The eight-schwabe-cycle pulsation

Abstract

The shape of the Sun's secular activity cycle is found to be a saw-tooth curve. The additional Schwabe cycle 4 (1793 -1799) suggested by Usoskin, Mursula, and Kovaltsov (2001a) is taken into account in the telescopic sunspot record (1610 -2001). Instead of a symmetrical Gleissberg cycle, a saw-tooth of exactly eight Schwabe sunspot maxima ('Pulsation') is found. On average, the last sunspot maximum of an eight-Schwabe-cycle saw-tooth pulsation has been about three times as high as its first maximum. The Maunder Minimum remains an exception to this pattern. The Pulsation is defined as a secular-scale envelope of Schwabe-cycle maxima, whereas the Gleissberg cycle is a result of long-term smoothing of the sunspot series.

Calibration curve from AD 1250 to AD 1650 by measurements of tree-rings grown on the Korean peninsula

“…3.The large peak near 5.5 years is thought to be the second harmonic of the 11 year cycle and is seen in many records [14]. The peak at 10.9 years is estimated to be related to the sunspot cycle known as Schwabe cycle [15]. The fluctuation of the 14 C production rate directly depends on the fluctuation of galactic cosmic ray intensity, which is partially excluded from the solar system by the outward sweep of magnetic fields in the solar wind [16].…”

Connection between solar activity cycles and grand minima generation

“…Moreover, since the EMD describes a signal in terms of empirical time-dependent amplitude and phase functions, it overcomes some limitations of methods based on fixed basis functions such as Fourier and wavelet analysis, thus allowing a correct description of nonlinearities and nonstationarities (Huang et al 1998). Since the scale of variability of the EMD modes is given by the sequence of the local maxima/minima in the data, our approach retraces the early works of Wolf (1861) and Gleissberg (1971) and, more recently, Richard (2004) who tried to recognize long-term variations from the sequence of local maxima in the data.…”

“…Investigations involving Fourier and wavelet based techniques and generalized time-frequency distributions provided the following conclusions (Kolláth & Oláh 2009): the Gleissberg cycle has two high amplitude occurrences, around 1800 and 1950, and its period increases in time varying from about 50 yr near 1750 to approximately 130 yr around 1950. A simpler approach, based on the identification of relative solar cycle maxima on WSN and GSN data, underlined a sawtooth pulsation of eight Schwabe maxima (Richard 2004). However, owing to the relative shortness of the sunspot records (about three periods of Gleissberg cycle are encompassed) the detection of a ∼100 yr oscillation on a ∼300 yr dataset is quite questionable, so that the properties of the Gleissberg cycle are not well constrained and in particular its role in producing grand minima is still unclear.…”

Variations of 14C around AD 775 and AD 1795 – due to solar activity

“…The sinusoidal secular change in the location of the magnetic equator seen in Pulkkinen et al (1999) does not continue into the Maunder Minimum: for the last four cycles of the Maunder Minimum, one cannot state that the magnetic equator was shifted towards the north, the opposite is true (almost only spots in the south); also, one cannot state that north was not leading. Also for Richard's (2004), Waldmeier's (1957), and all kinds of Gleissberg-like long cycles, 18 the Maunder Minimum appears to be an exception. For our picture above, the turnover from the Maunder Minimum to afterwards does not need to be an exception: there is not neccessarily a large drop in activity before each of those four packages where south is stronger, but a large change (drop or rise).…”