Sunspot equilibrium and lottery equilibrium are two stochastic solution concepts for nonstochastic economies. Recent work by Garratt, Keister, Qin, and Shell (in press) and Kehoe, Levine, and Prescott (in press) on nonconvex exchange economies has shown that when the randomizing device is continuous, applying the two concepts to the same fundamental economy yields the same set of equilibrium al...

Data for geomagnetic activity index aa for 1868±1994 were subjected to spectral analysis for 12 intervals each of 11 consecutive years. In each interval, QBO and QTO (quasi-biennial and quasi-triennial oscillations) were observed at 2:00, 2.15, 2.40, 2.70 y and 3:20, 3.40 y, but not all in all intervals. These ̄uctuations are absent near (2±3 y before and after) the sunspot minima and are presen...

Infrared spectral observations of sunspots from 1998-2011 have shown that on average sunspots changed; the magnetic fields weakened and the temperatures rose. The data also show that sunspots or dark pores can only form at the solar surface only if the magnetic field strength exceeds about 1500 Gauss. Sunspots appear at the solar surface with a variety of field strengths, and during the period ...

Power spectrum techniques are applied to series of daily, weekly, and monthly average temperature and precipitation values, recorded since 1870 at the Woo'dstock Climatologioal Benchmark Station in Maryland, in order to gain a reasonable interpretation of the extent and frequency distribution of periodic variations in these data. Analysis procedures are outlined, and the results presented, inte...

Hierarchical organization is a cornerstone of complexity and multifractality constitutes its central quantifying concept. For model uniform cascades the corresponding singularity spectra are symmetric while those extracted from empirical data are often asymmetric. Using selected time series representing such diverse phenomena as price changes and intertransaction times in financial markets, sen...

Changes in the heliosphenc magnetic field during the rcccnt declining phase in solar activity are reviewed and compared with observations during past sunspot cycles. The stud y is based pnncipall y on data obtained by IMP-8 and Ulysses. The field magnitude is found to have increased during the declining phase until it reached a maximum value of 11 .5nT in = 1991.5, approximately two years after...

The (14)C production rate in the upper atmosphere changes with time because the galactic cosmic-ray flux responsible for (14)C production is modulated by the changes in solar wind magnetic properties. The resulting changes in the atmospheric (14)C level are recorded in tree rings and are used to calculate past (14)C production rates from a carbon reservoir model that describes terrestrial carbo...

The length of the sunspot cycle determined by FriisChristensen & Lassen (1991) correlates well with indicators of terrestrial climate, but has been criticized as being subjective. In the present paper we present a more objective and general cycle-length determination. Objectivity is achieved by using the continuous wavelet transform based on Morlet wavelets and carrying out a careful error anal...

We report on the discovery of mostly horizontal field channels just outside sunspot penumbrae (in the so-called ‘moat’ region) that are seen to sustain supersonic flows (line-of-sight component of 6 km s). The spectral signature of these supersonic flows corresponds to circular polarization profiles with an additional, satellite, third lobe of the same sign as the parent sunspot’ Stokes V blue ...

[1] Observations from the recent Whole Heliosphere Interval (WHI) solar minimum campaign are compared to last cycle’s Whole Sun Month (WSM) to demonstrate that sunspot numbers, while providing a good measure of solar activity, do not provide sufficient information togaugesolar andheliosphericmagneticcomplexity and its effect at the Earth. Thepresent solarminimum is exceptionally quiet,with suns...