on our way to ASYEOS II W Trautmann
- Slides: 48
on our way to ASY-EOS II W. Trautmann, GSI Darmstadt ASY-EOS II Collaboration Meeting Catania & Caltagirone, 14 -15 December 2017
on our way to ASY-EOS II thanks where we are now interpreting ASY-EOS I what to expect therefore: best possible experiment KRAB+Neu. LAND to Neu. LAND through support of R 3 B ASY-EOS II Collaboration Meeting Catania & Caltagirone, 14 -15 December 2017 2
Laboratori Nazionali del Sud 4 double rings (352 modules) of CHIMERA multi-detector, LNS Catania, Sicilia 3, 8 m 3
CHIMERA LNS/Catania 352 modules 4
5
on our way to ASY-EOS II thanks where we are now interpreting ASY-EOS I what to expect therefore: best possible experiment KRAB+Neu. LAND to Neu. LAND through support of R 3 B 6
from acceptance-integrated flow ratios γ = 0. 7± 0. 2 L=72± 13 Me. V FOPI-LAND: Russotto et al. PLB 697 (2011) ASY-EOS: Russotto et al. PRC 94 (2016) 7
present status FOPI model predictions from Fuchs and Wolter, EPJA 30 (2006) ASY-EOS ∙∙∙∙∙ APR ---- graphics by Y. Leifels 8
sensitivity to density Dan Cozma using Tübingen QMD Difference of Elliptic-Flow Ratio ρswitch graphics by Y. Leifels P. Russotto et al. , PRC 94, 034608 (2016) 9
ASY-EOS: symmetry pressure p 0 = 3. 8 ± 0. 7 Me. V/fm 3 neutron star pressure p 0 = 3. 4 ± 0. 7 Me. V/fm 3 ρ0 Steiner, Lattimer, and Brown, Ap. J 765, L 5 (2013) 10
symmetry pressure vs neutron star radius 11
on our way to ASY-EOS II thanks where we are now interpreting ASY-EOS I what to expect therefore: best possible experiment KRAB+Neu. LAND to Neu. LAND through support of R 3 B 12
from acceptance-integrated flow ratios γ = 0. 7± 0. 2 L=72± 13 Me. V FOPI-LAND: Russotto et al. PLB 697 (2011) ASY-EOS: Russotto et al. PRC 94 (2016) 13
with Esym(ρ0) = 31 Me. V L L=63± 11 Me. V Esym(ρ0) (Me. V) Lattimer & Steiner, EPJA 50 (2014) FOPI-LAND: Russotto et al. PLB 697 (2011) P. Russotto et al. , PRC 94, 034608 (2016) 14
Dan Cozma: with accepted parameter range 15
on our way to ASY-EOS II thanks where we are now interpreting ASY-EOS I what to expect therefore: best possible experiment KRAB+Neu. LAND to Neu. LAND through support of R 3 B 16
SπRIT Experiment § SπRIT TPC and ancillary detectors are installed inside the SAMURAI magnet so as to obtain as much as uniform magnetic field inside the field cage. § Neu. LAND is placed at 8. 8 m from the target at the angle of 30 degrees. , Slide 17 17
Concettina Sfienti
opportunities for astrophysical observations NICER on the ISS Neutron-star Interior Composition Explorer 56 X-ray concentrators (0. 2 -12 ke. V, 100 ns) measures time resolved X-ray emissions of neutron stars launched on June 3, 2017, at 17: 07 EDT NICER science program started in July 2017 source: NASA 20
lower bound R = 12 km from GW 170817 Fattoyev, Piekarewicz, and Horowitz, ar. Xiv: 1711. 06615 21
on our way to ASY-EOS II thanks where we are now interpreting ASY-EOS I what to expect therefore: best possible experiment KRAB+Neu. LAND to Neu. LAND through support of R 3 B 22
event multiplicity ASY-EOS FOPI-LAND P. Russotto et al. (2016), Fig. 7 23
24
reaction plane orientation P. Russotto et al. (2016), Fig. 10 25
event multiplicity FOPI-LAND χ=1. 58 A. Andronic et al. , EPJA 30, 31 (2006) 26
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on our way to ASY-EOS II thanks where we are now interpreting ASY-EOS I what to expect therefore: best possible experiment KRAB+Neu. LAND to Neu. LAND through support of R 3 B 29
Micro. Ball (Washington University, St. Louis) µBall: 4 rings, 50 Cs. I(Tl) ~ 1 cm thick 60°< <147° Discriminate against interactions with air; multiplicity measurements 31
Neu. LAND all plastic improved calorimetry 4 planes in RIKEN 5 planes at GSI more planes to come, probably up to 15 32
Particle ID by Neu. LAND d t p 3 4 He He p d t 3 He, 4 He γ charged particles n γ Mizuki KURATA-NISHIMURA RIKEN, Japan For Sp. RIT-TPC collaboration Neutrons 33
on our way to ASY-EOS II thanks where we are now interpreting ASY-EOS I what to expect therefore: best possible experiment KRAB+Neu. LAND to Neu. LAND through support of R 3 B 34
35
ASY-EOS, truly international spokespersons: P. Russotto (Catania) R. C. Lemmon (Daresbury) P. Russotto, PRC 94, 034608 (2016) 93 authors from 14 countries
Byungsik Hong
FP Brown, PRL 85 (2000) Brown, PRL 111 (2013) 13 Skyrme sets fitted to ground-state properties of doubly magic nuclei Esym determined at 0. 1 fm-3 neutron skin determines slope at 0. 1 fm-3 38
ASY-EOS II proposal
ASY-EOS II proposal: Ur. QMD predictions Measure excitation function to improve resolving power At midvelocity b/bred <0. 53 Stiff γ=1. 5, Soft γ=0. 5 40
the world average: L = 58. 8865 Me. V Li and Han, PLB 727 (2013) (L=3 p 0/ρ0) ASY-EOS from n-skins neutron skins masses collective excitations isospin diffusion observation of neutron stars crust oscillations r-mode instabilities mass-radius analysis 41
from Zhang and Chen, Phys. Rev. C 92, 031301(R) (2015)
from Taranto, Baldo, Burgio, PRC 87, 045803 (2013) only BHF+UVIX TBF meets all the constraints from HIC and NS observations 43
opportunities for astrophysical observations NICER on the ISS Neutron-star Interior Composition Explorer 56 X-ray concentrators (0. 2 -12 ke. V, 100 ns) measures time resolved X-ray emissions of neutron stars launched on June 3, 2017, at 17: 07 EDT NICER science program started in July 2017 source: NASA 45
gravitational light bending ± 5% (3σ)
expected accuracy, goal is ± 5% in mass and radius goal: ± 5% in radius and mass Özel et al. , ar. Xiv: 1512. 03067 [astro-ph. HE] 47
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