Using the Scale-Symmetric Theory (SST), we argue for the tower of the Chandrasekhar limits as the origin of the helium-rich hot subdwarfs in omega Centauri cluster. The structure of bare muons described within SST leads to the hot blue stars with a mass of 0.465 solar masses. Previously we showed that stars with masses of 1.395, 11.20 and 0.891 solar masses should behave as the Type Ia supernovae i.e. after the explosion of such stars there should not be created a neutron star as a remnant. Stars with a mass of 0.465 solar masses are the untypical supernovae. They are the remnants of the exploding stars with a mass of 0.891 solar masses which lose their outer hydrogen layers. Their mass is too small to cause a collapse and next explosion as it is for higher Chandrasekhar limits. But the 3-component weak mass (a ball/condensate composed of the confined Einstein-spacetime components that is entangled with two rotating neutrinos) in muons (for mass equal to 0.465 solar masses there appears a maximum for number density of such 3-component systems and each component carries energy equal to 17.61 MeV) is a catalyst for fusions of three alpha particles into carbon-12 (the last experimental data show that any nonzero amount of coherence in a system can be converted into an equal amount of entanglement between that system and another initially incoherent one). Due to such fusions, surfaces of the untypical supernovae are very hot (a narrow temperature range from 35,000 K to 40,000 K). They are the extreme horizontal branch (EHB) stars.