Dr. Yohsida said that his simulations were the first to be able to follow the complex interactions of gas and radiation that dominate evolution of the protostar.
Numerical simulations were the main method adopted to achieve this objective.
The observations used to validate the historical simulations were the NOAA OI SST data over the period 1 January 1982 to 5 July 2016, averaged over the SEAus region.
Other features examined in the simulations were the effect of initial stresses and defects resulting from the material manufacturing process.
Considered in the simulations were the influence of the volume percentage of fractures, the length of fractures, the relative location of the water table, and the influence of pulsed pumping.
Other settings of the WRF simulations were the same as the settings of the original simulation described in subsection 2c.
Some of the important parameters used in the above simulations were the absorption coefficient at the pump excitation wavelength α = 8×104 cm−1[30], and the ambipolar diffusion coefficient D = 0.6 cm2 s−1[31].
The fourth and fifth simulations were the same as the second simulation, except for the more frequent use of the reusable scope 1 in the fourth simulation (2/3 vs. 1/3) and the more frequent use of the reusable scope 2 in the fifth simulation (2/3 vs. 1/3).
