I cannot figure out how the sun can rise or set with the version of a flat earth as accepted by this website (the standard monopole flat earth map,

https://wiki.tfes.org/File:Map.png).

The maps on this website do not contain any dimensions. However, from what I have been able to gather, the earth is a flat circular disc with a diameter of approximately 20,000 km. I get to this number by assuming that the equator is 10,000 km from the North Pole, and the southern ice wall is the same distance from the equator. At least, that is how your published maps look.

I have also seen various figures for the altitude of the sun, ranging from 1,100 km (700 mi) to 6,400 km (4,000 mi). For the rest of this question I will assume 1,100 km as that is the best case for FE; any higher figure makes sunset even more impossible.

Now let us consider how the sun looks for someone at the North Pole. The furthest that the sun can possibly be away from the North Pole is 20,000 km, assuming it ever got near the southern ice wall. No FE maps show the sun that far south, but again, this is the best scenario for FE. Now, if the sun is 1,100 km high at a distance of 20,000 km, the angle between the horizon and the sun is given by simple trigonometry, as follows:

A = atan(1100/20000) = 3 degrees

If we assume the sun sits at an altitude of 6,400 km then we get

A = atan(6400/20000) = 18 degrees

In other words, even in the best (for FE) case, we can NEVER see the sun less than 3 degrees above the horizon. If the observer is farther south, or if we look at the sun at sunset instead of at midnight, the observer will be closer to the sun, and hence the sun will appear even higher above the horizon. For example, if the sun is 4,000 km high, and the observer is 4,000 km away from it (horizontally) at sunset, then the sun will "set" at an elevation of 45 degrees above the horizon.

Hence my question: please explain how we can ever see the sun sink below the horizon. If any of my numbers are wildly wrong, please feel free to show me the correct calculations.