The fusion reaction [1] is a source of solar Ps production that persistent in thermal plasma at [20] for a while that is good enough to measure the transition energies between the quantum states. Since the reduced mass of Ps is just half of that of H atom and hence the binding energy of Rydberg Ps is −6.8 eV. Correspondingly Ps-Lyman- has a wavelength of 243 nm and was observed by Canter et al. [21] . The total wave function of the Ps state is the product of three wave functions depending on the spin, space and charge coordinates:

This is a symmetric-antisymmetric wave function depends on the spin functions for a combination of two spin-1/2 particle-antiparticle (and) can be expressed in the following four possible blends [22] :

where the first three form a spin triplet of and, 0, −1 states have the property that they are symmetric under particle interchange, and the last one is a singlet of state has the prop-

erty of antisymmetric. The symmetry of the spin function under particle interchange is, where

is the total spin. Particle interchange is equivalent to space inversion, introducing a factor, where is the orbital angular momentum of the system. The charge wave function acquire a charge conjugation factor where is the number of photons under particle interchange. The product of the factors applying to the separate spin, space, and charge function must then be that of the total wave function, which we denote by, so that. Individuality of the singlet and the triplet states Ps are presented in Table 1.

Since most of the previous studies have focused on the Galactic centre as the most promising source of Ps, although visual extinction is very high. However, detection of Ps recombination line made by Puxley & Skimer (1996) who searched for Ps Paschen- from the Galactic centre but undetected [23] . Very recently study chromaticity of solar spectrum lead me to discover the solar Ps which is described in the following sections. This renewed interest is motivated by several recent and imminent advances in technology. From the literature survey it is found that Ps formation, recombination and quenching largely take place at temperature <10⁶ K. Therefore, most astrophysical environments (~10³ - 10⁶ K) for Ps formation will be the dominant process leading to annihilation [24] . A comparative study of Ps, H and He are shown in Table 2.

The spectral lines (wavelength) of solar radiation spectrum are achieved from the Rydberg-Ritz formula:

where is the Planck’s constant, is the speed of light, is the Rydberg energy (shown in Table 2). Hence, wavelength of each atom will be different i.e., different color bands in the spectrum. The quantum numbers and respectively are the initial and final states of the atomic transition. For the Lyman series and; for the Balmer series and; for the Paschen series and; and for the Brackett series and, .... etc. The intensity of each color bands will be distributed according to the Planck’s radiation formula which is given below and details of this formulation can be found elsewhere [25] .

where is the Boltzmann constant and is the temperature of the photosphere (5800 K). The wavelength of the corresponding H, He and Ps can be obtained from Equation (1).

In order to understand the solar radiation spectrum intensively, an extensive simulation is carried out for the atomic transitions of He, Ps and H according to the Rydberg-Ritz principle (see Equation (1)). Simulation results are shown in Figures 2(a)-(c) and solar spectrum (sum of a, b and c) is depicted in (d) where components of each atomic transitions are clearly exhibited with the colour bands, but data do not illustrate the distribution of solar radiation spectrum.

Hence wavelengths which are obtained by the Rydberg-Ritz’s formula stated in Equation (1) are fed into the Planck’s radiation formula. The wavelength distributions are shown in Figures 3(a)-(c). After combining those data of Ps, He and H the solar radiation spectrum is achieved and that is revealed in (d) and consequently the area of interest (720 - 830 nm, Ps-Balmer series) is illuminated.

Theoretical contribution of H-(Balmer+Paschen), He-(Paschen+Brackett) and Ps-(Balmer) spectra in visible range of solar radiation respectively are estimated to be 37%, 41% and 22%.

Similarly experimental data are analyzed by subtracting each background from the respective colored bands and converted energy (eV) to wavelength (nm) which is depicted in Figures 4(a)-(d). In order to see the contribu-

tion of each component in the solar radiation spectrum data are fitted with Gaussian. The mean and FWHM of the Gaussian are shown in Table 3 and considered for the evaluation with a LED manufacturer’s quoted values found elsewhere [26] for better understanding.

Contribution of H-Balmer 54% in Green, H-Paschen 4.2% in Orange and 66% in Red spectra are estimated from the fitted frequencies. Similarly He-Paschen 8% in Green, 2.34% in Yellow, and He-Brackett 34% in Green, 93% in Yellow; and Ps-Balmer 1% in Yellow, 41% in Orange and 26% in Red are estimated. In total contributions of H-(Balmer + Paschen), He-(Paschen + Brackett) and Ps-(Balmer) respectively are determined to be 31%, 52% and 17% in the visible range of solar radiation spectrum.

The extremity at right hand side of each spectrum shows the temperament of Planck’s radiation formula. In order to find exact distribution of this formula more colored LEDs (Violet, Indigo and Blue) data are required. However reported results confirm a good agreement with the theoretical achievement of Ridberg-Ritz-Planck’s principle within this constraint. The differences what are merely appeared due to the diverse transitional times among H, He and Ps in the solar environment, refraction and reflection of light due to solar and earth atmospheres and statistical error due to electronics fluctuations which are not determinative. The FWHM of each Gaussian distribution represents the wide range of colors originated from the respective atoms of different transition series. The FWHM of Red spectrum shows maximum due to the widest range of different series and the highest contribution of H-Paschen (66%) series. Yellow spectrum shows minimum because of the shorter range and maximum contribution of He-Brackett (93%) series. The contribution of the He atom is maximum because

^a. Reference [26] is not the same manufacture of LEDs which are used in this experiment.

it is stable and inert. On the other hand, higher ionization probability leads H for taking part in the fusion reaction. Ps is unstable, quenching in the huge magnetic field and have the shortest lifetimes; as a result transitional probabilities of Ps are fewer than H and He. In the Orange spectrum (600 - 700 nm), around 40% contribution comes from the He-Pfund series. But I suppose this probability is very low in compare to He-Brackett and He-Paschen series in the range of visible light. Hence, it is better to think other type of lighter atoms forming in the fusion mechanisms whose binding energy (~8.25 eV) is fewer than H and greater than Ps atom. That hypothetical atom (presume Nm) will provide the color band of wavelength (600 - 700 nm) from the transition of Nm-Balmer series.