their annual funds from the Science Directorate, the IAC by the CICYT through PNIE, and the OCA by the CNES and CNRS. Funding Information: All three instruments benefit from the quiet and well run SOHO platform built by Matra-Marconi Space. SOHO is an international collaboration programme of the European Space Agency and the National Aeronautics Space Administration. F.B. and the SOI/MDI Team at Stanford acknowledge support from NASA under Contract NAS 5–30386.",

year = "1997",

doi = "10.1023/A:1004949832159",

language = "English (US)",

volume = "175",

pages = "311--328",

journal = "Solar Physics",

issn = "0038-0938",

publisher = "Springer Netherlands",

number = "2",

}

Toutain, T, Appourchaux, T, Baudin, F, Fröhlich, C, Gabriel, A, Scherrer, P, Andersen, BN, Bogart, R, Bush, R, Finsterle, W, García, RA, Grec, G, Henney, CJ, Hoeksema, JT, Jiménez, A, Kosovichev, A, Roca Cortés, T, Turck-Chièze, S, Ulrich, R & Wehrli, C 1997, 'Tri-phonic helioseismology: Comparison of solar p modes observed by the helioseismology instruments aboard SOHO', Solar Physics, vol. 175, no. 2, pp. 311-328. https://doi.org/10.1023/A:1004949832159

TY - JOUR

T1 - Tri-phonic helioseismology

T2 - Comparison of solar p modes observed by the helioseismology instruments aboard SOHO

AU - Toutain, T.

AU - Appourchaux, T.

AU - Baudin, F.

AU - Fröhlich, C.

AU - Gabriel, A.

AU - Scherrer, P.

AU - Andersen, B. N.

AU - Bogart, R.

AU - Bush, R.

AU - Finsterle, W.

AU - García, R. A.

AU - Grec, G.

AU - Henney, C. J.

AU - Hoeksema, J. T.

AU - Jiménez, A.

AU - Kosovichev, A.

AU - Roca Cortés, T.

AU - Turck-Chièze, S.

AU - Ulrich, R.

AU - Wehrli, C.

N1 - Funding Information: VIRGO is a cooperative effort of many individual scientists and engineers at several institutes in Europe and U.S.A. The VIRGO team has been supported by several national and international funding agencies which are gratefully acknowledged: the PMOD/WRC by the Swiss National Science Foundation and PRODEX, the IRMB by the Fonds de la Recherche Fondamentale Collection d’initiative min-istérielle and PRODEX, the SSD/ESA by their annual funds from the Science Directorate, the IAC by the CICYT through PNIE, and the OCA by the CNES and CNRS. Funding Information: All three instruments benefit from the quiet and well run SOHO platform built by Matra-Marconi Space. SOHO is an international collaboration programme of the European Space Agency and the National Aeronautics Space Administration. F.B. and the SOI/MDI Team at Stanford acknowledge support from NASA under Contract NAS 5–30386.

PY - 1997

Y1 - 1997

N2 - The three helioseismology instruments aboard SOHO observe solar p modes in velocity (GOLF and MDI) and in intensity (VIRGO and MDI). Time series of two months duration are compared and confirm that the instruments indeed observe the same Sun to a high degree of precision. Power spectra of 108 days are compared showing systematic differences between mode frequencies measured in intensity and in velocity. Data coverage exceeds 97% for all the instruments during this interval. The weighted mean differences (V - I) are -0.1 μHz for l = 0, and -0.16 μHz for l = 1. The source of this systematic difference may be due to an asymmetry effect that is stronger for modes seen in intensity. Wavelet analysis is also used to compare the shape of the forcing functions. In these data sets nearly all of the variations in mode amplitude are of solar origin. Some implications for structure inversions are discussed.

AB - The three helioseismology instruments aboard SOHO observe solar p modes in velocity (GOLF and MDI) and in intensity (VIRGO and MDI). Time series of two months duration are compared and confirm that the instruments indeed observe the same Sun to a high degree of precision. Power spectra of 108 days are compared showing systematic differences between mode frequencies measured in intensity and in velocity. Data coverage exceeds 97% for all the instruments during this interval. The weighted mean differences (V - I) are -0.1 μHz for l = 0, and -0.16 μHz for l = 1. The source of this systematic difference may be due to an asymmetry effect that is stronger for modes seen in intensity. Wavelet analysis is also used to compare the shape of the forcing functions. In these data sets nearly all of the variations in mode amplitude are of solar origin. Some implications for structure inversions are discussed.

UR - https://www.scopus.com/pages/publications/0031318796

UR - https://www.scopus.com/pages/publications/0031318796#tab=citedBy

U2 - 10.1023/A:1004949832159

DO - 10.1023/A:1004949832159

M3 - Article

AN - SCOPUS:0031318796

SN - 0038-0938

VL - 175

SP - 311

EP - 328

JO - Solar Physics

JF - Solar Physics

IS - 2

ER -

Tri-phonic helioseismology: Comparison of solar p modes observed by the helioseismology instruments aboard SOHO

Abstract

All Science Journal Classification (ASJC) codes

Access to Document

Other files and links

Fingerprint

Cite this