How to derive Kepler's 1st Law? I was going through the derivation of Kepler's 1st Law in the textbook &quot;An Introduction to Modern Astrophysics&quot; by Carroll and Ostlie. From there, I got stuck in a few places in their derivation as I found it confusing. In total, I have 2 questions.

Q1: In the second sentence that I highlighted, it is mentioned that when equation 29 is translated into a physical standpoint, it implies that &quot;both objects in a binary orbit move about the centre of mass in ellipses, with the centre of mass occupying one focus of each ellipse&quot; however I don't see how the physical implications of equation 29 will translate into this that they claim. This equation clearly only describes the position vector of the reduced mass, so how can it be extrapolated to talk about the motion of a binary system when there are 2 masses rather than 1 reduced mass. (Clarification: I am aware that reduced mass is a way to model binary systems, but in this case I don't see the link between the motion of the reduced mass and the motion of 2 bodies)
Q2: On the very last line, it is mentioned that &quot;L is at minimum as eccentricity approaches unity, as expected&quot;. However I don't see the qualitative reasoning as to why this would be &quot;expected&quot;. Is there a physical or physics explanation as to why we expect an orbit with a large eccentricity to have a lower angular momentum than one with a low eccentricity?
I must say that I agree with you, this way of derivate the Kepler law is not the most intuitive, it's maybe for this reason they specify: &quot;revisited&quot;.
R1: The reason is stated at the very begin of the chapter, where you derive the relation between $r$ and the angle to the perihelion $\theta$ for the general case of an ellipse (Eq 3 in your book in Cap 2.1 Elliptical orbit, but I can see I have an older version than yours), where:
$$ r = \frac{a(1-e^2)}{1+e\,cos(\theta)}$$
here, the eccentricity of a ellipse is then define as:
$$ e = \sqrt{1- \frac{b^2}{a^2}}$$
in the case of Kepler's law you can define the eccentricity as $e = D/\mu G M$ and  $a$ as:
$$ a = \frac{L^2 G\, M}{\mu^2\,G^2\,M^2 - D^2}$$
and you can work out in equation (29), obtaining the equation in the same form as for an elliptical orbit.
The reason to derive $r$ is because it indicates the distance of the object from the focal point (centre of mass of the system), which in the case of the solar system, is the distance of the planet to the Sun (actually the focal point of the solar system, or better to say of the Sun-Jupiter system, is a few kilometre above the solar surface).
R2: the eccentricity $e$ quantify the shape of a cone cross-section Eccentricity (math) Wikipedia.
For example, in the case of the an ellipse you have $0 &lt; e &lt; 1$, and it indicates how much the ellipse is &quot;squashed&quot;. Another example, if you have $e=0$ than you have a circle.
In the case of $e=1$ you have a parabola, from the equation of $e$ above it means that $a\gg b$. In a more physics sense, it means that the system is not in a gravitationally bounded state, and the less massive object $m_1 \ll m_2$ is on a parabolic trajectory, deviated by the gravitational pull of $m_2$, and will not stay in orbit.