1 / 7

Reconstructing Solar Wind Magnetic Field from Historical Data: Analysis of Sunspot Numbers and Model Inputs

Delve into the progress made in reconstructing the solar wind magnetic field back to the 1840s using the 'IDV' signature. Explore the key findings from recent Sunspot Number Workshops (2011-2014) and the consensus on major issues with the SSN series. Discover how the new Wolf Number offers insights into historical sunspot activity and its implications for understanding solar cycles. Uncover the impact of ‘ephemeral regions’ on solar cycle dependence and the implications for modeling the Maunder Minimum.

lilian
Download Presentation

Reconstructing Solar Wind Magnetic Field from Historical Data: Analysis of Sunspot Numbers and Model Inputs

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Progress in Reconstructing Solar Wind Magnetic Field back to 1840s Svalgaard 2014 Using u-measure Even using only ONE station, the ‘IDV’ signature is strong enough to show the effect

  2. As the Sunspot Number is used as Model input it is important to get that right • Four recent Sunspot Number Workshops (2011-2014) have critically examined the historical sunspot number record(s) • There is now broad consensus among the participants that we have identified the major problems with the SSN series: • A) Error (65%) in Wolf-Wolfer calibration for the GSN before ~1882 • B) Weighting of sunspot counts (20%) for the Int. SSN starting in 1940s

  3. Counting with no Weighting 1 6 2 9 1 xx 19 5x10+44=94 5x10+19=69 94/69 = 1.36 Recounted 2003-2014: ~55,000 spots

  4. Effect on the Wolf Number Factor to remove weighting 0.8535 [inverse of 1.17]

  5. SSN4: No Modern Grand Maximum The preliminary new sunspot record expressed in terms of the number of sunspot groups. Of note is that there is a maximum in every century, none of them particularly ‘Grand’. The new Wolf Number should be used as model input and we should understand the behavior and the fit of the model to the new perspective and to HMF B before we can extrapolate with any degree of confidence to the Maunder Minimum.

  6. No Rising Background ‘Base Level’ Open Flux TSI (LASP) Corr. SSN GSN

  7. Perhaps the Maunder Minimum was Less Extreme than we Thought The emergence of ‘ephemeral regions’ does not show any solar cycle dependence [e.g. Hagenaar, 2008], thus no ever-increasing background

More Related