CCD-Doppler measurements of solar differential rotation

Solar Physics ◽  
1996 ◽  
Vol 167 (1-2) ◽  
pp. 441-444 ◽  
Author(s):  
Axel D. Wittmann
Solar Physics ◽  
1991 ◽  
Vol 133 (2) ◽  
pp. 177-194
Author(s):  
L. L. Kichatinov

Solar Physics ◽  
2021 ◽  
Vol 296 (1) ◽  
Author(s):  
Bibhuti Kumar Jha ◽  
Aditya Priyadarshi ◽  
Sudip Mandal ◽  
Subhamoy Chatterjee ◽  
Dipankar Banerjee

Solar Physics ◽  
2013 ◽  
Vol 289 (3) ◽  
pp. 759-768 ◽  
Author(s):  
K. J. Li ◽  
W. Feng ◽  
X. J. Shi ◽  
J. L. Xie ◽  
P. X. Gao ◽  
...  

1985 ◽  
Vol 19 (1) ◽  
pp. 71-78
Author(s):  
V. Buraba

Several proceedings of scientific meetings on sunspots appeared during the 1981-1984 period [The Physics of Sunsots, Cram and Thomas (eds.) 1981; see also reports of regional meetings, e.g.. Third European Solar Meeting, Oxford 1981; Nordic Astronomy Meeting, O. Hauge (ed.), Oslo 1983; 11th Regional Consultation on Solar Physics, L. Dezsö and B. Kalman (eds.), Debrecen 1983]. New interest in sunspots was aroused through observations of EUV sunspot spectra from space and was also inspired by the growing number of observations of starspots and other stellar activities [IAU Symposium No. 102, Solar and Stellar Magnetic Fields: Origin and Coronal Effects, J.O. Stenflo (ed.) 1983; Colloquium IAU No. 71 Activity in Red Dwarf Stars, Catania 1982]. Other reasons for the increased interest in sunspots and their energetics were prompted by the correlation between sunspot occurrence and the variations of the solar constant (Hudson et al. 1982) and by the use of sunspot positions for determining solar differential rotation and its change with latitude, depth, and time (Howard et al. 1984, Godoli S Mazzucconi 1982, Balthasar et al. 1984, Tuominen & Kyrolainen 1982, Adam 1983, Koch 1984).


1991 ◽  
Vol 130 ◽  
pp. 178-181
Author(s):  
Kwing L. Chan ◽  
Hans G. Mayr

Recent results from helioseismology (see Goode, these Proceedings) have shown that the inferred contours of the solar angular velocity are more or less radial in the convection region, and the rotation becomes uniform below. These observations contradict the prevailing numerical models of Taylor columns which predict angular velocity contours parallel to the rotation axis of the Sun. Thus, an alternative explanation of solar differential rotation is called for.Presently, it is not feasible to construct a thermally-relaxed, dynamically self-consistent numerical model of the solar convection zone (see Chan and Serizawa, these Proceedings). It is then appropriate to explore simplified models that may shed some light. A number of analytical models have been proposed for the solar differential rotation, and the reader is referred to the book by Rüdiger (1989) for a comprehensive review of this subject. Here, we report on some recent development on the convective resonance model proposed by Chan et al. (1987; hereafter referred as CSM).


Solar Physics ◽  
1991 ◽  
Vol 133 (2) ◽  
pp. 195-203 ◽  
Author(s):  
R. Brajša ◽  
B. Vršnak ◽  
V. Ruždjak ◽  
A. Schroll ◽  
S. Pohjolainen ◽  
...  

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