Comparison of two fitting methods for ring diagram analysis of very high / solar oscillations

J. Patrón; I. González Hernández; Dean Y.I. Chou; M. T. Sun; T. M. Mu; S. Loudagh; B. Bala; Y. P. Chou; C. H. Lin; I. J. Huang; A. Jiménez; M. C. Rabello-Soares; G. Ai; G. P. Wang; H. Zirin; W. Marquette; J. Nenow; S. Ehgamberdiev; S. Khalikov

doi:10.1086/304469

Comparison of two fitting methods for ring diagram analysis of very high / solar oscillations

J. Patrón^*, I. González Hernández, Dean Y.I. Chou, M. T. Sun, T. M. Mu, S. Loudagh, B. Bala, Y. P. Chou, C. H. Lin, I. J. Huang, A. Jiménez, M. C. Rabello-Soares, G. Ai, G. P. Wang, H. Zirin, W. Marquette, J. Nenow, S. Ehgamberdiev, S. Khalikov

^*Corresponding author for this work

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

31 Scopus citations

Abstract

A new method of fitting tridimensional power spectra of solar oscillations is described and compared with a previous one whose use has been more common. The new method fits the parameters of the Lorentzian profiles in a bidimensional k - ω diagram constructed from an azimuthal average of the tridimensional one. The horizontal velocities are then determined keeping these parameters fixed, greatly reducing the computation time. Both methods are compared for two radial orders (n = 3, 4) of a tridimensional power spectrum obtained for a region of about 15° square around solar disk center. The images used in this work correspond to a 3 day set of 1080 × 1080 pixel intensity images obtained at the Observatorio del Teide on 1994 November 8-10 with the Taiwanese Oscillation Network (TON) instrument. The results of the fitted velocities agree within the estimated errors for the two methods. The reduction of the computing time, obtained with the new method makes it convenient for the ring diagram analysis.

Original language	English
Pages (from-to)	869-874
Number of pages	6
Journal	Astrophysical Journal
Volume	485
Issue number	2 PART I
DOIs	https://doi.org/10.1086/304469
State	Published - 1997
Externally published	Yes

Keywords

Convection
Methods: numerical
Sun: oscillations

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10.1086/304469

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Patrón, J., Hernández, I. G., Chou, D. Y. I., Sun, M. T., Mu, T. M., Loudagh, S., Bala, B., Chou, Y. P., Lin, C. H., Huang, I. J., Jiménez, A., Rabello-Soares, M. C., Ai, G., Wang, G. P., Zirin, H., Marquette, W., Nenow, J., Ehgamberdiev, S., & Khalikov, S. (1997). Comparison of two fitting methods for ring diagram analysis of very high / solar oscillations. Astrophysical Journal, 485(2 PART I), 869-874. https://doi.org/10.1086/304469

@article{c31c8da4f12d49bab4256f81fee12856,

title = "Comparison of two fitting methods for ring diagram analysis of very high / solar oscillations",

abstract = "A new method of fitting tridimensional power spectra of solar oscillations is described and compared with a previous one whose use has been more common. The new method fits the parameters of the Lorentzian profiles in a bidimensional k - ω diagram constructed from an azimuthal average of the tridimensional one. The horizontal velocities are then determined keeping these parameters fixed, greatly reducing the computation time. Both methods are compared for two radial orders (n = 3, 4) of a tridimensional power spectrum obtained for a region of about 15° square around solar disk center. The images used in this work correspond to a 3 day set of 1080 × 1080 pixel intensity images obtained at the Observatorio del Teide on 1994 November 8-10 with the Taiwanese Oscillation Network (TON) instrument. The results of the fitted velocities agree within the estimated errors for the two methods. The reduction of the computing time, obtained with the new method makes it convenient for the ring diagram analysis.",

keywords = "Convection, Methods: numerical, Sun: oscillations",

author = "J. Patr{\'o}n and Hern{\'a}ndez, {I. Gonz{\'a}lez} and Chou, {Dean Y.I.} and Sun, {M. T.} and Mu, {T. M.} and S. Loudagh and B. Bala and Chou, {Y. P.} and Lin, {C. H.} and Huang, {I. J.} and A. Jim{\'e}nez and Rabello-Soares, {M. C.} and G. Ai and Wang, {G. P.} and H. Zirin and W. Marquette and J. Nenow and S. Ehgamberdiev and S. Khalikov",

year = "1997",

doi = "10.1086/304469",

language = "英语",

volume = "485",

pages = "869--874",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "2 PART I",

}

Patrón, J, Hernández, IG, Chou, DYI, Sun, MT, Mu, TM, Loudagh, S, Bala, B, Chou, YP, Lin, CH, Huang, IJ, Jiménez, A, Rabello-Soares, MC, Ai, G, Wang, GP, Zirin, H, Marquette, W, Nenow, J, Ehgamberdiev, S & Khalikov, S 1997, 'Comparison of two fitting methods for ring diagram analysis of very high / solar oscillations', Astrophysical Journal, vol. 485, no. 2 PART I, pp. 869-874. https://doi.org/10.1086/304469

TY - JOUR

T1 - Comparison of two fitting methods for ring diagram analysis of very high / solar oscillations

AU - Patrón, J.

AU - Hernández, I. González

AU - Chou, Dean Y.I.

AU - Sun, M. T.

AU - Mu, T. M.

AU - Loudagh, S.

AU - Bala, B.

AU - Chou, Y. P.

AU - Lin, C. H.

AU - Huang, I. J.

AU - Jiménez, A.

AU - Rabello-Soares, M. C.

AU - Ai, G.

AU - Wang, G. P.

AU - Zirin, H.

AU - Marquette, W.

AU - Nenow, J.

AU - Ehgamberdiev, S.

AU - Khalikov, S.

PY - 1997

Y1 - 1997

N2 - A new method of fitting tridimensional power spectra of solar oscillations is described and compared with a previous one whose use has been more common. The new method fits the parameters of the Lorentzian profiles in a bidimensional k - ω diagram constructed from an azimuthal average of the tridimensional one. The horizontal velocities are then determined keeping these parameters fixed, greatly reducing the computation time. Both methods are compared for two radial orders (n = 3, 4) of a tridimensional power spectrum obtained for a region of about 15° square around solar disk center. The images used in this work correspond to a 3 day set of 1080 × 1080 pixel intensity images obtained at the Observatorio del Teide on 1994 November 8-10 with the Taiwanese Oscillation Network (TON) instrument. The results of the fitted velocities agree within the estimated errors for the two methods. The reduction of the computing time, obtained with the new method makes it convenient for the ring diagram analysis.

AB - A new method of fitting tridimensional power spectra of solar oscillations is described and compared with a previous one whose use has been more common. The new method fits the parameters of the Lorentzian profiles in a bidimensional k - ω diagram constructed from an azimuthal average of the tridimensional one. The horizontal velocities are then determined keeping these parameters fixed, greatly reducing the computation time. Both methods are compared for two radial orders (n = 3, 4) of a tridimensional power spectrum obtained for a region of about 15° square around solar disk center. The images used in this work correspond to a 3 day set of 1080 × 1080 pixel intensity images obtained at the Observatorio del Teide on 1994 November 8-10 with the Taiwanese Oscillation Network (TON) instrument. The results of the fitted velocities agree within the estimated errors for the two methods. The reduction of the computing time, obtained with the new method makes it convenient for the ring diagram analysis.

KW - Convection

KW - Methods: numerical

KW - Sun: oscillations

UR - http://www.scopus.com/inward/record.url?scp=21744432071&partnerID=8YFLogxK

U2 - 10.1086/304469

DO - 10.1086/304469

M3 - 文章

AN - SCOPUS:21744432071

SN - 0004-637X

VL - 485

SP - 869

EP - 874

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2 PART I

ER -

Comparison of two fitting methods for ring diagram analysis of very high / solar oscillations

Abstract

Keywords

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