Editing Appendix/Ramblings/T1Coordinates (section)

==Preamble==

In the mid-1990s I invested time trying to gain a better understanding of the "<math>3^\mathrm{rd}</math> Integral of Motion" that is discussed especially in the context of galaxy dynamics.  For example, [[User:Tohline/Appendix/References#BT87|BT87]] discuss the behavior of particle orbits in static potentials in which equipotential contours are nested oblate spheroidal surfaces with uniform eccentricity.  This set of equipotential contours does not conform to, and therefore cannot be defined by, the traditional ''Oblate Spheroidal'' Coordinate system &#8212; detailed, for example, in MF53 &#8212; because in that traditional coordinate system surfaces of constant <math>\xi_1</math> are ''confocal'' rather than concentric oblate spheroids.  In an effort to uncover a closed-form mathematical prescription for the "<math>3^\mathrm{rd}</math> integral" in this case, I developed an orthogonal coordinate system in which surfaces of constant <math>\xi_1</math> are ''concentric'' oblate spheroids.  The properties of this ''T1'' coordinate system are detailed in the Appendix of the [http://www.phys.lsu.edu/astro/H_Book.current/H_Book.html original version] of this H_Book.  Here are two relevant links:
* [http://www.phys.lsu.edu/astro/H_Book.current/Appendices/Mathematics/operators.text.shtml Original presentation of ''T1 Coordinates'']; (This page of ''shtml'' text may only be viewable using Internet Explorer.)
* [http://www.phys.lsu.edu/astro/H_Book.current/Appendices/Mathematics/operators.tohline1.pdf PDF-formatted presentation of ''T1 Coordinates'']
I have just realized (in May, 2010) that there is a connection between this T1 Coordinate system and the equipotential contours that arise from at least one of the equilibrium models of the axisymmetric structure of rotationally flattened isothermal gas clouds presented by Hayashi, Narita &amp; Miyama (1982; hereafter HNM82).  What follows is a discussion of this connection.