Betty Tsang, NSCL/MSU 曾敏兒. collaboration

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1 Science of the SpRIT Time Projection Chamber From Earth to Heavens: Femto-scale nuclei to Astrophysical objects SAMURAI International Collaboration Meeting, Sept 8-9, 2014 Sendai, Japan 曾敏兒 for Betty Tsang, NSCL/MSU collaboration

Science of the SpRIT Time Projection Chamber From Earth to Heavens: Femto-scale nuclei to Astrophysical objects Equation of State of nuclear matter E/A (, ) = E/A (,0) + 2 S( ) = ( n - p )/ ( n + p )

2 Science of the SpRIT Time Projection Chamber From Earth to Heavens: Femto-scale nuclei to Astrophysical objects Equation of State of nuclear matter E/A (, ) = E/A (,0) + 2 S( ) = ( n - p )/ ( n + p ) = (N-Z)/A Symmetry Energy of asymmetric matter To probe fundamental questions on the nature of isospin asymmetric matter. To recreate and study astrophysical environments 曾敏兒 for Betty Tsang, NSCL/MSU collaboration

E/A ( MeV) 120 100 80 60 40 20 Equation of State of nuclear matter EOS is a fundamental

The asymmetric terms has wide implications to nuclear physics and astrophysics.

V central r -20 0 1 2 3 4 / 0 Nuclear Structure Radii, masses, saturation density, nature

3 E/A ( MeV) Equation of State of nuclear matter EOS is a fundamental property of nuclear matter. The asymmetric terms has wide implications to nuclear physics and astrophysics. 0 symmetric matter NL3 Bog1:e/a Bog2:e/a K=300, m*/m=70 Akmal_corr. V central r / 0 Nuclear Structure Radii, masses, saturation density, nature of nuclear force. Nuclear Reactions Fusion, Fission, Fragment productions, nucleon transport, phase transitions. Nuclear Astrophysics Core collapse supernova, Neutron Star, Nucleosynthesis. V tensor

4 ASTRO-H New field Material Science of Quarks Understand Internal structure of Neutron Star Theory Determine EOS of nuclear Matter RIBF X-ray Observation Radius of Neutron Star J-PARC Strangeness Nuclear Physics r Interaction between hyperons Neutron-Rich Nuclear Physics Cold Atomic Gas Nature of Neutron Matter

Future Plans and Challenges US Long Range Plan EOS Working Group August 21-23, 2014, College Station, Texas At << 0 : Measurements to benchmark: Clustering effects in low-density EoS; a clustering at

At 0 : Measurements from both structure and reaction experiments: masses, skins (PREXII and CREX), polarizability, Giant Resonances etc.

5 Future Plans and Challenges US Long Range Plan EOS Working Group August 21-23, 2014, College Station, Texas At << 0 : Measurements to benchmark: Clustering effects in low-density EoS; a clustering at the nuclear surface Observables relevant to the neutrino-sphere. At 0 : Measurements from both structure and reaction experiments: masses, skins (PREXII and CREX), polarizability, Giant Resonances etc. more precise isospin transport, n/p, t/ 3 He sub-barrier fusion cross-sections and fission barriers of exotic nuclei; thermodynamic properties of isospin asymmetric nuclear matter. At : Probe symmetry energy at supra-saturation densities and determine the momentum dependence of the symmetry (isovector) potential. With the SpRIT TPC! From Masses SE>0 Constraint from Isospin diffusion Skyrme interactions

6 Density dependence of symmetry energy at supra-saturation density Wiringa, Fiks, & Fabrocini 1988 Neutron Star observations Heavy Ion Collisions Skyrme interactions Neutron Star obs. HIC Above saturation density, the symmetry energy density dependence may have a different energy dependence than Skyrme interactions.

7 S. Guillot, et al Astrophys. J. 772, 7 (2013), New observations of Neutron Stars (Mass) Lattimar & Prakash too soft Very small Neutron Star radius rules out nearly all EOS

8 S. Guillot, et al Astrophys. J. 772, 7 (2013), New observations of Neutron Stars (radius/radii) Lattimar & Prakash too soft Steiner Suleimanov Very small Neutron Star radius rules out nearly all EOS

9 Status of laboratory measurements at high density Au+Au E/A=0.4-1 GeV Xiao et al p - /p + ratios Inconsistent constraints at HIC results at high densities

10 Successful Strategies used to study the symmetry energy with Heavy Ion collisions Target 112 Sn Tsang et al., PRL 92 (2004) Isospin Diffusion; low, E beam Projectile 124 Sn Vary the N/Z compositions of projectile and targets e.g. 124 Sn+ 124 Sn, 124 Sn+ 112 Sn, 112 Sn+ 124 Sn, 112 Sn+ 112 Sn Measure isospin sensitive observables such as isotope distributions (isospin diffusion), n/p, t/ 3 He ratios Simulate collisions with transport theory Find the symmetry energy density dependence that describes the data. Constrain the relevant input transport variables.

11 Successful Strategies used to study the symmetry energy with Heavy Ion collisions with RIB Isospin degree of freedom Au+Au Xiao et al p - /p + ratios Vary the N/Z compositions of projectile and targets e.g. 132 Sn+ 124 Sn, 132 Sn+ 112 Sn, 108 Sn+ 124 Sn, 108 Sn+ 112 Sn Measure isospin sensitive observables such as multiplex ratios, p - /p +, n/p, t/ 3 He. Simulate collisions with transport theory Find the symmetry energy density dependence that describes the data. Constrain the relevant input transport variables.

12 R( )-R( ) Simulated Pion observables with pbuu Stiffness of symmetry energy soft Stiff R=Y(p - )/Y(p + ) E/A = 300 MeV p Kinetic Energy (MeV) Differences of pion spectra are more sensitive than ratios of integrated yields. SpRIT TPC is ready to probe these observables

13 Heavy Ion Collisions at high density with RIB Old data: Au+Au, E/A=150 to 1500 MeV Proposed New Experiments at RIB facilities Simulate collisions with transport theory o Constrain the relevant input transport variables such as the momentum dependence, NN collisions & cluster effects. o Importance of having two beam energies; E/A=300 & 200 MeV. o Symmetric and asymmetric reactions.

14 Heavy Ion Collisions at high density with RIB Old data: Au+Au, E/A=150 to 1500 MeV Proposed New Experiments at RIB facilities 13.5 days approved by June and Dec, 2013 RIKEN PAC

15 Day 1 experimental setup To be Tested at HIMAC in Nov. Tested at GSI in July

16 Schedule Fall, 2013 February, 2014 Summer 2014 Spring 2015 Construction of TPC completed Shipment of TPC to RIKEN Installation of TPC into SAMURAI magnet Commission of TPC and first experiments (13.5 days of Sn+Sn approved) Importance of Spring 2015: 1. US DOE 5 year award expires on September 30, Loss of experienced manpower: postdoc and students will move on with their careers. 3. The 112Sn and 124Sn targets ($80k) are available for loan in Spring of 2015 but not Fall (Sobotka s group is running experiment with complete different target geometry cylinder vs. foil). 4. Schedule needs to be firmed up soon for manpower allocation e.g. teaching relief for Bill Lynch.

17 Best Scenario November, 2014 December, 2014 March, 2015 April 2015 Beam test of scintillators at HiMAC Installation of GET electronics Commissioning of TPC with Beam at RIKEN First TPC Experiment (132Sn or 108Sn Beam) Importance of Spring 2015: 1. US DOE 5 year award expires on September 30, Loss of experienced manpower: postdoc and students will move on with their careers. 3. The 112Sn and 124Sn targets ($80k) are available for loan in Spring of 2015 but not Fall (Sobotka s group is running experiment with complete different target geometry cylinder vs. foil). 4. Schedule needs to be firmed up soon for manpower allocation e.g. teaching relief for Bill Lynch

18 MSU,TAMU RIBF, Lanzhou, FRIB, RAON GSI FAIR Symmetry Energy Project International collaboration to determine the symmetry energy over a range of density

20 Participating institutions in TPC construction

21 Thank you very much July 23, 2014: TPC inserted into SAMURAI dipole 曾敏兒 for Betty Tsang, NSCL/MSU collaboration

22 Science of the SpRIT Time Projection Chamber From Earth to Heavens: Exploring Physics of Femto-scale nuclei to Astrophysical objects July 23, 2014: TPC inserted into SAMURAI dipole collaboration

24 Density dependence of symmetry energy E/A (, ) = E/A (,0) + 2 S( ) = ( n - p )/ ( n + p ) = (N-Z)/A S( ) = E/A (,1)-E/A (,0)

25 Constraints from nuclear structure and reactions with credible uncertainties NuSYM13 & ICNT2013 S L - o B 0 ( S 0 A Way Forward from ICNT2013 & NuSYM13 J. of Phys G 41(2014)

26 OUTLINE 1. Introduction 2. Current Status of constraints from HIC and nuclear structure 3. From Heavens to Earth: Astrophysics observations to nuclear physics experiments new observations of neutron star radius & masses Experimental plans with HIC at ~2 0 and beyond 4. Summary EOS physics with SpRIT TPC

27 Y(p - )/Y(p + ) Ratios and Difference of pions emitted in collisions of Sn isotopes E/A =120 MeV AT-TPC 124 Sn+ 124 Sn E lab =120 MeV/A b = 1fm Bickley et al., private comm. (2009) Y(p - )/Y(p + ) Y(p - )/Y(p + ) E/A = 300 MeV soft stiff TPC Pion ratio depends strongly on the symmetry energy. Differences of spectra are more sensitive than ratios of integrated yields. SpRIT TPC is ready to probe these observables

28 Constraints from nuclear structure and reactions with credible uncertainties NuSYM13 & ICNT2013 Isospin diffusion in HIC neutrinosphere

Collaboration (NSF MRI) Solenoidal (MRI) magnet Recently completed (2013)

29 Time Projection Chambers : SAMURAI TPC and AT-TPC Active Target -TPC TPC U.S. Collaboration (NSF MRI) Solenoidal (MRI) magnet Recently completed (2013) Measure p +, p -, t, 3 He, n, MSU U.S./Japan collaboration SAMURAI dipole Recently completed (2013) Measure p +, p -, t, 3 He, n, RIKEN R. Shane s talk Aug. 18

30 Existing Radioactive Beam Facilities worldwide Texas A&M NSCL /FRIB GANIL GSI/ FAIR Lanzhou RAON RIBF Existing SEP collaboration Symmetry Energy Project International collaboration to determine the symmetry energy over a range of density using different facilities 3

31 collaboration To study symmetry energy ~2 0 with RIB Constructed at MSU & TAMU Shipped to RIKEN in February, 2014 Experimental program starts in Spring, 2015

32 Day 1 experimental setup

33 SUMMARY from LRP EOS Working Group For sub-saturation density: Improve existing constraints with RIB and more precise measurements. For supra-saturation density: New experiments using new detectors are planned in various laboratories; Theorists are engaged to provide better understanding of the transport models to interpret the new (& old data) regarding theoretical error bars and consistency of the results; Global efforts from different facilities & close interactions between theorists and experimentalists.

Momentum dependence of symmetry energy

Momentum dependence of symmetry energy Joint DNP of APS & JPS October 7-11, 2014 Kona, HI, USA 曾敏兒 Betty Tsang, NSCL/MSU Equation of State of Asymmetric Nuclear Matter E/A (, ) = E/A (,0) + 2 S( ) = (