Shedding light on the X(3930) and X(3960) states with the $$B^- \rightarrow K^- J/\psi \omega $$ reaction

Author:

Abreu L. M.ORCID,Albaladejo M.ORCID,Feijoo A.ORCID,Oset E.ORCID,Nieves J.ORCID

Abstract

AbstractWe have studied the contribution of the state X(3930), coming from the interaction of the $$D \overline{D}$$ D D ¯ and $$D^{+}_s D^{-}_s$$ D s + D s - channels, to the $$B^- \rightarrow K^- J/\psi \omega $$ B - K - J / ψ ω decay. The purpose of this work is to offer a complementary tool to see if the X(3930) state observed in the $$D^+ D^-$$ D + D - channel is the same or not as the X(3960) resonance claimed by the LHCb Collaboration from a peak in the $$D^{+}_s D^{-}_s$$ D s + D s - mass distribution around threshold. We present results for what we expect in the $$J/\psi \omega $$ J / ψ ω mass distribution in the $$B^- \rightarrow K^- J/\psi \omega $$ B - K - J / ψ ω decay and conclude that a clear signal should be seen around $$3930\,\text {MeV}$$ 3930 MeV . At the same time, finding no extra resonance signal at $$3960\,\text {MeV}$$ 3960 MeV would be a clear indication that there is not a new state at $$3960\,\text {MeV}$$ 3960 MeV , supporting the hypothesis that the near-threshold peaking structure peak in the $$D^{+}_s D^{-}_s$$ D s + D s - mass distribution is only a manifestation of a resonance below threshold.

Publisher

Springer Science and Business Media LLC

Subject

Physics and Astronomy (miscellaneous),Engineering (miscellaneous)

Reference52 articles.

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3. LHCb Collaboration, E. Spadaro Norella, C. Chen, Particle Zoo 2.0: new tetra- and pentaquarks at LHCb, July, 2022. arXiv:indico.cern.ch/event/1176505

4. M. Bayar, A. Feijoo, E. Oset, The $$X(3960)$$ seen in $$D_{s}^{+} D_{s}^{-}$$ as the $$X(3930)$$ state seen in $$ D^{+} D^{-} $$. arXiv:2207.08490

5. T. Ji, X.-K. Dong, M. Albaladejo, M.-L. Du, F.-K. Guo, J. Nieves, Establishing the heavy quark spin and light flavor molecular multiplets of the $$X(3872)$$, $$Z_c(3900)$$, and $$X(3960)$$. Phys. Rev. D Ser. 106, 094002 (2022). https://doi.org/10.1103/PhysRevD.106.094002. arxiv:2207.08563

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