The orbit of the A and B components is so close that together they are seen as a single star in this image. This combined multiple is a magnitude 4.92 white star and it is bright enough to be visible to the naked eye.
The primary, μ Dra A is an F-type main sequence star with a spectral type of F6V.
The closest companion star, μ Dra B, orbits so close to the primary that it does not show up in this image as a separate star. The B component is itself a spectroscopic binary and its two components are given the designations μ Dra Ba and μ Dra Bb.
μ Draconis A and Ba are nearly indentical F type stars. They are the same spectral type (F6V) and shine at magnitudes 5.66 (A) and 5.69 (B). The combined flux from all stars in the system is 4.92 in the visual band.
The furthest component from the primary, μ Dra C, is barely visible in the main image above. In the main image above, the C star is just a small bulge of light below the center of the primary and slightly to the left. It is will within the glare zone of the main star so to see it, you need to zoom in quite a bit.The close-up shown here is a cropped and reprocessed version of Mu Draconis. It is taken from the same data used to make the main image above. In this version, most of the glare has been removed from the AB component, and the position and orange hue of the C component are clearly visible. μ Dra C is listed in SIMBAD as being a high proper motion star with the spectral type M3. It is magnitude 11.7 in the visual band.
