000003016 001__ 3016
000003016 005__ 20170106120215.0
000003016 037__ $$aSCART-2017-0012
000003016 100__ $$aCliver, Edward W. 
000003016 245__ $$aComparison of New and Old Sunspot Number Time Series
000003016 260__ $$c2016
000003016 520__ $$aAs a result of the Sunspot Number Workshops, five new sunspot series have recently been proposed: a revision of the original Wolf or international sunspot number (Lockwood et al., 2014), a backbone-based group sunspot number (Svalgaard and Schatten, 2016), a revised group number series that employs active day fractions (Usoskin et al., 2016), a provisional group sunspot number series (Cliver and Ling, 2016) that removes flaws in the normalization scheme for the original group sunspot number (Hoyt and Schatten,1998), and a revised Wolf or international number (termed SN) published on the SILSO website as a replacement for the original Wolf number (Clette and Lefèvre, 2016; thttp://www.sidc.be/silso/datafiles). Despite quite different construction methods, the five new series agree reasonably well after about 1900. From 1750 to ~1875, however, the Lockwood et al. and Usoskin et al. time series are lower than the other three series. Analysis of the Hoyt and Schatten normalization factors used to scale secondary observers to their Royal Greenwich Observatory primary observer reveals a significant inhomogeneity spanning the divergence in ~1885 of the group number from the original Wolf number. In general, a correction factor time series, obtained by dividing an annual group count series by the corresponding yearly averages of raw group counts for all observers, can be used to assess the reliability of new sunspot number reconstructions.
000003016 594__ $$aSTCE
000003016 700__ $$aClette, Frédéric
000003016 700__ $$aLefèvre, Laure
000003016 700__ $$aSvalgaard, Leif
000003016 773__ $$c11.01$$pAmerican Astronomical Society$$vSPD meeting #47$$y2016
000003016 8560_ $$flaure.lefevre@observatoire.be
000003016 905__ $$apublished in
000003016 980__ $$aNONREF