Solar physics meeting at IIA, Bangalore
Solar physics meeting at IIA, Bangalore Solar physics meeting at IIA, Bangalore
Layout of the talk: ‣Observational features of Maunder Minimum. ‣Building a flux transport Babcock-Leighton model. ‣Find out the source of randomness in solar cycle. ‣Use this model to explain the origin of Maunder Minimum.
Maunder minimum: ‣Galileo's s Telescope invention in 1609. ‣Maunder minimum period = 1645 to 1715 (Eddy, 1976; Foukal, 1990; Wilson, 1994) ‣68% of days were observed; sunspots appeared during 2% of the days (Hoyt & Schatten 1996) ‣Related to little ice age. ‣Cosmogenic isotopes: Be 10 and C 14
- Page 1: A possible explanation of Maunder m
- 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
- Page 30: Path between D to A can be advectio
Layout of the talk:<br />
‣Observ<strong>at</strong>ional fe<strong>at</strong>ures of Maunder<br />
Minimum.<br />
‣Building a flux transport Babcock-Leighton<br />
model.<br />
‣Find out the source of randomness in solar<br />
cycle.<br />
‣Use this model to explain the origin of<br />
Maunder Minimum.
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