Caption: A diagram of a gravitational 2-body system with the spherically-symmetric bodies orbiting in elliptical orbits the system center of mass marked by a red cross. The center of mass is at rest in celestial frame (i.e., inertial frame) of the gravitational 2-body system. The at rest is also the common focus of the elliptical orbits. The other focuses for the elliptical orbits are just empty points in physical space with NO special significance.

Features:

1. The elliptical orbits of this gavitational two-body system are determined by Newtonian physics (what is universal about the physical system) and initial conditions (what is peculiar or individual about the physical system).

2. Gravity is, of course, the force that pulls the astro-bodies into orbits.

3. Now in astro jargon, an apsis (plural apsides) is an extreme point in the orbit of an astro-body.

   The two kinds of apsides are periapsis and apoapsis.

4. The periapsis (AKA pericenter) is the arrangement of closest separation and the term is also sometimes used for the closest separation distance.

5. The apoapsis (AKA apocenter) is the arrangement of farthest separation and the term is also sometimes used for the farthest separation distance.

   A physical fact for orbits is that astro-bodies move slowest at apoapsis and fastest at periapsis.

6. The apse line (AKA line of apsides is drawn through the periapsis and apoapsis.

7. In the analysis of gavitational two-body systems, people usually use the relative orbit of the smaller astro-body to the larger astro-body.

   A relative orbit is also an elliptical orbit if the non-relative orbit is.

   You will have imagine the relative orbit since it is NOT shown in the diagram.

8. By normal convention, the relative orbit mean orbital radius (AKA relative semi-major axis) is defined to be

           r_mean = (1/2)( r_periapsis + r_apoapsis ), 

   where r_periapsis is the periapsis separation and r_apoapsis is the apoapsis separation.

9. The relative elliptical orbit with mean orbital radius r_mean has periapsis and apoapsis distances given by, respectively,

             r_periapsis = r_mean*(1 - e)   and   r_apoapsis = r_mean*(1 + e) , 

   where e is the eccentricity of the relative elliptical orbit.

10. The actual elliptical orbits relative to the center of mass are scaled down versions of the relative elliptical orbit. The scale radii for any epoch are

                 r_1 = r*(m_2/m) and r_2 = r*(m_1/m) , 

    where 1 is the index for astro-body 1, 2 is the index for astro-body 2, r is the relative separation distance, and m = m_1+m_2 is the total mass. As you can see, if m_1 >> m_2, we have r_1 ≅ 0 and r_2 ≅ r. This just shows that if m_1 >> m_2, we effectively have astro-body 2 orbiting astro-body 1 which is effectively at rest at the center of mass.

11. In most real orbits, astronomical perturbations cause noticeable deviations from exact gavitational two-body system behavior.

12. There are special-case names for the apsides of familiar astronomical objects (see Wikipedia: Apsis: Terminology). But yours truly thinks mostly these are overly fancy, except for the most familiar astronomical objects: e.g.,
    1. Earth: perigee and apogee, where suffix gee is derived from Greek Earth goddess Gaia.
    2. Sun: perihelion and aphelion, where suffix helion is derive from Greek Sun god Helios.
    3. star: periastron and apastron, where suffix astron is ancient Greek language word for star.

    Other than the example cases, if one wants a fancy name, yours truly suggests just prefix the name by peri- or ap-: e.g., peri-Jupiter and ap-Jupiter.