Nuclear moment of inertia at high rotational frequencies

Johnson, A.; Ryde, H.; Hjorth, S.A.

doi:10.1016/0375-9474(72)90617-3

Cited by 219 publications

(60 citation statements)

References 17 publications

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“…Such an anomalous decrease of the moment of inertia as described is analogous to the phenomenon of "backbending" in the rotational bands of nuclei predicted by Mottelson and Valatin and observed years ago [12][13][14]. The moment of inertia of a nucleus changes anomalously because of a change in phase from a nucleon spin-aligned phase at high angular momentum to a pair-correlated superfluid phase at low.…”

mentioning

confidence: 82%

Signal of Quark Deconfinement in the Timing Structure of Pulsar Spin-Down

1997

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confidence: 82%

Signal of Quark Deconfinement in the Timing Structure of Pulsar Spin-Down

1997

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“…Such an anomalous decrease of I is analogous to the 'backbending' phenomenon known from nuclear physics, in which case the moment of inertia of an atomic nucleus changes anomalously because of a change in phase from a nucleon spin-aligned state at high angular momentum to a paircorrelated superfluid phase at low angular momentum. In the nuclear physics case, the backbending in the rotational bands of nuclei that was predicted by Mottelson and Valatin [316] and then observed years later by Stephens and Simon [317], and Johnson, Ride and Hjorth [318]. For neutron stars, the stellar backbending of I is shown in Fig.…”

Section: Isolated Pulsarsmentioning

confidence: 95%

Strange quark matter and compact stars

Weber

2005

Progress in Particle and Nuclear Physics

692

280

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Astrophysicists distinguish between three different types of compact stars. These are white dwarfs, neutron stars, and black holes. The former contain matter in one of the densest forms found in the Universe which, together with the unprecedented progress in observational astronomy, make such stars superb astrophysical laboratories for a broad range of most striking physical phenomena. These range from nuclear processes on the stellar surface to processes in electron degenerate matter at subnuclear densities to boson condensates and the existence of new states of baryonic matter-like color superconducting quark matter-at supernuclear densities. More than that, according to the strange matter hypothesis strange quark matter could be more stable than nuclear matter, in which case neutron stars should be largely composed of pure quark matter possibly enveloped in thin nuclear crusts. Another remarkable implication of the hypothesis is the possible existence of a new class of white dwarfs. This article aims at giving an overview of all these striking physical possibilities, with an emphasis on the astrophysical phenomenology of strange quark matter. Possible observational signatures associated with the theoretically proposed states of matter inside compact stars are discussed as well. They will provide most valuable information about the phase diagram of superdense nuclear matter at high baryon number density but low temperature, which is not accessible to relativistic heavy ion collision experiments.

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“…In such a representation all the important physical quantities as energy, angular momentum, aligned angular momentum and moment of inertia, etc. were discovered experimentally for the first time by Johnson et al, [10] and are often called a backbending effect.…”

Section: Introductionmentioning

confidence: 99%

“…Johnson et al, [10] chose to represent the excitation energies E(I) of the ground-state levels in terms of a plot between the nuclear moment of inertia φ and the squared rotational frequencies ω 2 . Such plots have revealed that in some cases, φ increases so rapidly with I that ω 2 actually decreases as higher spin states are reached, resulting in the appearance of backbending in these plots.…”

Section: Introductionmentioning

confidence: 99%

Comparative Phenomenological Description of Even-Even Isotopes at Mass Region A ≈ 70

El‐Kameesy¹,

Shahbunder²,

Abdelmageed³

et al. 2016

JAMP

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In the present work the nuclear structure properties and the backbending phenomena of eveneven isotopes at A ≈ 70 mass region are analyzed using two simultaneous theoretical models based on a simple modified version of the collective model predictions besides an improved version of exponential model with the inclusion of pairing correlation. In general, both models successfully describe the backbending phenomena in that region. From the comparison between the predictions of the two proposed models a firm conclusion is obtained concerning the superiority of the simple improved version of the exponential model in describing the forward and downbending region of the φ-ω 2 plots.

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Nuclear moment of inertia at high rotational frequencies

Cited by 219 publications

References 17 publications

Signal of Quark Deconfinement in the Timing Structure of Pulsar Spin-Down

Signal of Quark Deconfinement in the Timing Structure of Pulsar Spin-Down

Strange quark matter and compact stars

Comparative Phenomenological Description of Even-Even Isotopes at Mass Region A ≈ 70

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