It is visible to the naked eye as a faint, white-hued star with a typical apparent visual magnitude of 4.66.

[2] This object is moving closer to the Earth with a heliocentric radial velocity of −26 km/s.

However, Gray & Garrison (1989) found a class of kA5hA7mA7 (IV–V),[4] which matches a blend of subgiant and main sequence luminosity classes with the K-line (kA5) of an A5 star and the hydrogen (hA7) and metal (mA7) absorption lines of an A7 star.

[a] It is radiating 62 times the Sun's luminosity from its photosphere at an effective temperature of 7,685 K.[7] It is an Alpha2 Canum Venaticorum-type variable with magnitude ranging from 4.62 down to 4.67 over a period of 14 days.

[3] There is evidence that 15 Vulpeculae may have a companion star, given the high margins of error in the astrometric measurements taken by Gaia DR3, as well as its unusually slow projected rotational velocity, which could also be explained if the star is being viewed pole-on.