Magnetic field corrections to solar oscillation frequencies

Nature ◽  
1986 ◽  
Vol 323 (6089) ◽  
pp. 603-605 ◽  
Author(s):  
B. Roberts ◽  
W. R. Campbell
2000 ◽  
Vol 179 ◽  
pp. 343-347
Author(s):  
H. M. Antia ◽  
S. M. Chitre ◽  
M. J. Thompson

AbstractThe observed splittings of solar oscillation frequencies can be utilized to study possible large-scale magnetic fields present in the solar interior. Using the GONG data on frequency splittings an attempt is made to infer the strength of magnetic fields inside the Sun.


Evidence for variability in the solar output is briefly discussed. If the solar neutrino flux and the solar oscillation frequencies vary over a solar cycle this could indicate that the solar cycle has its origin in the solar core rather than be due to dynamo action in the solar convective zone.


Nature ◽  
1988 ◽  
Vol 336 (6201) ◽  
pp. 720-720 ◽  
Author(s):  
D. O. GOUGH

Nature ◽  
1990 ◽  
Vol 345 (6278) ◽  
pp. 779-782 ◽  
Author(s):  
K. G. Libbrecht ◽  
M. F. Woodard

2000 ◽  
Vol 531 (2) ◽  
pp. 1088-1093 ◽  
Author(s):  
Sarbani Basu ◽  
H. M. Antia

1993 ◽  
Vol 141 ◽  
pp. 545-548
Author(s):  
Philip R. Goode

The Sun’s rotation rate near the base of its convection zone might be expected to vary over the solar cycle because of related changes there in the magnetic field. Helioseismic analyses have taught us that much of the Sun’s convection zone rotates with surface-like differential rotation and a transition toward solid body rotation beneath. For a review of what we know about the Sun’s internal rotation, see Goode, et al.(1991). We now have sufficient solar oscillation data to look for changes in the internal rotation near the base of the convection zone. The relevant data are from the 1986, 1988, 1989 and 1990 Big Bear Solar Observatory( BBSO) sets, Libbrecht and Woodard(1992, private communication). These four datasets were gathered at the same site for roughly the same number of days, reduced in the same way and span the same temporal and spatial frequency ranges—the differences between the sets should arise primarily because they were obtained in different years.


2001 ◽  
Vol 203 ◽  
pp. 43-45
Author(s):  
M. Takata ◽  
H. Shibahashi

In our previous work (Takata & Shibahashi 1998), we constructed a solar model called the seismic solar model, which has the consistent profile of sound speed as well as the consistent depth of the convection zone with helioseismology. The profile of the heavy element abundance, however, had to be assumed to be constant for feasibility. Here we try to constrain the distribution of the heavy element abundance as well by the solar oscillation frequencies, adopting all of the basic equations which govern the solar structure.


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