separation between band pairs, $2z$; and (v) the solar elongation angle of the line of sight, $\epsilon$: see Equations (1) and (2) of @Reach92. For AKARI observations at constant solar elongation, $\epsilon \sim 90\degree$, the average latitude of the northern and southern bands (the midplane of the band pairs) is $$\tan\beta = -\frac{R}{\sqrt{R^2-1}}~\tan i~\sin\left(\lambda-\Omega\pm\sin^{-1}\frac{1}{R}\right),$$ where $\lambda$ is the geocentric ecliptic longitude of the line of sight, and the plus/minus signs in the $\pm$ notation refer to the Earth-leading/trailing direction: see Equation \[3\] of @Reach92. Generally, the heliocentric distance of the dust band ($R$) is determined as a parallactic distance from the band-pair latitudes and the solar elongation angle ([@Reach92; @Reach97; @Spiesman95]). Since most AKARI scans were limited to a constant solar elongation, $\epsilon \sim 90\degree$, it is difficult to determine the parallactic distance based on the AKARI data. Instead, the phase difference, $\Delta\phi$, between the annual variation of the average latitude of the band pair for scans leading and trailing the Earth can be used to measure the heliocentric distance of the bands, $R$ [@Reach91]: $$\Delta\phi = 2~\tan^{-1}~\sqrt{R^2-1}.$$ Once we obtain the heliocentric distance of the band pair ($R$), we can derive the inclination, $i$, and the ascending node, $\Omega$. 