Solar physics meeting at IIA, Bangalore
Solar physics meeting at IIA, Bangalore Solar physics meeting at IIA, Bangalore
from physics.iisc.ernet.in
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23.05.2014
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Path between D to A can be advection dominated or diffusion dominated (Yeates, Nandy & Mackey 2008) or can be turbulent pumping p dominated.
- Page 1 and 2: A possible explanation of Maunder m
- Page 3 and 4: Maunder minimum: ‣Galileo's s Tel
- Page 5 and 6: Usual 11-year period of solar activ
- Page 7 and 8: Dynamo Model: Parker (1955) Axisymm
- Page 9 and 10: Poloidal Field Generation:- The Mea
- Page 11 and 12: In axisymmetry case Velocity field=
- Page 13 and 14: Transport mechanisms: 1) meridional
- Page 15 and 16: Chatterjee et al. (2004)
- Page 17 and 18: 2. Fluctuation in the meridional ci
- Page 19 and 20: ∂B 1⎡ ∂ ∂ ⎤ 2 1 + ( rvrB)
- Page 21 and 22: How to introduce fluctuation? The s
- Page 23 and 24: all Choudhuri & Karak (2009)
- Page 25 and 26: Dynamo growth rate is determined by
- Page 27 and 28: Are we entering another grand minim
P<strong>at</strong>h between D to A can be advection domin<strong>at</strong>ed or<br />
diffusion domin<strong>at</strong>ed (Ye<strong>at</strong>es, Nandy & Mackey 2008)<br />
or can be turbulent pumping p domin<strong>at</strong>ed.
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