Study of the Solar Cycle Dependence of Low‐Degreep‐Modes with Michelson Doppler Imager and VIRGO

2005 ◽  
Vol 622 (2) ◽  
pp. 1314-1319 ◽  
Author(s):  
T. Toutain ◽  
A. G. Kosovichev
2009 ◽  
Vol 5 (S264) ◽  
pp. 21-32 ◽  
Author(s):  
Marcelo Emilio ◽  
Jeff R. Kuhn ◽  
Rock I. Bush

AbstractIn this work we describe the method and results of precise solar astrometry made with the Michelson Doppler Imager (MDI), on board the Solar and Heliospheric Observatory (SOHO), during one complete solar cycle. We measured an upper limit to the solar radius variation, the absolute solar radius value and the solar shape. Our results are 22 mas peak-to-peak upper limit for the solar radius variation over the solar cycle, the absolute radius was measured as 959.28 ± 0.15 arcsec at 1 AU and the difference between polar and equatorial solar radii in 1997 was 5 km and about three times larger in 2001.


1996 ◽  
Vol 101 (A11) ◽  
pp. 24359-24371 ◽  
Author(s):  
J. Américo González-Esparza ◽  
Edward J. Smith

1997 ◽  
Vol 59 (5) ◽  
pp. 497-509 ◽  
Author(s):  
J. Bremer ◽  
R. Schminder ◽  
K.M. Greisiger ◽  
P. Hoffmann ◽  
D. Kürschner ◽  
...  

2020 ◽  
Vol 895 (1) ◽  
pp. 3
Author(s):  
Xiantong Wang ◽  
Yang Chen ◽  
Gabor Toth ◽  
Ward B. Manchester ◽  
Tamas I. Gombosi ◽  
...  

1973 ◽  
Vol 7 (3) ◽  
pp. 135-140 ◽  
Author(s):  
H Hauska ◽  
S Abdel-Wahab ◽  
E Dyring

2008 ◽  
Vol 15 (3) ◽  
pp. 445-455 ◽  
Author(s):  
S. C. Chapman ◽  
B. Hnat ◽  
K. Kiyani

Abstract. In this review we collate recent results for the statistical scaling properties of fluctuations in the solar wind with a view to synthesizing two descriptions: that of evolving MHD turbulence and that of a scaling signature of coronal origin that passively propagates with the solar wind. The scenario that emerges is that of coexistent signatures which map onto the well known "two component" picture of solar wind magnetic fluctuations. This highlights the need to consider quantities which track Alfvénic fluctuations, and energy and momentum flux densities to obtain a complete description of solar wind fluctuations.


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