scholarly journals Magnetic field reversal of the Sun in polarization of radioemission 17GHz

2004 ◽  
Vol 2004 (IAUS223) ◽  
pp. 145-146
Author(s):  
A. G. Tlatov ◽  
V. I. Makarov
Keyword(s):  
Magnetic Field ◽  
The Sun ◽  
Field Reversal ◽  
Magnetic Field Reversal

Polar Magnetic Field Reversals of the Sun in Maunder Minimum

2000 ◽  
Vol 179 ◽  
pp. 193-196
Author(s):  
V. I. Makarov ◽  
A. G. Tlatov
Keyword(s):  
Magnetic Field ◽  
Maunder Minimum ◽  
The Sun ◽  
Annual Rings ◽  
Field Reversal ◽  
Polar Magnetic Field ◽  
Pine Trees ◽  
Using Data ◽  
Magnetic Field Reversal

AbstractA possible scenario of polar magnetic field reversal of the Sun during the Maunder Minimum (1645–1715) is discussed using data of magnetic field reversals of the Sun for 1880–1991 and the14Ccontent variations in the bi-annual rings of the pine-trees in 1600–1730 yrs.

Synchronized periodic maser flares of multiple OH and CH3OH lines in G323.459–0.079

2021 ◽  
Vol 502 (4) ◽  
pp. 5658-5667
Author(s):  
G C MacLeod ◽  
Derck P Smits ◽  
J A Green ◽  
S P van den Heever
Keyword(s):  
Magnetic Field ◽  
Excited State ◽  
Central Region ◽  
Time Lags ◽  
Field Reversal ◽  
Methanol Maser ◽  
Physical Conditions ◽  
Upper Limit ◽  
Methanol Masers ◽  
Magnetic Field Reversal

ABSTRACT The first confirmed periodically varying 6.031 and 6.035 GHz hydroxyl masers are reported here. They vary contemporaneously with the 6.7 GHz methanol masers in G323.459–0.079. The 1.665 GHz hydroxyl and 12.2  GHz methanol masers associated with G323.459–0.079 are also periodic. Evidence for periodicity is seen in all features in all transitions save a single 1.665 GHz hydroxyl maser feature. Historical excited-state hydroxyl maser observations set a stricter upper limit on the epoch in which a significant accretion event occurred. The associated burst in 6.7 GHz methanol maser activity has subsided significantly while the hydroxyl transitions are brightening possibly the result of changing physical conditions in the masing cloudlets. Time lags in methanol are confirmed and may be the result of the periodic flaring propagating outward from the central region of maser activity. A possible magnetic field reversal occurred during the accretion event.

scholarly journals A Quantitative Study of Magnetic Flux Transport on the Sun

1983 ◽  
Vol 102 ◽  
pp. 273-278 ◽  
Author(s):  
N.R. Sheeley ◽  
J.P. Boris ◽  
T.R. Young ◽  
C.R. DeVore ◽  
K.L. Harvey
Keyword(s):  
Magnetic Field ◽  
Magnetic Flux ◽  
Quantitative Study ◽  
Differential Rotation ◽  
Meridional Circulation ◽  
Diffusion Constant ◽  
The Sun ◽  
Flux Transport ◽  
Field Reversal ◽  
Best Fit

A computational model, based on diffusion, differential rotation, and meridional circulation, has been developed to simulate the transport of magnetic flux on the Sun. Using Kitt Peak magnetograms as input, we have determined a best-fit diffusion constant by comparing the computed and observed fields at later times. Our value of 730 ± 250 km2/s is consistent with Leighton's (1964) estimate of 770–1540 km2/s and is significantly larger than Mosher's (1977) estimate of 200–400 km2/s. This suggests that diffusion may be fast enough to account for the observed polar magnetic field reversal without requiring a significant assist from meridional currents.

Radiation Belts during a Magnetic Field Reversal

2020 ◽  
Vol 58 (4) ◽  
pp. 227-233
Author(s):  
O. O. Tsareva ◽  
L. M. Zelenyi ◽  
Kh. V. Malova ◽  
V. Yu. Popov
Keyword(s):  
Magnetic Field ◽  
Radiation Belts ◽  
Field Reversal ◽  
Magnetic Field Reversal

On 22-Year Pole To Equator Variation of the Corona Intensity

1994 ◽  
Vol 144 ◽  
pp. 96
Author(s):  
V. I. Makarov ◽  
A. G. Tlatov
Keyword(s):  
Magnetic Field ◽  
Velocity Field ◽  
Solution Method ◽  
Least Square ◽  
Field Reversal ◽  
Torsional Oscillations ◽  
Zero Values ◽  
The Magnetic Field ◽  
Magnetic Field Reversal

AbstractKislovodsk sets of observations (1957.5-1991.0) of the corona in the line Fe XIV 5303 Å have been processed. Half annual intensities of corona have been approximated with the polynoms of the m-degree in dependence on latitude. The coefficients of these sets have been found using the least square solution method. The zone of zero values of the second derivation of the coronal intensity on latitude has been determined. It is shown that this zone emerges after the magnetic field reversal at the latitudes near 80° then migrates equatorward during 22 years with a velocity of 2 m/s. The obtained data were compared with a pattern of torsional oscillations plotted on the basis of the velocity field. A possible reason for 22 year pole to equator variations in the corona is considered.

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