Article

Comparison of Two Fitting Methods for Ring Diagram Analysis of Very High<i>l</i>Solar Oscillations

J. PatrónInstituto de Astrofísica de Canarias, 38200, La Laguna, Tenerife, SpainJ. I. Gónzalez HernándezInstituto de Astrofísica de Canarias, 38200, La Laguna, Tenerife, SpainDean‐Yi ChouPhysics Department, Tsing Hua University, Hsinchu, 30043, Taiwan, Republic of ChinaMing SunPhysics Department, Tsing Hua University, Hsinchu, 30043, Taiwan, Republic of ChinaTao-Mo MuPhysics Department, Tsing Hua University, Hsinchu, 30043, Taiwan, Republic of ChinaS. LoudaghPhysics Department, Tsing Hua University, Hsinchu, 30043, Taiwan, Republic of ChinaB. K. BalaPhysics Department, Tsing Hua University, Hsinchu, 30043, Taiwan, Republic of ChinaYi-Li ChouPhysics Department, Tsing Hua University, Hsinchu, 30043, Taiwan, Republic of ChinaChih‐Yuan LinPhysics Department, Tsing Hua University, Hsinchu, 30043, Taiwan, Republic of ChinaI.‐J. HuangPhysics Department, Tsing Hua University, Hsinchu, 30043, Taiwan, Republic of ChinaA. JiménezInstituto de Astrofísica de Canarias, 38200, La Laguna, Tenerife, Canary Islands, SpainM. C. Rabello‐SoaresInstituto de Astrofísica de Canarias, 38200, La Laguna, Tenerife, Canary Islands, SpainG. X. AiBeijing Astronomical Observatory, 15 Zhongguancun, Beijing, China 100080G. P. WangBeijing Astronomical Observatory, 15 Zhongguancun, Beijing, China 100080H. ZirinBig Bear Solar Observatory, 40386 North Shore Lane, Big Bear City, CA 92314W. MarquetteBig Bear Solar Observatory, 40386 North Shore Lane, Big Bear City, CA 92314J. NenowBig Bear Solar Observatory, 40386 North Shore Lane, Big Bear City, CA 92314Sh. A. EhgamberdievAstronomical Institute, Uzbek Academy of Science, 700052 Tashkent, UzbekistanS. KhalikovAstronomical Institute, Uzbek Academy of Science, 700052 Tashkent, Uzbekistan(The TON Team)

The Astrophysical Journaljournal1997en

ABI

Abstract

A new method of tting tridimensional power spectra of solar oscillations is described and compared with a previous one whose use has been more common. The new method ts the parameters of the Lorentzian proles in a bidimensional k [ u diagram constructed from an azimuthal average of the tridimensional one. The horizontal velocities are then determined keeping these parameters xed, 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 810 with the Taiwanese Oscillation Network (TON) instrument. The results of the tted 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.

Topics

Solar and Space Plasma Dynamics Atmospheric Ozone and Climate Climate variability and models

Identifiers

DOI: 10.1086/304469

Citations and references

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