TY - JOUR

T1 - Instability of rotating Bose stars

AU - Dmitriev, A. S.

AU - Levkov, D. G.

AU - Panin, A. G.

AU - Pushnaya, E. K.

AU - Tkachev, I. I.

N1 - Funding Information: Instabilities of rotating Bose stars were studied within the framework of the RSF Grant No. 16-12-10494. The rest of this paper was funded by the Foundation for the Advancement of Theoretical Physics and Mathematics “BASIS.” Numerical calculations were performed on the computational cluster of the Theory Division of Institute for Nuclear Research RAS. Publisher Copyright: © 2021 American Physical Society.

PY - 2021/7/15

Y1 - 2021/7/15

N2 - Light bosonic (axionlike) dark matter may form Bose stars - clumps of nonrelativistic Bose-Einstein condensate supported by self-gravity. We study rotating Bose stars composed of condensed particles with nonzero angular momentum l. We analytically prove that these objects are unstable at arbitrary l≠0 if particle self-interactions are attractive or negligibly small. They decay by shedding off the particles and transporting the angular momentum to the periphery of the system until a Saturn-like configuration appears: One (or several) spin-zero Bose stars and clouds of diffuse particles orbit around the mutual center. In the case of no self-interactions, we calculate the profiles and dominant instability modes of the rotating stars: numerically at 1≤l≤15 and analytically at l≫1. Notably, their lifetimes are always comparable to the inverse binding energies; hence, these objects cannot be considered long-living. Finally, we numerically show that in models with sufficiently strong repulsive self-interactions the Bose star with l=1 is stable.

AB - Light bosonic (axionlike) dark matter may form Bose stars - clumps of nonrelativistic Bose-Einstein condensate supported by self-gravity. We study rotating Bose stars composed of condensed particles with nonzero angular momentum l. We analytically prove that these objects are unstable at arbitrary l≠0 if particle self-interactions are attractive or negligibly small. They decay by shedding off the particles and transporting the angular momentum to the periphery of the system until a Saturn-like configuration appears: One (or several) spin-zero Bose stars and clouds of diffuse particles orbit around the mutual center. In the case of no self-interactions, we calculate the profiles and dominant instability modes of the rotating stars: numerically at 1≤l≤15 and analytically at l≫1. Notably, their lifetimes are always comparable to the inverse binding energies; hence, these objects cannot be considered long-living. Finally, we numerically show that in models with sufficiently strong repulsive self-interactions the Bose star with l=1 is stable.

UR - http://www.scopus.com/inward/record.url?scp=85109265807&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.104.023504

DO - 10.1103/PhysRevD.104.023504

M3 - Article

AN - SCOPUS:85109265807

VL - 104

JO - Physical Review D

JF - Physical Review D

SN - 2470-0010

IS - 2

M1 - 023504

ER -