Origin of stellar magnetic fields

It is pointed out that the magnetic field of a star is originated from dynamo action associated with the stellar evolution. The magnetic field of a star is related with how much nuclear energy is generated in its phase of evolution. From this we can explain why some stars possess a magnetic field high than that of the Sun. In our case the magnetic field of the star is a by-product of the stars evolution and it has no influence on the internal structure of the star but it does have influence on the flare, chromosphere and coronal activities of the star. Again it is stressed that to confirm the activities of the star, the details of evolution of stars should be calculated according to the photon-neutrino coupling theory.     

Remarks on the soft X-ray emission from the galactic radio spurs

It is pointed out that the all old supernova remnants are not in general sources of soft X-ray emission. Again it is pointed out that the galactic radio spur (Cetus arc) may be an old supernova remnant but it has already ceased to be a source of X-ray emission. Finally X-ray flux from Vela is ostimated from cooling rate of neutron star by neutrino emission. The results agree approximately with the observed X-ray flux from Vela X.     

Periodicities in Forbush decreases and solar activity

We have studied Forbush decreases (FD) with solar flare data and major solar proton event (SPE) data (E > 10 MeV) for the years 1976–1986 and have found that FD solar flare data exhibit periods around 0.95, 2.4, and 4.75 years at >99% level of confidence (CL), while SPE data exhibit periods around 2.6 and 5.0 years (at >95% CL). Because of a common periodicity around 2.5 years, it is suggested that FD with the solar flare data and major SPE data, together with solar diameter and solar neutrino variations, behave similarly and may have a common origin.