The Bahcall–Wolf solution applies to a nucleus consisting of stars of a single mass. If there is a range of masses, each component will have a different density profile. There are two limiting cases. If the more massive stars dominate the total density, their density will follow the Bahcall–Wolf form, whereas the less-massive objects will have ρ ∝ ∝ r. If the less massive stars dominate the total density, their density will follow the Bahcall–Wolf form, whereas the more-massive stars will follow ρ ∝ ∝ r.