I have found 2 definitions of Eclipse Magnitude in total eclipse:

Solar eclipse for example, below we define $r_1$ as the radius of the Sun, $r_2$ as the radius of the Moon's Shadow, $d$ as the distance of Sun's center and Moon's center

if it is a partial eclipse, the Eclipse Magnitude have no objection:

$$ \epsilon = \frac{r_1 + r_2 - d}{2r_1} $$

Definition 1:

After the Sun is totally blocked, the Eclipse Magnitude jumps from $1$ to $r_2/r_1$, which is the ratio of Moon and Sun's diameter

http://www.jgiesen.de/eclipse/

https://www.oxfordreference.com/display/10.1093/oi/authority.20110803100126148

Definition 2:

After the Sun is totally blocked, the Eclipse Magnitude is still:

$$ \epsilon = \frac{r_1 + r_2 - d}{2r_1} > 1,\quad 0 \leq d \leq r_2 - r_1 $$

only if the Sun and Moon's center overlap, will $d = 0$, and $\epsilon = \epsilon_{max} = \dfrac{r_1 + r_2}{2r_1}$, but this will still be less than $r_2/r_1$

This provide a continuous definition of eclipse magnitude, on the other hand, in an annular solar eclipse, the Eclipse Magnitude is always $r_2/r_1$, having nothing to do with $d$, but this is continuous

https://www.geogebra.org/m/SnZ7QGTJ

Which one is right? I didn't find any books or professional articles defines the calculation of Eclipse Magnitude, Thanks!

The core question I think is: a total eclipse, especially lunar total eclipse, while the earth's umbra is much larger than the moon.

Then the magnitude will be larger if the center of the Moon and the center of the Earth's umbra are closer together See Bottom Figure

(comparing if the moon is close to the edge of the umbra See Top Figure) if using Definition II.

In Definition I, the magnitude will have nothing to do with center distance, as long as the moon is all in the earth's shadow.