The orbit of the Moon is not exactly simple. First, it’s an ellipse, as you probably know already. The Earth is at one focus of the ellipse; this is why sometimes the Moon is closer, sometimes it’s farther.
This ellipse is tilted with respect to the ecliptic, not the Earth’s equator (it’s one of the few planetary satellites in that situation), by about 5.15° (it’s slightly variable). If you imagine the lunar orbit ellipse and the ecliptic as two planes, then a line is formed by their junction. It’s called the nodal line, as it joins the nodes of the Moon’s orbit: the ascending node when the Moon goes from south of the ecliptic to north of it; the descending node when it goes from north to south.
Now, imagine another line, joining the apses of the Moon’s orbit—the apogee and the perigee. This is the apsidal node.
Let’s make that move, now.
First, the Moon travels on its orbit in about 27.322 days with respect to the stars—in other words, that’s the time it takes to align with the same star again. Because the Earth travels around the Sun during that time, it takes a little more than 2 more days (total ≈ 29.530 days) to align again with the Sun, hence returning from, e.g., a new moon to another new moon.
Now, the fun begins…
The nodal line rotates around the Earth in the opposite direction of the Moon, in about 18.6 years (this rate is variable). This means the nodes are not always in line with the Sun from one revolution of the Moon to the next.
The apsidal line also rotates around the Earth, in the same direction as the Moon, in about 8.85 Earth years. This means the apses (apogee and perigee) don’t necessarily align with the Sun at each of the Moon’s revolution around the Earth.
Finally, the size of the Moon’s orbit varies with time as well, so one perigee can be closer than another one—hence the “supermoon” phenomenon that happens only a few times a year at most.
All this combines to make the Moon sometimes closer, sometimes further; sometimes more to the north, sometimes more to the south; and sometimes going north to south, sometimes going south to north, at any particular point of the celestial equator (the projection of the Earth’s equator on the celestial sphere).