Abstract. In Knowledge of the proton-proton (p-p) chain and CNO cycle are required for the evolution of main sequence stars during the early formation of the universe. In this study, we summarized the excitation functions of (p,γ) and (p,α) reactions for 7 Be(p,γ) 8 B, 12 C(p,γ) 13 N, 13 C(p,γ) 14 N, 14 N(p,γ) 15 O and 15 N(p,α) 15 O in p-p chain and CNO cycle using EMPIRE and TALYS computer up to 10 MeV. The calculated data on nuclear fusion cross sections in hydrogen-burning stars were compared with theoretical TENDL-2014 and ENDF/B-VII data from EXFOR. The calculation results show closed agreement between the calculations and the data from literature.Animals, plants, soil, air, planets, stars like everything formed by the basic blocks of matter called atoms. After the big bang, approximately 13.7 billion years ago, a large part of atoms formed in the early formation of the universe and came unchanged until the present day. Since the universe includes everything from subatomic particles to galaxies, from planets to stars, it is needed to be explored in detailed.All stars are born from collapsing clouds of gas and dust the interstellar medium (ISM). During their lives, they deposit energy into the ISM in the form of electromagnetic radiation and stellar winds. When they die, they return some of their matter and energy back into the ISM. The life time of stars range from a few million years for the most massive to trillions of years for the least massive [1][2][3].The amount of H and He elements in the universe are approximately 73% and 25% of the mass, respectively. After H and He, C, N and O elements are the most abundant elements in the Universe. Energy production in massive stars is governed by the CNO cycles throughout most of their lifetimes [4]. Hydrogen and helium elements having low-mass were produced in the hot and dense conditions of the birth of the universe itself. The life of stars is described in terms of nuclear reactions.The Hydrogen burning mechanism is essentially the nuclear fusion of four protons into one 4 He nucleus. There are two reaction chains that can convert hydrogen to helium, namely the proton-proton (or pp chain) chain, also called pp reaction, and the CNO cycle. The pp chain is more important in stars the mass of the Sun or less and stars of similar mass The CNO cycle by which stars convert hydrogen to helium is the dominant source of energy in more massive stars [5].The p-p fusion is the nuclear fusion process which fuels the Sun and other stars which have core temperatures less than 15×10 6 K and a reaction cycle at energy of 25 MeV. The p-p chains occur under lower temperature than the carbon-nitrogen-oxygen cycle. The pp chain in stars like our Sun divides into three main branches, called as the ppI, ppII and ppIII chains. These are given Eq. 1-3. According to Eq. 1, in the protonproton fusion reaction inside stars like the sun, the first step in ppI process is the collision of two protons (p or 1 H) to make an atom of heavy hydrogen ( 2 H). The second step contain...