Sentence examples for density of the disk from inspiring English sources

The surface density of the disk increases, while the compressional energy is radiated away by H2 line emission.

As in the previous subsection, we assume that the surface density of the disk is given by a power law of r, i.e., the form of Eq. (1).

They limited themselves to the case where the surface density of the disk depends on the radial distance from the central star r as.

Formally, the radial mass distribution of the disk is given by the same law as in the case of Y07, i.e., by a power-law function of r with an index γ: (1 where Σ is the surface density of the disk and Σ0 is that at r = 1 AU.

Although Y07 is the first work in which the effect of the stellar wind is taken into account, their study has been found wanting for the following reasons; (1) They limited themselves to the case where the surface density of the disk depends on the radial distance from the central star r as.   (2) They limited themselves to the case where the wind velocity is constant.

This means that the data density of the disk's surface can be increased immensely.

When H2 is used as carrier gas, an entirely rough laminar pyrolytic carbon matrix and C/C disks with average bulk density of 1.67 g/cm3 are obtained in the same time, and the radial density difference of the disk is only 0.11 g/cm3.

When N2 is used as carrier gas, the average bulk density of the carbon disk is 1.54 g/cm3 after 400-h infiltration, and the radial density difference of the disk is 0.24 g/cm3.

where (sigma (r) (= int _{-infty }^{infty } rho dz)) is the surface density of the nebula disk, (H r) = sqrt {2} c/Omega _{mathrm {K}}) is the disk scale height, Ω K=(G M ∗/r 3 1/2 is the Keplerian angular velocity, and G is the gravitational constant.

The spectral density distribution of the disk around Vega.

Prior to the experiment, the density of the silica disk was determined by Archimedes' method to be 2.208 g/cm3.