Search arXiv⌕ Search
Home/Archive/arXiv

arXiv · 2301.13253

Dense Nuclear Matter Equation of State from Heavy-Ion Collisions

Agnieszka Sorensen·Kshitij Agarwal·Kyle W. Brown·Zbigniew Chajęcki·Paweł Danielewicz·Christian Drischler·Stefano Gandolfi·Jeremy W. Holt·Matthias Kaminski·Che-Ming Ko·Rohit Kumar·Bao-An Li·William G. Lynch·Alan B. McIntosh·William G. Newton·Scott Pratt·Oleh Savchuk·Maria Stefaniak·Ingo Tews·ManYee Betty Tsang·Ramona Vogt·Hermann Wolter·Hanna Zbroszczyk·Navid Abbasi·Jörg Aichelin·Anton Andronic·Steffen A. Bass·Francesco Becattini·David Blaschke·Marcus Bleicher·Christoph Blume·Elena Bratkovskaya·B. Alex Brown·David A. Brown·Alberto Camaiani·Giovanni Casini·Katerina Chatziioannou·Abdelouahad Chbihi·Maria Colonna·Mircea Dan Cozma·Veronica Dexheimer·Xin Dong·Travis Dore·Lipei Du·José A. Dueñas·Hannah Elfner·Wojciech Florkowski·Yuki Fujimoto·Richard J. Furnstahl·Alexandra Gade·Tetyana Galatyuk·Charles Gale·Frank Geurts·Fabiana Gramegna·Sašo Grozdanov·Kris Hagel·Steven P. Harris·Wick Haxton·Ulrich Heinz·Michal P. Heller·Or Hen·Heiko Hergert·Norbert Herrmann·Huan Zhong Huang·Xu-Guang Huang·Natsumi Ikeno·Gabriele Inghirami·Jakub Jankowski·Jiangyong Jia·José C. Jiménez·Joseph Kapusta·Behruz Kardan·Iurii Karpenko·Declan Keane·Dmitri Kharzeev·Andrej Kugler·Arnaud Le Fèvre·Dean Lee·Hong Liu·Michael A. Lisa·William J. Llope·Ivano Lombardo·Manuel Lorenz·Tommaso Marchi·Larry McLerran·Ulrich Mosel·Anton Motornenko·Berndt Müller·Paolo Napolitani·Joseph B. Natowitz·Witold Nazarewicz·Jorge Noronha·Jacquelyn Noronha-Hostler·Grażyna Odyniec·Panagiota Papakonstantinou·Zuzana Paulínyová·Jorge Piekarewicz·Robert D. Pisarski·Christopher Plumberg·Madappa Prakash
View original source ↗Read source document ↗Export metadata ↓

Abstract

The nuclear equation of state (EOS) is at the center of numerous theoretical and experimental efforts in nuclear physics. With advances in microscopic theories for nuclear interactions, the availability of experiments probing nuclear matter under conditions not reached before, endeavors to develop sophisticated and reliable transport simulations to interpret these experiments, and the advent of multi-messenger astronomy, the next decade will bring new opportunities for determining the nuclear matter EOS, elucidating its dependence on density, temperature, and isospin asymmetry. Among controlled terrestrial experiments, collisions of heavy nuclei at intermediate beam energies (from a few tens of MeV/nucleon to about 25 GeV/nucleon in the fixed-target frame) probe the widest ranges of baryon density and temperature, enabling studies of nuclear matter from a few tenths to about 5 times the nuclear saturation density and for temperatures from a few to well above a hundred MeV, respectively. Collisions of neutron-rich isotopes further bring the opportunity to probe effects due to the isospin asymmetry. However, capitalizing on the enormous scientific effort aimed at uncovering the dense nuclear matter EOS, both at RHIC and at FRIB as well as at other international facilities, depends on the continued development of state-of-the-art hadronic transport simulations. This white paper highlights the essential role that heavy-ion collision experiments and hadronic transport simulations play in understanding strong interactions in dense nuclear matter, with an emphasis on how these efforts can be used together with microscopic approaches and neutron star studies to uncover the nuclear EOS.

Explore related subjects

nucl-thnucl-ex

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Agnieszka Sorensen, Kshitij Agarwal, Kyle W. Brown, Zbigniew Chajęcki, Paweł Danielewicz, Christian Drischler, Stefano Gandolfi, Jeremy W. Holt, Matthias Kaminski, Che-Ming Ko, Rohit Kumar, Bao-An Li, William G. Lynch, Alan B. McIntosh, William G. Newton, Scott Pratt, Oleh Savchuk, Maria Stefaniak, Ingo Tews, ManYee Betty Tsang, Ramona Vogt, Hermann Wolter, Hanna Zbroszczyk, Navid Abbasi, Jörg Aichelin, Anton Andronic, Steffen A. Bass, Francesco Becattini, David Blaschke, Marcus Bleicher, Christoph Blume, Elena Bratkovskaya, B. Alex Brown, David A. Brown, Alberto Camaiani, Giovanni Casini, Katerina Chatziioannou, Abdelouahad Chbihi, Maria Colonna, Mircea Dan Cozma, Veronica Dexheimer, Xin Dong, Travis Dore, Lipei Du, José A. Dueñas, Hannah Elfner, Wojciech Florkowski, Yuki Fujimoto, Richard J. Furnstahl, Alexandra Gade, Tetyana Galatyuk, Charles Gale, Frank Geurts, Fabiana Gramegna, Sašo Grozdanov, Kris Hagel, Steven P. Harris, Wick Haxton, Ulrich Heinz, Michal P. Heller, Or Hen, Heiko Hergert, Norbert Herrmann, Huan Zhong Huang, Xu-Guang Huang, Natsumi Ikeno, Gabriele Inghirami, Jakub Jankowski, Jiangyong Jia, José C. Jiménez, Joseph Kapusta, Behruz Kardan, Iurii Karpenko, Declan Keane, Dmitri Kharzeev, Andrej Kugler, Arnaud Le Fèvre, Dean Lee, Hong Liu, Michael A. Lisa, William J. Llope, Ivano Lombardo, Manuel Lorenz, Tommaso Marchi, Larry McLerran, Ulrich Mosel, Anton Motornenko, Berndt Müller, Paolo Napolitani, Joseph B. Natowitz, Witold Nazarewicz, Jorge Noronha, Jacquelyn Noronha-Hostler, Grażyna Odyniec, Panagiota Papakonstantinou, Zuzana Paulínyová, Jorge Piekarewicz, Robert D. Pisarski, Christopher Plumberg, Madappa Prakash. 2024-01-25. Dense Nuclear Matter Equation of State from Heavy-Ion Collisions. https://doi.org/10.1016/j.ppnp.2023.104080

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

Three-dimensional orbital-free density functional theory description of nuclear pasta in the inner crust of neutron stars

Background: In the bottom layer of the inner crust of neutron stars, various crystalline structures are expected to emerge that are collectively called ``nuclear pasta.'' It is desirable to know properties of nuclear pasta in a wide variety of conditions for astrophysical applications. However, three-dimensional fully-microscopic calculations require huge computational effort that makes it still challenging to carry out systematic calculations. Purpose: In this paper, we propose an efficient method to calculate various nuclear pasta configurations in a non-empirical manner, based on three-dimensional orbital-free density functional theory (OF-DFT). We demonstrate the feasibility of the proposed approach by applying it to densities across the inner crust of neutron stars. Methods: As a first application of OF-DFT for nuclear pasta, we employ the second-order extended Thomas-Fermi (ETF) expansion of Skyrme energy density functional (EDF) to construct an EDF that depends only on neutron and proton number densities. Based on the variational principle, we derive Euler-Lagrange equations to determine optimal neutron and proton density distributions and solve them self-consistently. In this work, we call this approach the self-consistent ETF (SC-ETF) method. Results: We perform three-dimensional SC-ETF calculations with various box sizes. We successfully obtain various pasta structures, depending on given average nucleon number densities, consistent with earlier studies. Moreover, we find other exotic structures, such as bending and/or connected rods, slabs with a hole, etc., underlining the advantage of the self-consistent formalism. Conclusions: We demonstrate that the SC-ETF method proposed in this study, which can be regarded as a realization of OF-DFT, is a promising tool that can efficiently describe complex pasta structures without empirical assumptions on geometric shapes.

nucl-th↗
arXiv2026

Microscopic analysis of M1 scissors mode in $^{254}$No

The low-energy $M1$ orbital scissors mode (SM) was recently observed by Oslo group in deformed nucleus $^{254}$No. This is the heaviest nucleus where SM was ever experimentally found. We propose the analysis of SM, together with the spin-flip $M1$ resonance, within fully self-consistent Quasiparticle Random-Phase Approximation (QRPA) with Skyrme forces SG2, SLy4 and SLy5. The impact of "tensor" $J^2$-term, introduced by perturbative (on the base of SG2) and consistent (SLy5) ways, is analyzed and shown to be noticeable but not decisive. The deformation-induced coupling of $M1$ and $E2$ states is inspected. The calculations reasonably describe Oslo's experimental data. The best agreement is obtained for SLy5. A fine structure of SM in $^{254}$No is predicted. A significant constructive interference of the dominant orbital and minor spin-flip contributions to $M1$ strength at SM energy region is found. What is remarkable, our analysis of distributions of the convective nuclear currents challenges the scissors-like flow usually assumed for SM.

nucl-th↗
arXiv2026

Systematic Study of Proton, Two-Proton, Alpha, and Cluster Radioactivity Half-Lives based on the Deformed Gamow-like Model and Tabular Prior-data Fitted Network ($\mathrm{TabPFN}$)

A hybrid framework combining the deformed Gamow-like model ($\mathrm{DGLM}$) with the Tabular Prior-data Fitted Network ($\mathrm{TabPFN}$) is developed to improve half-life predictions for two-proton emission, proton emission, $α$ decay, and cluster radioactivity. A total of 583 radioactive nuclei are investigated, including 17 two-proton emitters, 42 proton emitters, 498 $α$ emitters, and 26 cluster emitters. Among the four considered models, $\mathrm{DGLM}^{b}+\mathrm{TabPFN}$ achieves the best overall performance, with $σ_{\mathrm{RMS}}=0.423$, corresponding to an improvement of approximately $82.2\%$ over $\mathrm{DGLM}^{b}$. The model parameters are optimized for each decay mode using the least-squares method. After introducing $\mathrm{TabPFN}$, the prediction errors for proton emission and $α$ decay are reduced by approximately $80.6\%$ and $87.6\%$, respectively. For $α$ decay, the training, test, and overall RMSEs are 0.208, 0.305, and 0.240, indicating good generalization capability without evident overfitting. The model also reproduces the systematic evolution of $α$-decay half-lives and the shell-closure effect around $N=126$. These results demonstrate that combining $\mathrm{DGLM}$ with $\mathrm{TabPFN}$ significantly improves the accuracy and robustness of radioactive-decay half-life predictions while retaining the physical interpretability of the original model.

nucl-th↗