The Solar Wind Mass-Loss Rate from In Situ Densities and Speeds, and Its Integrated Effect Over the Solar Lifetime

This paper computes the solar wind mass-loss rate from in situ densities and speeds, and its integrated effect over the solar lifetime from published solar observations and places the result against the density, shear and energy scales of the torsion bounce frame. The headline values are: mdot slow kg s = 9.408e+08; mdot fast kg s = 1.058e+09; mdot solar masses per yr = 1.493e-14; cumulative fraction 4p6Gyr = 6.868e-05; particles per s slow = 5.625e+35; ram pressure slow nPa = 1.34. The central density of the Sun, 150 grams per cubic centimetre, stands at a fraction 1.54e-53 of the neutron-branch bound density of 9.72e+54 grams per cubic centimetre, and the quantity treated here inherits that separation: conventional solar physics accounts for the observed value completely, and no bound-derived correction reaches a level that current or foreseeable observations could register. The result is therefore negative with respect to the bound and positive with respect to the solar accounting, which closes with the numbers shown. This study is simulated and computed from stated assumptions and published values; it is not a measurement.