Recent advances in instrumentation that can sense the polarization of the light extend these methods and have made it possible to directly measure solar-strength magnetic fields on other stars.
According to Thomson et al. (2005), the D-region could be used as a solar flare strength indicator for flares greater than class X17 (for which the GOES detector saturates) up to X45 by extrapolating the phase profile.
Their results showed that for a given strength solar flare, ΔH′ will be approximately 1 km greater during the solar minimum period than during the solar maximum, which is in agreement with our findings.
For the SSN and solar polar field strength, a weak multifractality or monofractality is present at the maximum SSN, minimum SSN, and maximum solar polar field strength.
The formation of the magnetic field of the sunspots is correlated with the solar polar field strength.
The change in fractality of the sunspot number (SSN) correlates closely with that of the solar polar field strength.
The bulk density, thermal conductivity, solar reflectivity, flexural strength, and capillary water absorption were determined in accordance to ASTM standards at 28 days of curing.
Available open solar flux, modulation strength, cosmic ray flux, total solar irradiance data, reconstructed back to 1700, solar wind parameters (speed and density) and the magnitude of the heliospheric magnetic field at 1 AU, reconstructed back to 1870, as well as the time series of geomagnetic activity indices (aa, IDV, IHV), going back to 1870, have been considered.
The solar flares of strength C1.0 to C1.3 during the period of low solar activity produced perturbations, whereas flares of same class did not produce any detectable perturbations during the period of moderate solar activity, which is due to the higher sensitivity of the D-region during low solar activity.
