👉 Telescope math involves calculating the magnification and resolution of a telescope, which are crucial for observing distant celestial objects. Magnification is determined by the ratio of the focal length of the eyepiece to that of the objective lens or mirror, often expressed as \( M = \frac{f_o}{f_e} \), where \( f_o \) is the focal length of the objective and \( f_e \) is that of the eyepiece. Higher magnification allows for more detailed views but can also reduce light-gathering ability and increase image distortion. Resolution, on the other hand, is the telescope's ability to distinguish between two closely spaced objects and is given by the formula \( \theta = 1.22 \frac{\lambda}{D} \), where \( \lambda \) is the wavelength of light and \( D \) is the diameter of the telescope's aperture. Larger apertures improve resolution, enabling clearer and more detailed images of distant stars and galaxies.
