Phi Cassiopeiae
Star in the constellation Cassiopeia
From Wikipedia, the free encyclopedia
Phi Cassiopeiae is a multiple star system in the northern constellation of Cassiopeia. Its name is a Bayer designation that is Latinized from φ Cassiopeiae, and abbreviated Phi Cas or φ Cas. With a combined apparent magnitude of +4.95, it is visible to the naked eye. The two brightest components are A and C, sometimes called φ1 and φ2 Cas. φ Cas A is an F0 bright supergiant of magnitude 4.95 and φ Cas C is a 7.08 magnitude B6 supergiant at 134".
System
φ Cassiopeiae appears among the stars of the open cluster NGC 457, which located at a distance of 7,800 light-years (2,400 pc), but it is uncertain whether φ Cas is a member of this cluster.[13] φ Cas is generally treated as having five component stars, designated A to E in order of distance from the brightest star. The two components A and C are the brightest stars in the field of NGC 457; they are sometimes referred to as φ1 and φ2 Cassiopeiae.[15] Component B is a 12th magnitude star 49" from φ1.
Components D and E and both 10th magnitude B-type main sequence stars in the field of NGC 457, with component E only 42" from φ2. Another three components are sometimes listed as components of the multiple system, although this is somewhat arbitrary with dozens of members of NGC 457 being found within a few arc-minutes.[16]
The two supergiants, components A and C, share a similar space motion to the other stars in NGC 457, but their evolutionary status and brightness makes them unlikely members.[10] Their Gaia Data Release 2 parallaxes are comparable to other stars in the cluster and consistent with the accepted distance of NGC 457,[17] and component C has been given a 70% likelihood of being a member of the cluster.[18]
Properties
The primary component of the φ Cassiopeiae system is a very luminous yellow supergiant. Its absolute magnitude is comparable to some yellow hypergiants but it does not show the level of mass loss and instability that would qualify it as a hypergiant itself. Various model atmospheres all give a temperature around 7,300K, a low surface gravity, a radius around 250 R☉, and a luminosity well over 100,000 L☉. More uncertain is the mass, which would be expected to have been well over 25 M☉ initially, but much less now. Different authors have published values from 6 M☉ to 17 M☉.[10][11]
Component C is a relatively typical B class supergiant, 83,000 times the luminosity of the sun. It is a suspected variable and a suspected spectroscopic binary.[19]