This is a lower luminosity supergiant star with a stellar classification of B1 Ib.[3] This is an enormous star, with an estimated 26–27[8] times the Sun's radius and 13–16 times the Sun's mass.[7] It has about 47,000 times the luminosity of the Sun and it is radiating this energy at an effective temperature of 20,800 K,[7] giving it the blue-white hue of a B-type star.[11] The spectrum displays anomalously high levels of carbon.[12] Zeta Persei has a strong stellar wind that is expelling 0.23 × 10−6 times the mass of the Sun per year, or the equivalent of the Sun's mass every 4.3 million years.[13]
Zeta Persei has a 9th magnitude companion at an angular separation of 12.9 arcseconds. The two stars have the same proper motion, so they may be physically associated. If so, they are separated by at least 4,000 Astronomical Units.[14] Zeta Persei is a confirmed member of the Perseus OB2 association (Per OB2), also called the Zeta Persei association, which is a moving group of stars that includes 17 massive, high luminosity members with spectral types of O or B, giving them a blue hue. These stars have a similar trajectory through space,[4] suggesting they originated in the same molecular cloud and are about the same age.[15]
^"The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on 2013-12-03, retrieved 2012-01-16
^Jaschek, M.; Jaschek, C. (December 1974), "The CNO stars", Astronomy and Astrophysics, 36 (3): 401–408, Bibcode:1974A&A....36..401J
