REACTIONS THAT GENERATE SOLAR WIND ¹H AND LUMINOSITY FROM THE SUN’S CENTRAL NEUTRON STAR

1. For solar neutrinos from the pep cycle:

a. Neutrons escape from the NS, <¹n> —> ¹n

b. Free neutrons decay, ¹n —> ¹H⁺+ e^- + n_anti

c. Hydrogen fusion, 4 ¹H⁺ + 2 e^- —> ⁴He⁺⁺ + 2 n

d. Some H⁺ reaches the surface and departs in the solar wind

2. For solar neutrinos from other proton capture reactions:

a. Neutrons escape from the NS, <¹n> —> ¹n

b. Free neutrons decay, ¹n —> ¹H⁺ + e^- + n_anti

c. Proton capture, e.g., ¹H⁺ + _ZX —> _Z+1Y —> ^A+1X + n + b⁺

d. Some H+ reaches the surface and departs in the solar wind

3. If neutron capture reactions occur before all neutrons decay:

a. Neutrons escape from the NS, <¹n> —> ¹n

b. N-capture, e.g., ¹n + ^AX —> ^A+1X —> ^A+1Y + e^- + n_anti

c. Free neutrons decay, ¹n —> ¹H⁺ + e^- + n_anti

d. H-fusion by reactions 1c. or 2c., above.

e. Some H⁺ reaches the surface and departs in the solar wind