TY - JOUR

T1 - Myers–Perry black holes with scalar hair and a mass gap

T2 - Unequal spins

AU - Herdeiro, Carlos

AU - Kunz, Jutta

AU - Radu, Eugen

AU - Subagyo, Bintoro

N1 - Publisher Copyright:
© 2015 The Authors

PY - 2015/9/1

Y1 - 2015/9/1

N2 - We construct rotating boson stars and Myers–Perry black holes with scalar hair (MPBHsSH) as fully non-linear solutions of five dimensional Einstein gravity minimally coupled to a complex, massive scalar field. The MPBHsSH are, in general, regular on and outside the horizon, asymptotically flat, and possess angular momentum in a single rotation plane. They are supported by rotation and have no static limit. Such hairy BHs may be thought of as bound states of boson stars and singly spinning, vacuum MPBHs and inherit properties of both these building blocks. When the horizon area shrinks to zero, the solutions reduce to (in a single plane) rotating boson stars; but the extremal limit also yields a zero area horizon, as for singly spinning MPBHs. Similarly to the case of equal angular momenta, and in contrast to Kerr black holes with scalar hair, singly spinning MPBHsSH are disconnected from the vacuum black holes, due to a mass gap. We observe that for the general case, with two unequal angular momenta, the equilibrium condition for the existence of MPBHsSH is w=m1Ω1+m2Ω2, where Ωi are the horizon angular velocities in the two independent rotation planes and w,mi, i=1,2, are the scalar field's frequency and azimuthal harmonic indices.

AB - We construct rotating boson stars and Myers–Perry black holes with scalar hair (MPBHsSH) as fully non-linear solutions of five dimensional Einstein gravity minimally coupled to a complex, massive scalar field. The MPBHsSH are, in general, regular on and outside the horizon, asymptotically flat, and possess angular momentum in a single rotation plane. They are supported by rotation and have no static limit. Such hairy BHs may be thought of as bound states of boson stars and singly spinning, vacuum MPBHs and inherit properties of both these building blocks. When the horizon area shrinks to zero, the solutions reduce to (in a single plane) rotating boson stars; but the extremal limit also yields a zero area horizon, as for singly spinning MPBHs. Similarly to the case of equal angular momenta, and in contrast to Kerr black holes with scalar hair, singly spinning MPBHsSH are disconnected from the vacuum black holes, due to a mass gap. We observe that for the general case, with two unequal angular momenta, the equilibrium condition for the existence of MPBHsSH is w=m1Ω1+m2Ω2, where Ωi are the horizon angular velocities in the two independent rotation planes and w,mi, i=1,2, are the scalar field's frequency and azimuthal harmonic indices.

UR - http://www.scopus.com/inward/record.url?scp=84984879095&partnerID=8YFLogxK

U2 - 10.1016/j.physletb.2015.06.059

DO - 10.1016/j.physletb.2015.06.059

M3 - Article

AN - SCOPUS:84984879095

SN - 0370-2693

VL - 748

SP - 30

EP - 36

JO - Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics

JF - Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics

ER -