1 The Mean Field of the Sun Leif Svalgaard Stanford University Sept. 2, 2011.

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Presentation transcript:

1 The Mean Field of the Sun Leif Svalgaard Stanford University Sept. 2, 2011

2 Crimean Astrophysical Observatory [since 1968] Mount Wilson Observatory [ ]

3 Wilcox Solar Observatory [since 1976]

4 How the Mean Field is measured The MF is taken to be the difference between the magnetic signal in λ525.0 nm and the non- magnetic line λ512.4 nm.

5 The Early Interpretation 1968 MF as measured at CrAO B INT = 7.2×10 -5 B MF (for 2.0 R ☼ ). “Thus there is a very direct relationship in polarity and in magnitude between the mean solar field and the observed interplanetary field with a 4½ day delay” (Schatten, 1970)

6 The Polarity Relationship [then] WSO 5 days before

7 The Polarity Relationship [now] WSO 5 days before IMF

8 Same Recurrence Periods over Time for MF and HMF [IMF] HMF

9 Rotation Plots of the Sector Polarity Bartels Rotations 127 Skylab Workshop, 1976 CH

10 The Potential Field Source Surface Model Illustrates Many First-Order Effects Simplification and Flattening with Height “Domes of closed field lines” Flattening with Polar Fields

11 The Heliospheric Current Sheet through the Solar cycle Svalgaard & Wilcox, Nature, 1976 Artist: Werner Heil Cosmic Ray Modulation caused by latitudinal variation of HCS and CIRs

12 The MF at the Start of Cycle 24

13 And in Detail Note the detailed 27-day recurrence in sign and magnitude of the MF

14 Different Observatories Agree on the Polarity, but NOT on the Magnitude Roughly: WSO = 2, CrAO = 1, MWO = 4, and SOLIS = 1

15 MWO Anomaly Using the regression factors for each observatory we can bring them all onto the same scale and compute the yearly average of the magnitude After the upgrade of MWO their MF is much too small

16 Evolution of the MF Since 2003

17 Getting Smaller

18 And Smaller

19 And Smaller, but still matching HMF polarity

20 The MF is Riding on a Background HMF that does not Fall Below ~4 nT

21 The Importance of the Polar Fields [?] Pneuman & Kopp, 1971 MHD Vseskhsvjatsky, Eclipse Even with all the sophistication of current models of the Corona and HMF they are hostage to the correct value of the solar polar fields, which may be different at the two poles and even have longitudinal structure within the polar caps. This is particularly important at solar minimum when the HCS is largely flat.

22 Conclusion The Solar Mean Field continues to track the polarity of the HMF The magnitude of the MF does not reflect that of the HMF, but rides on top of a fixed [?] background [i.e. that does not track the polar fields] The MF can be used to monitor the calibration of magnetographs We should calculate the MF from HMI as a product.