Sunspots continued to represent enigma phenomena. The recent detection and measurement of sunspot magnetic field region, while emerging from solar interior, lead to suggestion of an elongated plasma body model composed of oppositely... more
Sunspots continued to represent enigma phenomena. The recent detection and measurement of sunspot magnetic field region, while emerging from solar interior, lead to suggestion of an elongated plasma body model composed of oppositely gyrating electrons and protons. It is thought to produce the Plasma Body External Magnetic Field (PB_Ex). Magnetic field emanating from PB_EX is thought to interacts through Active Region External Magnetic Field (B_AREx), with the granules and photosphere constituents, magnetizing these layers, and forming patches or sunspots. Produced magnetic force resulted from that, pulls the granules forming Wilson depression. An inter-atomic mechanism that decreased granules (sunspots) temperature due to B_AREx interaction with atomic magnetic field is proposed. The knowledge of these mechanisms may help to understand the solar activities and how it should be predicted to protect humanity from any hazardous consequences.
δ type sunspot groups are known to have high flare productivity and to produce very strong flares. In particular, βγδ type sunspots are the most active type of all. A βγδ active region NOAA9957 with frequent flux cancelations but without... more
δ type sunspot groups are known to have high flare productivity and to produce very strong flares. In particular, βγδ type sunspots are the most active type of all. A βγδ active region NOAA9957 with frequent flux cancelations but without any marked flare activity during its decay phase was studied in this work. Using SOHO/MDI Dopplergrams and magnetograms, we detected continuous prominent downflow motions of 1500-1700m s¡1 for several hours on the magnetic neutral line in this region. In the downflow region, penumbral structure were observed to decay. We will interpret and discuss the phenomenon as one case of submergence of the magnetic flux.
The partial pressures of 20 ionic molecular species are reported for standard facular, photospheric, and sunspot model atmospheres with a view to picking up ionized molecules for a possible identification in the solar spectrum. Comparing... more
The partial pressures of 20 ionic molecular species are reported for standard facular, photospheric, and sunspot model atmospheres with a view to picking up ionized molecules for a possible identification in the solar spectrum. Comparing the partial pressures with those of the molecule SiH(+), which is already detected in the solar spectrum, it appears probable that additional ionic species can be identified in the same spectrum. To predict the line intensities of such species, accurate values of oscillator strengths and dissociation energies are needed.
The stability of a solar model on the main sequence to linearized nonadiabatic nonradial oscillations has been studied. In the inner 99.9 per cent b.y. radius the eigenfunctions were barely distinguishable from those of the adiabatic... more
The stability of a solar model on the main sequence to linearized nonadiabatic nonradial oscillations has been studied. In the inner 99.9 per cent b.y. radius the eigenfunctions were barely distinguishable from those of the adiabatic approximation. The integrated effect of this region is to stabilize the oscillations at zero age, but after a time of order .1 b.y. the destabilizing effect of the 3He (3He, 2p) 4He reactions exceeds the damping. However, there is much more severe damping in a nonadiabatic shell beneath the photosphere about 300 km thick, which dominates the entire effect from the rest of the star interior to this shell.
