Using Old Geomagnetic Data to Say Something about the Sun

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Presentation transcript:

Using Old Geomagnetic Data to Say Something about the Sun Leif Svalgaard Oct. 16, 2013

The Russian Observatories Helsinki [Finland] established on 28th March 1838 by imperial decree of Czar Nicholas I. First director J.J. Nervandor (1805-1848). Ready for business: July 1st, 1844, continued until 1905. Last few years unreliable because of disturbances from electric tramway traffic started in 1901.

Variometer Invented by Gauss

The Raw Data 1844-1856 10 minute cadence 1856-1897 1 hour cadence 2.5 million observations Staff: Director and 12 observers [students] Many hundred notebooks

Detail of Raw Data Digitized by pupils in elementary schools all across Finland

Sample Data Regular daily variation Magnetic storm

Relation to HMF Strength B

Today B V n Kp

Wolf’s Discovery: rD = a + b RW . North X rY Morning H rD D Evening East Y Y = H sin(D) dY = H cos(D) dD For small dD A current system in the ionosphere is created and maintained by solar FUV radiation

The Diurnal Variation of the Declination for Low, Medium, and High Solar Activity

All Geomagnetic Observatories Show the Relationship with Sunspot Number

H Scale Value Problem at Helsinki

Also for Declination in 1886

Creates Problems for Assessment of Long-Term Variation of Activity

24-hour running means of the Horizontal Component of the low- & mid-latitude geomagnetic field remove most of local time effects and leaves a Global imprint of the Ring Current [Van Allen Belts]: A quantitative measure of the effect can be formed as a series of the unsigned differences between consecutive days: The InterDiurnal Variability, IDV-index

IDV is strongly correlated with HMF B, but is blind to solar wind speed V

Since we can also estimate solar wind speed from geomagnetic indices [Svalgaard & Cliver, JGR 2007] we can calculate the radial magnetic flux from the total B using the Parker Spiral formula: There seems to be both a Floor and a Ceiling and most importantly no long-term trend since the 1830s.

Re-evaluation of Cosmic Ray Data Still problem with the 1880-1890s and generally with low values

Conclusion Important to correct data for scale value errors Signs of consensus on Cosmic Ray data No Modern Grand Maximum This is still controversial, hence my current interest