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We fit an isothermal oscillatory density model of Neptune's protoplanetarydisk to the surviving regular satellites and its innermost ring and wedetermine the radial scale length of the disk, the equation of state and thecentral density of the primordial gas, and the rotational state of theNeptunian nebula. Neptune's regular moons suffered from the retrograde captureof Triton that disrupted the system. Some moons may have been ejected, whileothers may have survived inside their potential minima. For this reason, theNeptunian nebula does not look like any of the nebulae that we modeledpreviously. In particular, there must be two density maxima deep inside thecore of the nebula where no moons or rings are found nowadays. Even with thisstrong assumption, the recent discovery of the minor moon N XIV complicatesfurther the modeling effort. With some additional assumptions, the Neptuniannebula still shares many similarities with the Uranian nebula, as was expectedfrom the relative proximity and similar physical conditions of the two systems.For Neptune's primordial disk, we find a steep power-law index ($k=-3.0$),needed to accommodate the arrangement of the outer moons Larissa, N XIV, andProteus. The rotation parameter that measures centrifugal support againstself-gravity is quite small ($\beta_0=0.00808$), as is its radial scale length(13.6 km). The extent of the disk ($R_{\rm max}=0.12$ Gm) is a lot smaller thanthat of Uranus ($R_{\rm max}=0.60$ Gm) and Triton appears to be responsible forthe truncation of the disk. The central density of the compact Neptunian coreand its angular velocity are higher than but comparable to those of Uranus'core. In the end, we compare the models of the protoplanetary disks of the fourgaseous giants.

Model of Neptune's protoplanetary disk forming in-situ its surviving  regular satellites after Triton's capture and comparison of the  protoplanetary disks of the four gaseous giants