Isotopic Dependence of the Nuclear Caloric Curve

Sfienti, C.; Adrich, P.; Aumann, T.; Bacri, C.O.; Barczyk, T.; Bassini, R.; Bianchin, S.; Boiano, C.; Botvina, A. S.; Boudard, A.; Brzychczyk, J.; Chbihi, A.; Cibor, J.; Czech, B.; Napoli, M. De; Ducret, J. E.; Emling, H.; Frankland, J.D.; Hellström, M.; Henzlová, D.; Immé, G.; Iori, I.; Johansson, H.; Kezzar, K.; Lafriakh, A.; Févre, A. Le; Gentil, É. Le; Leifels, Y.; Lühning, J.; Łukasik, J.; Lynch, W. G.; Lynen, U.; Majka, Z.; Mocko, M.; Müller, W. F. J.; Mykulyak, A.; Orth, H.; Otte, A. N.; Palit, R.; Pawłowski, P.; Pullia, A.; Raciti, G.; Rapisarda, E.; Sann, H.; Schwarz, C.; Simon, H.; Sümmerer, K.; Trautmann, W.; Tsang, M.B.; Verde, G.; Volant, C.; Wallace, Mark; Weick, H.; Wiechuła, J.; Wieloch, A.; Zwiȩgliński, B.

doi:10.1103/physrevlett.102.152701

Cited by 69 publications

(37 citation statements)

References 32 publications

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“…On the theoretical side the calculated temperature variation with isospin is small [229][230][231] lower temperatures for neutron-richer nuclei were observed. Note that, unlike the ensemble of caloric curves presented in [234], none of those derived in [184,232,233] exhibits a plateau. In [233] the temperature linearly increases with energy between 2 and 8 MeV per nucleon, reaching 12 MeV at an excitation energy of 8 MeV per nucleon.…”

Section: Constrained Caloric Curvesmentioning

confidence: 98%

Liquid–Gas phase transition in nuclei

Borderie

Frankland

2019

Progress in Particle and Nuclear Physics

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Section: Constrained Caloric Curvesmentioning

confidence: 98%

Liquid–Gas phase transition in nuclei

Borderie

Frankland

2019

Progress in Particle and Nuclear Physics

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“…Equation (6) displays a convenient separation between the symmetric and aymmetric parts of the EoS, which facilitates the identification of observables that may be sensitive, for instance, mainly to the symmetry energy. At this time, groups from GSI (Sfienti et al, 2009;Trautmann et al, 2009), MSU (Tsang et al, 2009), Italy (Greco, 2010), France (Borderie & Rivet, 2008), China (Feng, 2010;Yong, 2010), Japan (Isobe, 2011), Texas A&M (Kohley et al, 2011), and more are investigating the density dependence of the symmetry energy through heavy-ion collisions. Typically, constraints are extracted from heavy-ion collision simulations based on transport models.…”

Section: A Microscopic Equation Of State For Neutron-rich Matter and mentioning

confidence: 99%

Neutron star properties and the nuclear equation of state

Sammarruca¹

2012

Astrophysics

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“…For example, a 132 Sn + 132 Sn reaction will exhibit a much larger sensitivity to the symmetry energy in comparison to a 124 Sn + 124 Sn reaction due to the increased δ of the 132 Sn system. The work of the ALADIN Collaboration represents the only experimental example in which RIB-induced reactions ( 124 La and 107 Sn) were used to examine the symmetry energy [36][37][38]. The experimental results were shown to be sensitive to the strength of the symmetry energy through comparisons with the statistical multifragmentation model [37,38] and the isospin quantum molecular dynamics model [39].…”

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confidence: 99%

Exploiting neutron-rich radioactive ion beams to constrain the symmetry energy

et al. 2013

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The Modular Neutron Array (MoNA) and 4 Tm Sweeper magnet were used to measure the free neutrons and heavy charged particles from the radioactive ion beam induced 32 Mg + 9 Be reaction. The fragmentation reaction was simulated with the constrained molecular dynamics model (CoMD), which demonstrated that the N/Z of the heavy fragments and free neutron multiplicities were observables sensitive to the density dependence of the symmetry energy at subsaturation densities. Through comparison of these simulations with the experimental data, constraints on the density dependence of the symmetry energy were extracted. The advantage of radioactive ion beams as a probe of the symmetry energy is demonstrated through examination of CoMD calculations for stable and radioactive-beam-induced reactions. PACS number(s): 21.65. Mn, 25.70.Mn, 21.65.Ef Introduction. The desire to extend our understanding of nuclear matter at densities, temperatures, pressures, and neutron-to-proton ratios (N/Z) away from that of ground-state nuclei has become a driving force in the nuclear science community. In particular, the emergence of radioactive ion beam (RIB) facilities has placed an emphasis on exploring nuclear matter along the isospin degree of freedom. The symmetry energy is the critical component which defines how the properties of nuclear matter, or the nuclear equation of state (EoS), change as a function of isospin. The nuclear EoS can be approximated aswhere the energy per nucleon of infinite nuclear matter, E(ρ, δ), is a function of the density (ρ) and isospin concentration (δ) [1][2][3]. The isospin concentration is the difference in the neutron and proton densities, δ = (ρ n − ρ p )/(ρ n + ρ p ) ≈ (N − Z)/A. The first term of the EoS is isopin independent and thus represents the binding energy of symmetric (N = Z) nuclear matter. The second term of the EoS has a strong dependence on the asymmetry of the nuclear matter and has been historically termed the symmetry energy (however, a more appropriate term is the asymmetry energy). The EoS for symmetric nuclear matter is relatively well constrained around the saturation density (ρ 0 = 0.16 fm −3 ) from isoscalar giant monopole and dipole resonances [4,5] and at higher densities (up to ρ/ρ 0 ∼4.5) from heavy-ion collisions [6,7]. Constraining the form of the density dependence of the symmetry energy [E sym (ρ)] is essential for developing a complete description of asymmetric nuclear matter. For example, the properties of neutron stars are strongly correlated to the * kohley@nscl.msu.edu † Present address: TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada.

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Isotopic Dependence of the Nuclear Caloric Curve

Cited by 69 publications

References 32 publications

Liquid–Gas phase transition in nuclei

Liquid–Gas phase transition in nuclei

Neutron star properties and the nuclear equation of state

Exploiting neutron-rich radioactive ion beams to constrain the symmetry energy

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