恒星视差是天文学中因为恒星距离产生视差的效应。它是恒星际尺度的视差，经由天文测量学，视差可以直接测量出一颗恒星与地球的准确距离。它曾是天文学辩论了数百年的议题，但是因为太困难了，在19世纪初期才取得了最接近几颗恒星的值。即使在21世纪，恒星视差的测量已经达到银河系的尺度，但大多数的距离测量还是经由红移的计算或是其它的方法。

视差通常是由地球在轨道上不同的位置，导致观察到近距离的恒星相对于遥远的天体移动到不同位置获得的。经由观察视差，测量角度和利用三角学，可以测量不同物体在空间中的距离，通常是恒星，但在太空中的其它天体也可以。

Stellar parallax is parallax on an interstellar scale: the apparent shift of position of any nearby star (or other object) against the background of distant objects. Created by the different orbital positions of Earth, the extremely small observed shift is largest at time intervals of about six months, when Earth arrives at exactly opposite sides of the Sun in its orbit, giving a baseline distance of about two astronomical units between observations. The parallax itself is considered to be half of this maximum, about equivalent to the observational shift that would occur due to the different positions of Earth and the Sun, a baseline of one astronomical unit (AU).