56,105 research outputs found

    Meson decay in a corrected 30P3^P_0 model

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    Extensively applied to both light and heavy meson decay and standing as one of the most successful strong decay models is the 30P3^P_0 model, in which qqΛ‰q\bar{q} pair production is the dominant mechanism. The pair production can be obtained from the non-relativistic limit of a microscopic interaction Hamiltonian involving Dirac quark fields. The evaluation of the decay amplitude can be performed by a diagrammatic technique for drawing quark lines. In this paper we use an alternative approach which consists in a mapping technique, the Fock-Tani formalism, in order to obtain an effective Hamiltonian starting from same microscopic interaction. An additional effect is manifest in this formalism associated to the extended nature of mesons: bound-state corrections. A corrected 30P3^P_0 is obtained and applied, as an example, to b1→ωπb_{1}\to\omega\pi and a1→ρπa_{1}\to\rho\pi decays.Comment: 3 figures. To appear in Physical Review

    Strong evidences for a nonextensive behavior of the rotation period in Open Clusters

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    Time-dependent nonextensivity in a stellar astrophysical scenario combines nonextensive entropic indices qKq_{K} derived from the modified Kawaler's parametrization, and qq, obtained from rotational velocity distribution. These qq's are related through a heuristic single relation given by qβ‰ˆq0(1βˆ’Ξ”t/qK)q\approx q_{0}(1-\Delta t/q_{K}), where tt is the cluster age. In a nonextensive scenario, these indices are quantities that measure the degree of nonextensivity present in the system. Recent studies reveal that the index qq is correlated to the formation rate of high-energy tails present in the distribution of rotation velocity. On the other hand, the index qKq_{K} is determined by the stellar rotation-age relationship. This depends on the magnetic field configuration through the expression qK=1+4aN/3q_{K}=1+4aN/3, where aa and NN denote the saturation level of the star magnetic field and its topology, respectively. In the present study, we show that the connection qβˆ’qKq-q_{K} is also consistent with 548 rotation period data for single main-sequence stars in 11 Open Clusters aged less than 1 Gyr. The value of qK∼q_{K}\sim 2.5 from our unsaturated model shows that the mean magnetic field topology of these stars is slightly more complex than a purely radial field. Our results also suggest that stellar rotational braking behavior affects the degree of anti-correlation between qq and cluster age tt. Finally, we suggest that stellar magnetic braking can be scaled by the entropic index qq.Comment: 6 pages and 2 figures, accepted to EPL on October 17, 201

    A nonextensive insight to the stellar initial mass function

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    the present paper, we propose that the stellar initial mass distributions as known as IMF are best fitted by qq-Weibulls that emerge within nonextensive statistical mechanics. As a result, we show that the Salpeter's slope of ∼\sim2.35 is replaced when a qq-Weibull distribution is used. Our results point out that the nonextensive entropic index qq represents a new approach for understanding the process of the star-forming and evolution of massive stars.Comment: 5 pages, 2 figures, Accepted to EP

    Is the effect of birth weight on early breast cancer mediated through childhood growth?

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