Production of the $η_b(nS)$ states

Details Production of the $η_b(nS)$ states Production of the $η_b(nS)$ states

2001-04-24

arxiv.org/abs/hep-ph/0104253v5

Phys.Rev. D64 (2001) 074011; Erratum-ibid. D65 (2002) 039901

Physics

High Energy Physics

High Energy Physics - Phenomenology

8 pages, LaTeX, 1 figure, correction of version published in Phys. Rev. D (Errata sent to journal)

Scientific paper

10.1103/PhysRevD.64.074011

The rates for magnetic dipole (M1) transitions $\Upsilon(nS) \to \eta_b(n'S) + \gamma$, $n' \le n$, are compared. The photon energies for allowed ($n' = n$) M1 transitions are very small, so hindered ($n' < n$) transitions could be more favorable for discovering the $\eta_b(1S,2S)$. The question then arises whether $\Upsilon(2S)$ or $\Upsilon(3S)$ is a better source of $\eta_b(1S)$. Whereas one nonrelativistic model favors $\eta_b(1S)$ production from $\Upsilon(2S)$, this advantage is lost when relativistic corrections are taken into account, and is not common to all sets of wave functions even in the purely nonrelativistic limit. Thus, the prospects for discovering $\eta_b(1S)$ in $\Upsilon(3S)$ radiative decays could be comparable to those in $\Upsilon(2S)$ decays. We also discuss a suggestion for discovering the $\eta_b$ via $\Upsilon(3S) \to h_b(^1P_1) \pi \pi$, followed by $h_b \to \eta_b \gamma$.

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