Neutron Skins with α-clusters
|
|
- Prosper Jasper O’Connor’
- 6 years ago
- Views:
Transcription
1 Neutron Skins with α-clusters GSI Helmholtzzentrum für Schwerionenforschung, Darmstadt Nuclear Astrophysics Virtual Institute Hirschegg 2015 Nuclear Structure and Reactions: Weak, Strange and Exotic International Workshop XLIII on Gross Properties of Nuclei and Nuclear Reactions Hirschegg, Kleinwalsertal, Austria January 11 17, 2015
2 Outline Introduction Neutron Skins and Neutron Matter Equation of State, Density Dependence of Symmetry Energy, Correlations in Low-Density Nuclear Matter Generalized Relativistic Density Functional Details of grdf Model, Effective Interaction α-clusters on the Surface of Nuclei Application of grdf Model, Nuclei with α-clusters Experimental Test Quasi-Free (p,pα) Knockout Reactions, Kinematics, Cross Sections Conclusions Details: S. Typel, Phys. Rev. C 89 (2014) S. Typel, H.H. Wolter, G. Röpke, D. Blaschke, Eur. Phys. J. A 50 (2014) 17 M.D. Voskresenskaya, S. Typel, Nucl. Phys. A 887 (2012) 42 S. Typel, G. Röpke, T. Klähn, D. Blaschke, H.H. Wolter, Phys. Rev. C 81 (2010) Neutron Skins with α-clusters - 1
3 Introduction
4 Neutron Skins and Neutron Matter Equation of State neutron-rich nuclei development of neutron skin with thickness: r np = S = rn 2 rp 2 Neutron Skins with α-clusters - 2
5 Neutron Skins and Neutron Matter Equation of State neutron-rich nuclei development of neutron skin with thickness: r np = S = rn 2 rp 2 charge radii of nuclei well-known from electron scattering experiments, isotope shifts, etc. (see, e.g., I. Angeli et al., ADNDT 99 (2013) 69) Neutron Skins with α-clusters - 2
6 Neutron Skins and Neutron Matter Equation of State neutron-rich nuclei development of neutron skin with thickness: r np = S = rn 2 rp 2 charge radii of nuclei well-known from electron scattering experiments, isotope shifts, etc. (see, e.g., I. Angeli et al., ADNDT 99 (2013) 69) neutron matter radii less precisely known, suggested experimental approach: parity violation in electron scattering PREX@Jefferson Lab with 208 Pb target (C. J. Horowitz et al., Phys. Rev. C 63 (2001) ) Neutron Skins with α-clusters - 2
7 Neutron Skins and Neutron Matter Equation of State neutron-rich nuclei development of neutron skin with thickness: r np = S = rn 2 rp 2 charge radii of nuclei well-known from electron scattering experiments, isotope shifts, etc. (see, e.g., I. Angeli et al., ADNDT 99 (2013) 69) neutron matter radii less precisely known, suggested experimental approach: parity violation in electron scattering PREX@Jefferson Lab with 208 Pb target (C. J. Horowitz et al., Phys. Rev. C 63 (2001) ) observation of B.A. Brown: strong correlation of neutron skin thickness with derivative of neutron matter equation of state (EoS) d(e/a) dn = p 0 n=n0 n 2 0 at density n 0 = 0.1 fm 3 for 18 Skyrme Hartree-Fock parameter sets (Phys. Rev. Lett. 85 (2000) 5296) Neutron Skins with α-clusters - 2
8 Neutron Skins and Neutron Matter Equation of State neutron-rich nuclei development of neutron skin with thickness: r np = S = rn 2 rp 2 charge radii of nuclei well-known from electron scattering experiments, isotope shifts, etc. (see, e.g., I. Angeli et al., ADNDT 99 (2013) 69) neutron matter radii less precisely known, suggested experimental approach: parity violation in electron scattering PREX@Jefferson Lab with 208 Pb target (C. J. Horowitz et al., Phys. Rev. C 63 (2001) ) observation of B.A. Brown: strong correlation of neutron skin thickness with derivative of neutron matter equation of state (EoS) d(e/a) dn = p 0 n=n0 n 2 0 at density n 0 = 0.1 fm 3 for 18 Skyrme Hartree-Fock parameter sets (Phys. Rev. Lett. 85 (2000) 5296) extension to relativistic mean-field models (S. Typel and B. A. Brown, Phys. Rev. C 64 (2001) ) Neutron Skins with α-clusters - 2
9 Neutron Skins and Symmetry Energy equivalent correlation of neutron skin thickness with slope of nuclear symmetry energy found in investigation guided by principles of effective field theory (R. J. Furnstahl, Nucl. Phys. 706 (2002) 85) Neutron Skins with α-clusters - 3
10 Neutron Skins and Symmetry Energy equivalent correlation of neutron skin thickness with slope of nuclear symmetry energy found in investigation guided by principles of effective field theory (R. J. Furnstahl, Nucl. Phys. 706 (2002) 85) expansion of energy per nucleon in nuclear matter E A (n,β) = E 0(n)+E s (n)β n = n n +n p β = (n n n p )/n with symmetry energy E s (n) Neutron Skins with α-clusters - 3
11 Neutron Skins and Symmetry Energy equivalent correlation of neutron skin thickness with slope of nuclear symmetry energy found in investigation guided by principles of effective field theory (R. J. Furnstahl, Nucl. Phys. 706 (2002) 85) expansion of energy per nucleon in nuclear matter E A (n,β) = E 0(n)+E s (n)β n = n n +n p β = (n n n p )/n with symmetry energy E s (n) essential parameters: symmetry energy at saturation J = E s (n sat ) slope coefficient L = 3n d dn E s n=nsat Neutron Skins with α-clusters - 3
12 Neutron Skins and Symmetry Energy equivalent correlation of neutron skin thickness with slope of nuclear symmetry energy found in investigation guided by principles of effective field theory (R. J. Furnstahl, Nucl. Phys. 706 (2002) 85) expansion of energy per nucleon in nuclear matter E A (n,β) = E 0(n)+E s (n)β n = n n +n p β = (n n n p )/n with symmetry energy E s (n) essential parameters: symmetry energy at saturation J = E s (n sat ) slope coefficient L = 3n d dn E s n=nsat determine L from experimental measurement of r np constraint for neutron matter EoS r np (fm) HFB-8 MSk7 v090 SkP D1S Linear Fit, r = Skyrme, Gogny RMF SkX Sk-T6 HFB-17 SGII D1N SkM* FSUGold DD-ME1 DD-ME2 SLy5 SLy4 SkMP SkSM* SIV MSL0 MSkA BCP Ska DD-PC1 Sk-Rs PK1.s L (MeV) (X. Viñas et al., Eur. Phys. J. A50 (2014) 27) G2 Sk-T4 NL3.s25 RHF-PKO3 SkI2 RHF-PKA1 SV Sk-Gs NL3* NL3 PK1 NL-SV2 TM1 SkI5 G1 NL-RA1 PC-F1 NL-SH PC-PK1 NL2 208 Pb NL1 Neutron Skins with α-clusters - 3
13 Symmetry Energy Parameters many attempts to determine symmetry energy J = S 0 = S v and slope coefficient L experimentally χ Lagrangian and Q. Montecarlo Neutron Matter Neutron-Star Neutron Star Data Observations p & α scattering Neutron Skin charge ex. Antiprotonic Atoms Nuclear Model Fit Heavy Ion Collisions Giant Resonances N A scattering Charge Ex. Reactions Energy Levels Parity Violating e-scattering IVGQR Neutron Skin PDR Neutron Skin Mass Mass n p Emission Ratio Isospin Diffusion GDR PDR N Optical Potential Empirical Dipole Polarizability Parity Violating Asymmetry L (MeV) Hebeler et al. PRL105 (2010) and Gandolfi et al. PRC85 (2012) (R) Steiner et al. Astrophys. J. 722 (2010) 33 Lie-Wen Chen et al. PRC 82 (2010) Centelles et al. PRL 102 (2009) Warda et al. PRC 80 (2009) Möller et al. PRL 108 (2012) Danielewicz NPA 727 (2003) 233 Agrawal et al. PRL109 (2012) Famiano et al. PRL 97 (2006) Tsang et al. PRL 103 (2009) Roca-Maza et al. PRC 87 (2013) Roca-Maza et al. PRC (2013), in press Trippa et al. PRC 77 (2008) (R) Klimkiewicz et al. PRC 76 (2007) (R) Carbone et al. PRC 81 (2010) (R) Xu et al. PRC 82 (2010) PREX Collab. PRL (2012) (X. Viñas et al., Eur. Phys. J. A50 (2014) 27) (J.M. Lattimer, Y. Lim, ApJ. 771 (2013) 51) Neutron Skins with α-clusters - 4
14 Symmetry Energy Parameters many attempts to determine symmetry energy J = S 0 = S v and slope coefficient L experimentally χ Lagrangian and Q. Montecarlo Neutron Matter Neutron-Star Neutron Star Data Observations p & α scattering Neutron Skin charge ex. Antiprotonic Atoms Nuclear Model Fit Heavy Ion Collisions Giant Resonances N A scattering Charge Ex. Reactions Energy Levels Parity Violating e-scattering IVGQR Neutron Skin PDR Neutron Skin Mass Mass n p Emission Ratio Isospin Diffusion GDR PDR N Optical Potential Empirical Dipole Polarizability Parity Violating Asymmetry L (MeV) Hebeler et al. PRL105 (2010) and Gandolfi et al. PRC85 (2012) (R) Steiner et al. Astrophys. J. 722 (2010) 33 Lie-Wen Chen et al. PRC 82 (2010) Centelles et al. PRL 102 (2009) Warda et al. PRC 80 (2009) Möller et al. PRL 108 (2012) Danielewicz NPA 727 (2003) 233 Agrawal et al. PRL109 (2012) Famiano et al. PRL 97 (2006) Tsang et al. PRL 103 (2009) Roca-Maza et al. PRC 87 (2013) Roca-Maza et al. PRC (2013), in press Trippa et al. PRC 77 (2008) (R) Klimkiewicz et al. PRC 76 (2007) (R) Carbone et al. PRC 81 (2010) (R) Xu et al. PRC 82 (2010) PREX Collab. PRL (2012) (X. Viñas et al., Eur. Phys. J. A50 (2014) 27) (J.M. Lattimer, Y. Lim, ApJ. 771 (2013) 51) measurement of neutron skin thickness (e.g. PREX), correlation with L from mean-field calculations: effects of clustering correlations on surface of nuclei? Neutron Skins with α-clusters - 4
15 Correlations in Low-Density Nuclear Matter surface of nuclei: densities much below saturation density nucleon-nucleon pairing correlations essential, usually considered in nuclear structure calculations Neutron Skins with α-clusters - 5
16 Correlations in Low-Density Nuclear Matter surface of nuclei: densities much below saturation density nucleon-nucleon pairing correlations essential, usually considered in nuclear structure calculations equation of state of nuclear matter at very low densities: many-body correlations clusters/nuclei as new degrees of freedom model-independent benchmark: virial equation of state (see, e.g., C. J. Horowitz, A. Schwenk, Nucl. Phys. A 776 (2006) 55) Neutron Skins with α-clusters - 5
17 Correlations in Low-Density Nuclear Matter surface of nuclei: densities much below saturation density nucleon-nucleon pairing correlations essential, usually considered in nuclear structure calculations equation of state of nuclear matter at very low densities: many-body correlations clusters/nuclei as new degrees of freedom model-independent benchmark: virial equation of state (see, e.g., C. J. Horowitz, A. Schwenk, Nucl. Phys. A 776 (2006) 55) incorporate clusters as explicit degrees of freedom in nuclear structure calculations adaption of generalized relativistic density functional (grdf) approach for EoS of nuclear and stellar matter Neutron Skins with α-clusters - 5
18 Correlations in Low-Density Nuclear Matter surface of nuclei: densities much below saturation density nucleon-nucleon pairing correlations essential, usually considered in nuclear structure calculations equation of state of nuclear matter at very low densities: many-body correlations clusters/nuclei as new degrees of freedom model-independent benchmark: virial equation of state (see, e.g., C. J. Horowitz, A. Schwenk, Nucl. Phys. A 776 (2006) 55) incorporate clusters as explicit degrees of freedom in nuclear structure calculations adaption of generalized relativistic density functional (grdf) approach for EoS of nuclear and stellar matter nucleons and clusters treated as quasiparticles with scalar potential S i and vector potential V i interaction by meson exchange, well calibrated parametrisation Neutron Skins with α-clusters - 5
19 Correlations in Low-Density Nuclear Matter surface of nuclei: densities much below saturation density nucleon-nucleon pairing correlations essential, usually considered in nuclear structure calculations equation of state of nuclear matter at very low densities: many-body correlations clusters/nuclei as new degrees of freedom model-independent benchmark: virial equation of state (see, e.g., C. J. Horowitz, A. Schwenk, Nucl. Phys. A 776 (2006) 55) incorporate clusters as explicit degrees of freedom in nuclear structure calculations adaption of generalized relativistic density functional (grdf) approach for EoS of nuclear and stellar matter nucleons and clusters treated as quasiparticles with scalar potential S i and vector potential V i interaction by meson exchange, well calibrated parametrisation study dependence of results on neutron excess and on isovector part of interaction experimental test of predictions? Neutron Skins with α-clusters - 5
20 Generalized Relativistic Density Functional
21 Generalized Relativistic Density Functional grand canonical approach extension of relativistic mean-field models with density-dependent meson-nucleon couplings grand canonical potential density ω(t,{µ i }) Neutron Skins with α-clusters - 6
22 Generalized Relativistic Density Functional grand canonical approach extension of relativistic mean-field models with density-dependent meson-nucleon couplings grand canonical potential density ω(t,{µ i }) chemical equilibrium chemical potentials µ i of particles not all independent Neutron Skins with α-clusters - 6
23 Generalized Relativistic Density Functional grand canonical approach extension of relativistic mean-field models with density-dependent meson-nucleon couplings grand canonical potential density ω(t,{µ i }) chemical equilibrium chemical potentials µ i of particles not all independent selected model features extended set of constituents: nucleons, light clusters ( 2 H, 3 H, 3 He, 4 He) and heavy nuclei experimental binding energies: AME 2012 (M. Wang et al., Chinese Phys. 36 (2012) 1603) extension: DZ10 predictions (J. Duflo, A.P. Zuker, Phys. Rev. C 52 (1995) R23) proton number Z DZ AME neutron number N Neutron Skins with α-clusters - 6
24 Generalized Relativistic Density Functional grand canonical approach extension of relativistic mean-field models with density-dependent meson-nucleon couplings grand canonical potential density ω(t,{µ i }) chemical equilibrium chemical potentials µ i of particles not all independent selected model features extended set of constituents: nucleons, light clusters ( 2 H, 3 H, 3 He, 4 He) and heavy nuclei experimental binding energies: AME 2012 (M. Wang et al., Chinese Phys. 36 (2012) 1603) extension: DZ10 predictions proton number Z DZ AME neutron number N (J. Duflo, A.P. Zuker, Phys. Rev. C 52 (1995) R23) medium modifications of composite particles (mass shifts, internal excitations) scattering correlations considered (essential for correct low-density limit) thermodynamically consistent approach ( rearrangement contributions) model parameters from fit to properties of finite nuclei Neutron Skins with α-clusters - 6
25 Effective Interaction exchange of Lorentz scalar mesons m S = {σ,δ,σ,...} Lorentz vector mesons m V = {ω,ρ,φ,...} Neutron Skins with α-clusters - 7
26 Effective Interaction exchange of Lorentz scalar mesons m S = {σ,δ,σ,...} Lorentz vector mesons m V = {ω,ρ,φ,...} represented by (classical) fields A m with mass m m coupling to constituents: Γ im = g im Γ m scaling factors g im density dependent Γ m = Γ m ( ) = i (N i + Z i )n i with parametrization DD2 (S. Typel et al., Phys. Rev. C 81 (2010) ) meson-nucleon coupling Γ i (ρ) DD vector density ρ [fm -3 ] nuclear matter parameters n sat = fm 3 a V = MeV K = MeV J = MeV L = MeV ω σ ρ Neutron Skins with α-clusters - 7
27 Effective Interaction exchange of Lorentz scalar mesons m S = {σ,δ,σ,...} Lorentz vector mesons m V = {ω,ρ,φ,...} represented by (classical) fields A m with mass m m coupling to constituents: Γ im = g im Γ m scaling factors g im density dependent Γ m = Γ m ( ) = i (N i + Z i )n i with parametrization DD2 (S. Typel et al., Phys. Rev. C 81 (2010) ) scalar potential S i = m S Γ ima m m i with medium-dependent mass shift m i (T,n j ) from microscopic calculations mainly action of Pauli principle dissolution of clusters at high densities meson-nucleon coupling Γ i (ρ) DD vector density ρ [fm -3 ] nuclear matter parameters n sat = fm 3 a V = MeV K = MeV J = MeV L = MeV ω σ ρ Neutron Skins with α-clusters - 7
28 Effective Interaction exchange of Lorentz scalar mesons m S = {σ,δ,σ,...} Lorentz vector mesons m V = {ω,ρ,φ,...} represented by (classical) fields A m with mass m m coupling to constituents: Γ im = g im Γ m scaling factors g im density dependent Γ m = Γ m ( ) = i (N i + Z i )n i with parametrization DD2 (S. Typel et al., Phys. Rev. C 81 (2010) ) scalar potential S i = m S Γ ima m m i with medium-dependent mass shift m i (T,n j ) from microscopic calculations mainly action of Pauli principle dissolution of clusters at high densities vector potential V i = m V Γ ima m + V (r) i with rearrangement contribution V (r) i meson-nucleon coupling Γ i (ρ) DD vector density ρ [fm -3 ] nuclear matter parameters n sat = fm 3 a V = MeV K = MeV J = MeV L = MeV ω σ ρ Neutron Skins with α-clusters - 7
29 Effective Interaction exchange of Lorentz scalar mesons m S = {σ,δ,σ,...} Lorentz vector mesons m V = {ω,ρ,φ,...} represented by (classical) fields A m with mass m m coupling to constituents: Γ im = g im Γ m scaling factors g im density dependent Γ m = Γ m ( ) = i (N i + Z i )n i with parametrization DD2 (S. Typel et al., Phys. Rev. C 81 (2010) ) scalar potential S i = m S Γ ima m m i with medium-dependent mass shift m i (T,n j ) from microscopic calculations mainly action of Pauli principle dissolution of clusters at high densities energy per nucleon E/A [MeV] symmetric nuclear matter χeft (N 3 LO) DD2 neutron matter density n [fm -3 ] χeft(n 3 LO): I. Tews et al., Phys. Rev. Lett 110 (2013) T. Krüger et al., Phys. Rev. C 88 (2013) vector potential V i = m V Γ ima m + V (r) i with rearrangement contribution V (r) i Neutron Skins with α-clusters - 7
30 α-clusters on the Surface of Nuclei
31 Application of grdf Model finite temperature grdf calculations in spherical Wigner-Seitz cell, extended Thomas-Fermi approximation without light clusters 10-1 particle number density n i [fm -3 ] A heavy = Z heavy = 62.3 p n e T = 5 MeV n = 0.01 fm -3 Y p = radius r [fm] Neutron Skins with α-clusters - 8
32 Application of grdf Model finite temperature grdf calculations in spherical Wigner-Seitz cell, extended Thomas-Fermi approximation without and with light clusters enhanced cluster probability at surface of heavy nuclei, effects for heavy nuclei in vacuum at zero temperature? particle number density n i [fm -3 ] A heavy = Z heavy = 62.3 p n e T = 5 MeV n = 0.01 fm -3 Y p = 0.4 particle number density n i [fm -3 ] A heavy = Z heavy = 48.2 p n e 2 H 3 H 3 He 4 He T = 5 MeV n = 0.01 fm -3 Y p = radius r [fm] radius r [fm] Neutron Skins with α-clusters - 8
33 Application of grdf Model finite temperature grdf calculations in spherical Wigner-Seitz cell, extended Thomas-Fermi approximation zero temperature: only α-particles relevant density distribution from ground-state wave function (WKB approximation) Neutron Skins with α-clusters - 8
34 Application of grdf Model finite temperature grdf calculations in spherical Wigner-Seitz cell, extended Thomas-Fermi approximation zero temperature: only α-particles relevant density distribution from ground-state wave function (WKB approximation) variation with neutron excess of nuclei chain of Sn nuclei Neutron Skins with α-clusters - 8
35 Application of grdf Model finite temperature grdf calculations in spherical Wigner-Seitz cell, extended Thomas-Fermi approximation zero temperature: only α-particles relevant density distribution from ground-state wave function (WKB approximation) variation with neutron excess of nuclei chain of Sn nuclei variation of isovector interaction modified parametrizations, 208 Pb nucleus parametrization symmetry slope ρ-meson ρ-meson energy coefficient coupling parameter J [MeV] L [MeV] Γ ρ (n ref ) a ρ DD DD DD DD DD DD [ )] Γρ(n) = Γρ(n ref )exp aρ( n n 1 ref Neutron Skins with α-clusters - 8
36 Application of grdf Model finite temperature grdf calculations in spherical Wigner-Seitz cell, extended Thomas-Fermi approximation zero temperature: only α-particles relevant density distribution from ground-state wave function (WKB approximation) variation with neutron excess of nuclei chain of Sn nuclei variation of isovector interaction modified parametrizations, 208 Pb nucleus parametrization symmetry slope ρ-meson ρ-meson energy coefficient coupling parameter J [MeV] L [MeV] Γ ρ (n ref ) a ρ DD DD DD DD DD DD energy per neutron E/A [MeV] DD2 +++ DD2 ++ DD2 + DD2 DD2 - DD2 - - neutron matter [ )] Γρ(n) = Γρ(n ref )exp aρ( n n 1 ref neutron density n [fm -3 ] Neutron Skins with α-clusters - 8
37 Neutron Skin of Sn Nuclei neutron and protons rms radii r n and r p neutron skin thickness r skin = r n r p neutron (proton) rms radius r n (r p ) [fm] neutrons (without α correlations) protons (without α correlations) neutron skin thickness r skin [fm] without α correlations mass number A mass number A Neutron Skins with α-clusters - 9
38 Neutron Skin of Sn Nuclei neutron and protons rms radii r n and r p neutron skin thickness r skin = r n r p neutron (proton) rms radius r n (r p ) [fm] neutrons (without α correlations) neutrons (with α correlations) protons (without α correlations) protons (with α correlations) neutron skin thickness r skin [fm] without α correlations with α correlations mass number A mass number A Neutron Skins with α-clusters - 9
39 Neutron Skin of Sn Nuclei density distributions of neutrons (dashed lines) and α particles (full lines) neutron skin thickness r skin = r n r p Sn 112 Sn 0.20 without α correlations with α correlations α particle density n α (r) [fm -3 ] Sn 120 Sn 124 Sn 128 Sn 132 Sn neutron skin thickness r skin [fm] radius r [fm] mass number A Neutron Skins with α-clusters - 9
40 Neutron Skin of Sn Nuclei density distributions of neutrons (dashed lines) and α particles (full lines) effective α-particle number N α α particle density n α (r) [fm -3 ] Sn 112 Sn 116 Sn 120 Sn 124 Sn 128 Sn 132 Sn effective number of α-particles N α radius r [fm] mass number A Neutron Skins with α-clusters - 9
41 Neutron Skin of Sn Nuclei density distributions of neutrons (dashed lines) and α particles (full lines) effective α-particle number N α experimental test of predictions? α particle density n α (r) [fm -3 ] Sn 112 Sn 116 Sn 120 Sn 124 Sn 128 Sn 132 Sn effective number of α-particles N α radius r [fm] mass number A Neutron Skins with α-clusters - 9
42 Neutron Skin of 208 Pb dependence on symmetry energy slope coefficient L use parametrizations DD2 +++,..., DD2 relativistic Hartree (RH) calculation used in original fit of model parameters (correlation r skin L not linear because no complete refit of model parameters, only of effective isovector interaction) neutron skin thickness r skin [fm] RH without α correlations slope coefficient L [MeV] Neutron Skins with α-clusters - 10
43 Neutron Skin of 208 Pb dependence on symmetry energy slope coefficient L use parametrizations DD2 +++,..., DD2 relativistic Hartree (RH) calculation used in original fit of model parameters relativistic Thomas-Fermi (RTF) calculation for description of nuclei with generalized relativistic density functional underestimate of neutron skin thickness but similar correlation as in RH calculation neutron skin thickness r skin [fm] RH without α correlations RTF without α correlations slope coefficient L [MeV] Neutron Skins with α-clusters - 10
44 Neutron Skin of 208 Pb dependence on symmetry energy slope coefficient L use parametrizations DD2 +++,..., DD2 relativistic Hartree (RH) calculation used in original fit of model parameters relativistic Thomas-Fermi (RTF) calculation for description of nuclei with generalized relativistic density functional underestimate of neutron skin thickness but similar correlation as in RH calculation with α-particles at surface systematic reduction of neutron skin neutron skin thickness r skin [fm] RH without α correlations RTF without α correlations RTF with α correlations slope coefficient L [MeV] Neutron Skins with α-clusters - 10
45 Experimental Test
46 Experimental Study of α-clustering at Nuclear Surface clean probe for α-particles in nuclei: quasi-free (p,pα) knockout reactions Neutron Skins with α-clusters - 11
47 Experimental Study of α-clustering at Nuclear Surface clean probe for α-particles in nuclei: quasi-free (p,pα) knockout reactions experiment at RCNP Cyclotron Facility, Osaka, Japan collaboration with T. Aumann (TU Darmstadt), T. Uesaka (RIKEN) et al. proposal accepted in PAC evaluation March 2014, experiment planned for 2015 Neutron Skins with α-clusters - 11
48 Experimental Study of α-clustering at Nuclear Surface clean probe for α-particles in nuclei: quasi-free (p,pα) knockout reactions experiment at RCNP Cyclotron Facility, Osaka, Japan collaboration with T. Aumann (TU Darmstadt), T. Uesaka (RIKEN) et al. proposal accepted in PAC evaluation March 2014, experiment planned for MeV proton beam targets: 112 Sn, 116 Sn, 120 Sn, 124 Sn proton detection: Grand Raiden α detection: LAS several spectrometer settings p Sn α Neutron Skins with α-clusters - 11
49 Experimental Study of α-clustering at Nuclear Surface clean probe for α-particles in nuclei: quasi-free (p,pα) knockout reactions experiment at RCNP Cyclotron Facility, Osaka, Japan collaboration with T. Aumann (TU Darmstadt), T. Uesaka (RIKEN) et al. proposal accepted in PAC evaluation March 2014, experiment planned for MeV proton beam targets: 112 Sn, 116 Sn, 120 Sn, 124 Sn proton detection: Grand Raiden α detection: LAS several spectrometer settings experimental signatures: dependence of effective α-particle number ( cross sections) on neutron excess N Z localisation of α-particles on surface of nucleus broad momentum distribution p Sn α Neutron Skins with α-clusters - 11
50 Quasi-Free (p,pα) Reactions on Sn 300 MeV kinematics low momentum transfer to residual Cd nucleus Neutron Skins with α-clusters - 12
51 Quasi-Free (p,pα) Reactions on Sn 300 MeV kinematics low momentum transfer to residual Cd nucleus strong correlation of angles/energies of emitted protons and α-particles E lab (p) [MeV] E lab (α) [MeV] θ lab (p) [deg] θ lab (p) [deg] θ lab (α) [deg] θ lab (α) [deg] Neutron Skins with α-clusters - 12
52 Quasi-Free (p,pα) Reactions on Sn 300 MeV θlab(p) [deg] Neutron Skins with α-clusters θlab(α) [deg] p α lab p [MeV/c] 300 θlab(p) [deg] 300 Elab(α) [MeV] Elab(p) [MeV] kinematics low momentum transfer to residual Cd nucleus strong correlation of angles/energies of emitted protons and α-particles select pair of angles, e.g., θlab(p) = 45 and θlab(α) = 60 choose spectrometer settings to cover different ranges of intrinsic α-particle momenta Q within acceptance (p, Grand Raiden: 5%, α, LAS: 30%) θlab(α) [deg] Q [MeV/c]
53 Quasi-Free (p,pα) Reactions on Sn 300 MeV cross sections relativistic distorted-wave impulse approximation Neutron Skins with α-clusters - 13
54 Quasi-Free (p,pα) Reactions on Sn 300 MeV cross sections relativistic distorted-wave impulse approximation factorization d 5 σ dqdω Q dω p = K d2 σ dω p W α( Q) R kinematic factor K Neutron Skins with α-clusters - 13
55 Quasi-Free (p,pα) Reactions on Sn 300 MeV cross sections relativistic distorted-wave impulse approximation factorization d 5 σ dqdω Q dω p = K d2 σ dω p W α( Q) R kinematic factor K half-off-shell p-α scattering cross section d2 σ dω p use parametrized experimental elastic p-α scattering cross section dσ/dω p cm [mb/sr] elastic 4 He(p,p) MeV Yoshimura et al., PRC 63 (2001) cm θ p [deg] Neutron Skins with α-clusters - 13
56 Quasi-Free (p,pα) Reactions on Sn 300 MeV cross sections relativistic distorted-wave impulse approximation factorization d 5 σ dqdω Q dω p = K d2 σ dω p W α( Q) R kinematic factor K half-off-shell p-α scattering cross section d2 σ dω p use parametrized experimental elastic p-α scattering cross section intrinsic momentum distribution W α ( Q) = χ α Cd ( Q) 2 with Q = k α Cd of α-particle in Sn nucleus reduction factor R due to absorption dσ/dω p cm [mb/sr] W α (Q) [fm 3 ] elastic 4 He(p,p) MeV Yoshimura et al., PRC 63 (2001) cm θ p [deg] Sn Q [MeV/c] Neutron Skins with α-clusters - 13
57 Quasi-Free (p,pα) Reactions on Sn 300 MeV cross sections relativistic distorted-wave impulse approximation factorization d 5 σ dqdω Q dω = K d2 σ p dω W α( Q) R p kinematic factor K half-off-shell p-α scattering cross section d2 σ dω p use parametrized experimental elastic p-α scattering cross section intrinsic momentum distribution W α ( Q) = χ α Cd ( Q) 2 with Q = k α Cd of α-particle in Sn nucleus reduction factor R due to absorption Monte Carlo simulation of experiment estimate of count rates dσ/dω p cm [mb/sr] W α (Q) [fm 3 ] elastic 4 He(p,p) MeV Yoshimura et al., PRC 63 (2001) cm θ p [deg] Sn Q [MeV/c] Neutron Skins with α-clusters - 13
58 Conclusions
59 Conclusions many-body correlations essential in low-density nuclear matter formation of clusters/nuclei conditions at surface of heavy nuclei prerequisite for explanation of α-decay generalized relativistic density functional (grdf) for equation of state calculations model with explicit cluster degrees of freedom, quasiparticles with medium-dependent properties effective interaction with density-dependent couplings, well-constrained parameters application of grdf approach to heavy nuclei predicts formation of α-clusters at surface of heavy nuclei reduction of neutron skin thickness affects correlation with slope coefficient of symmetry energy systematic variation of effect with neutron excess of nucleus and with isovector part of effective interaction experimental test of predictions quasi-free (p,pα) knockout reactions experiment with Sn nuclei planned at RCNP, Osaka Neutron Skins with α-clusters - 14
Cluster Correlations in Dilute Matter and Nuclei
Cluster Correlations in Dilute Matter and Nuclei GSI Helmholtzzentrum für Schwerionenforschung, Darmstadt Nuclear Astrophysics Virtual Institute Workhop on Weakly Bound Exotic Nuclei International Institute
More informationDipole Polarizability and the neutron skin thickness
Dipole Polarizability and the neutron skin thickness Xavier Roca-Maza Università degli Studi di Milano and INFN Joint LIA COLL-AGAIN, COPIGAL, and POLITA Workshop, April 26th-29th 2016. 1 Table of contents:
More informationClusters in Dense Matter and the Equation of State
Clusters in Dense Matter and the Equation of State Excellence Cluster Universe, Technische Universität München GSI Helmholtzzentrum für Schwerionenforschung, Darmstadt in collaboration with Gerd Röpke
More informationThe pygmy dipole strength, the neutron skin thickness and the symmetry energy
The pygmy dipole strength, the neutron skin thickness and the symmetry energy Xavier Roca-Maza INFN, Sezione di Milano, Via Celoria 16, I-2133, Milano (Italy) Giacomo Pozzi Marco Brenna Kazhuito Mizuyama
More informationCluster Correlations in Dilute Matter
Cluster Correlations in Dilute Matter GSI Helmholtzzentrum für Schwerionenforschung, Darmstadt Nuclear Astrophysics Virtual Institute NUFRA 2015 Fifth International Conference on Nuclear Fragmentation
More informationThe dipole strength: microscopic properties and correlations with the symmetry energy and the neutron skin thickness
The dipole strength: microscopic properties and correlations with the symmetry energy and the neutron skin thickness Xavier Roca-Maza INFN, Sezione di Milano, Via Celoria 16, I-2133, Milano (Italy) Giacomo
More informationNature of low-energy dipole states in exotic nuclei
Nature of low-energy dipole states in exotic nuclei Xavier Roca-Maza Università degli Studi di Milano, Via Celoria 16, I-133, Milano SPES One-day Workshop on "Collective Excitations of Exotic Nuclei" December
More informationIsospin asymmetry in stable and exotic nuclei
Isospin asymmetry in stable and exotic nuclei Xavier Roca Maza 6 May 2010 Advisors: Xavier Viñas i Gausí and Mario Centelles i Aixalà Motivation: Nuclear Chart Relative Neutron excess I (N Z )/(N + Z )
More informationDipole Polarizability and Parity Violating Asymmetry in 208 Pb
Dipole Polarizability and Parity Violating Asymmetry in 208 Pb Xavier Roca-Maza INFN, Sezione di Milano, Via Celoria 16, I-20133, Milano (Italy) 2nd European Nuclear Physics Conference EuNPC 2012, 16-21
More informationarxiv: v1 [nucl-th] 26 Jun 2011
Study of the neutron skin thickness of 208 Pb in mean field models X. Roca-Maza 1,2, M. Centelles 1, X. Viñas 1 and M. Warda 1, 1 Departament d Estructura i Constituents de la Matèria and Institut de Ciències
More informationDipole Polarizability and the neutron skin thickness
Dipole Polarizability and the neutron skin thickness Xavier Roca-Maza Università degli Studi di Milano and INFN MITP Scientific Program Neutron Skins of Nuclei May 17th-27th 2016. 1 Table of contents:
More informationParity-Violating Asymmetry for 208 Pb
Parity-Violating Asymmetry for 208 Pb Matteo Vorabbi Dipartimento di Fisica - Università di Pavia INFN - Sezione di Pavia Rome - 2015 January 15 Matteo Vorabbi (Università di Pavia) Parity-Violating Asymmetry
More informationDensity dependence of the nuclear symmetry energy estimated from neutron skin thickness in finite nuclei
Density dependence of the nuclear symmetry energy estimated from neutron skin thickness in finite nuclei X. Viñas a M. Centelles a M. Warda a,b X. Roca-Maza a,c a Departament d Estructura i Constituents
More informationPygmy dipole resonances in stable and unstable nuclei
Pygmy dipole resonances in stable and unstable nuclei Xavier Roca-Maza INFN, Sezione di Milano, Via Celoria 16, I-2133, Milano (Italy) Collaborators: Giacomo Pozzi, Marco Brenna, Kazhuito Mizuyama and
More informationThe Nuclear Equation of State
The Nuclear Equation of State Theoretical models for nuclear structure studies Xavier Roca-Maza Università degli Studi di Milano e INFN, sezione di Milano Terzo Incontro Nazionale di Fisica Nucleare LNF,
More informationDensity dependence of the nuclear symmetry energy estimated from neutron skin thickness in finite nuclei
Density dependence of the nuclear symmetry energy estimated from neutron skin thickness in finite nuclei X. Roca-Maza a,c X. Viñas a M. Centelles a M. Warda a,b a Departament d Estructura i Constituents
More informationPb, 120 Sn and 48 Ca from High-Resolution Proton Scattering MSU 2016
Dipole Polarizability and Neutron Skins in 208 Pb, 120 Sn and 48 Ca from High-Resolution Proton Scattering MSU 2016 Equation of State of neutron matter and neutron skin Proton scattering at 0 and electric
More informationConstraining the symmetry energy based on relativistic point coupling interactions and excitations in finite nuclei
7 th International Symposium on Nuclear Symmetry Energy, GANIL (France) 4-7.9.2017 Constraining the symmetry energy based on relativistic point coupling interactions and excitations in finite nuclei N.
More informationProbing the Nuclear Symmetry Energy and Neutron Skin from Collective Excitations. N. Paar
Calcium Radius Experiment (CREX) Workshop at Jefferson Lab, March 17-19, 2013 Probing the Nuclear Symmetry Energy and Neutron Skin from Collective Excitations N. Paar Physics Department Faculty of Science
More informationDiscerning the symmetry energy and neutron star properties from nuclear collective excitations
International Workshop XLV on Gross Properties of Nuclei and Nuclear Excitations Hirschegg, Kleinwalsertal, Austria, January 15-21, 2017 Discerning the symmetry energy and neutron star properties from
More informationNuclear symmetry energy deduced from dipole excitations: comparison with other constraints
Nuclear symmetry energy deduced from dipole excitations: a comparison with other constraints G. Colò June 15th, 2010 This work is part of a longer-term research plan. The goal is: understanding which are
More informationEquation-of-State of Nuclear Matter with Light Clusters
Equation-of-State of Nuclear Matter with Light Clusters rmann Wolter Faculty of Physics, University of Munich, D-878 Garching, Germany E-mail: hermann.wolter@lmu.de The nuclear equation-of-state (EoS)
More informationarxiv: v1 [nucl-th] 14 Feb 2012
The pygmy dipole strength, the neutron radius of 8 Pb and the symmetry energy arxiv:1.38v1 [nucl-th] 14 Feb 1 X. Roca-Maza 1,, M. Brenna 1,3, M. Centelles, G. Colò 1,3, K. Mizuyama 1, G. Pozzi 3, X. Viñas
More informationDipole Response of Exotic Nuclei and Symmetry Energy Experiments at the LAND R 3 B Setup
Dipole Response of Exotic Nuclei and Symmetry Energy Experiments at the LAND R 3 B Setup Dominic Rossi for the LAND collaboration GSI Helmholtzzentrum für Schwerionenforschung GmbH D 64291 Darmstadt, Germany
More informationDensity dependence of the nuclear symmetry energy estimated from neutron skin thickness in finite nuclei
Density dependence of the nuclear symmetry energy estimated from neutron skin thickness in finite nuclei X. Roca-Maza a,b X. Viñas b M. Centelles b M. Warda b,c a INFN sezione di Milano. Via Celoria 16,
More informationThe Nuclear Equation of State and the neutron skin thickness in nuclei
The Nuclear Equation of State and the neutron skin thickness in nuclei Xavier Roca-Maza Università degli Studi di Milano e INFN, sezione di Milano Physics beyond the standard model and precision nucleon
More informationPREX and CREX. R N from Electroweak Asymmetry in Elastic Electron-Nucleus Scattering. Neutron Skin.
http://hallaweb.jlab.org/parity/prex PREX and CREX 08 Pb Horowitz 48 Ca Neutron Skin R N from Electroweak Asymmetry in Elastic Electron-Nucleus Scattering R L 4 6 A ~ 10 PV Q ~ 10 R L PRL 108 (01) 1150
More informationThe Nuclear Symmetry Energy: constraints from. Giant Resonances. Xavier Roca-Maza
The Nuclear Symmetry Energy: constraints from Giant Resonances Xavier Roca-Maza Dipartimento di Fisica, Università degli Studi di Milano and INFN, Sezione di Milano Trobada de Nadal 2012 Table of contents:
More informationRelativistic Radioactive Beams as a Tool for Nuclear Astrophysics
Relativistic Radioactive Beams as a Tool for Nuclear Astrophysics Thomas Aumann December 11 th 2013 27 th Texas Symposium on Relativistic Astrophysics Dallas, Texas Supported by the BMBF under contract
More informationDipole Polarizability and Parity Violating Asymmetry in 208 Pb
Dipole Polarizability and Parity Violating Asymmetry in 208 Pb Xavier Roca-Maza INFN, Sezione di Milano, Via Celoria 16, I-20133, Milano (Italy) Nuclear Structure and Dynamics II. July 9th to 13th 2012.
More informationTowards a universal nuclear structure model. Xavier Roca-Maza Congresso del Dipartimento di Fisica Milano, June 28 29, 2017
Towards a universal nuclear structure model Xavier Roca-Maza Congresso del Dipartimento di Fisica Milano, June 28 29, 217 1 Table of contents: Brief presentation of the group Motivation Model and selected
More informationInner crust composition and transition densities
Inner crust composition and transition densities W.G.Newton 1, Bao-An Li 1, J.R.Stone 2,3 M. Gearheart 1, J. Hooker 1 1 Texas A&M University - Commerce 2 University of Oxford, UK 3 Physics Division, ORNL,
More informationParity violating asymmetry, dipole polarizability, and the neutron skin thickness in 48 Ca and 208 Pb
Parity violating asymmetry, dipole polarizability, and the neutron skin thickness in 48 Ca and 208 Pb Xavier Roca-Maza Università degli Studi di Milano and INFN Via Celoria 16, I-20133, Milano (Italy)
More informationCorrelating the density dependence of the symmetry y energy to neutron skins and neutron-star properties
Correlating the density dependence of the symmetry y energy to neutron skins and neutron-star properties Farrukh J Fattoyev Texas A&M University-Commerce i My TAMUC collaborators: B.-A. Li, W. G. Newton
More informationParity violating asymmetry, dipole polarizability, and the neutron skin thickness in 48 Ca and 208 Pb
Parity violating asymmetry, dipole polarizability, and the neutron skin thickness in 48 Ca and 208 Pb Xavier Roca-Maza Università degli Studi di Milano and INFN Via Celoria 16, I-20133, Milano (Italy)
More informationClusters in Nuclear Matter
Clusters in Nuclear Matter Excellence Cluster Universe, Technische Universität München GSI Helmholtzzentrum für Schwerionenforschung, Darmstadt in collaboration with Gerd Röpke (Universität Rostock) Thomas
More informationMomentum 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( ) = (
More informationSymmetry energy of dilute warm nuclear matter
Symmetry energy of dilute warm nuclear matter J. B. Natowitz, G. Röpke, 1 S. Typel, 2,3 D. Blaschke, 4, 5 A. Bonasera, 6 K. Hagel, T. Klähn, 4, 7 S. Kowalski, L. Qin, S. Shlomo, R. Wada, and H. H. Wolter
More informationReactions of neutron-rich Sn isotopes investigated at relativistic energies at R 3 B
investigated at relativistic energies at R 3 B for the R 3 B collaboration Technische Universität Darmstadt E-mail: fa.schindler@gsi.de Reactions of neutron-rich Sn isotopes have been measured in inverse
More informationDensity dependence of the symmetry energy and the nuclear equation of state : A dynamical and statistical model perspective
Density dependence of the symmetry energy and the nuclear equation of state : A dynamical and statistical model perspective D. V. Shetty, S. J. Yennello, and G. A. Souliotis The density dependence of the
More informationNuclear Matter Incompressibility and Giant Monopole Resonances
Nuclear Matter Incompressibility and Giant Monopole Resonances C.A. Bertulani Department of Physics and Astronomy Texas A&M University-Commerce Collaborator: Paolo Avogadro 27th Texas Symposium on Relativistic
More informationLisheng Geng. Ground state properties of finite nuclei in the relativistic mean field model
Ground state properties of finite nuclei in the relativistic mean field model Lisheng Geng Research Center for Nuclear Physics, Osaka University School of Physics, Beijing University Long-time collaborators
More informationBeyond mean-field study on collective vibrations and beta-decay
Advanced many-body and statistical methods in mesoscopic systems III September 4 th 8 th, 2017, Busteni, Romania Beyond mean-field study on collective vibrations and beta-decay Yifei Niu Collaborators:
More informationAn empirical approach combining nuclear physics and dense nucleonic matter
An empirical approach combining nuclear physics and dense nucleonic matter Univ Lyon, Université Lyon 1, IN2P3-CNRS, Institut de Physique Nucléaire de Lyon, F-69622 Villeurbanne, France E-mail: j.margueron@ipnl.in2p3.fr
More informationCurrent status and challenges of ab-initio computations of nuclei
Current status and challenges of ab-initio computations of nuclei Gaute Hagen Oak Ridge National Laboratory INT workshop on Nuclear Physics from Lattice QCD INT, May 5th, 2016 Computing real nuclei from
More informationGianluca Colò. Density Functional Theory for isovector observables: from nuclear excitations to neutron stars. Università degli Studi and INFN, MIlano
Density Functional Theory for isovector observables: from nuclear excitations to neutron stars Gianluca Colò NSMAT2016, Tohoku University, Sendai 1 Outline Energy density functionals (EDFs): a short introduction
More informationEvolution Of Shell Structure, Shapes & Collective Modes. Dario Vretenar
Evolution Of Shell Structure, Shapes & Collective Modes Dario Vretenar vretenar@phy.hr 1. Evolution of shell structure with N and Z A. Modification of the effective single-nucleon potential Relativistic
More informationThe Isovector Giant Dipole Resonance
Giant Resonances First Experiments: G.C.Baldwin and G.S. Klaiber, Phys.Rev. 71, 3 (1947) General Electric Research Laboratory, Schenectady, NY Theoretical Explanation: M. Goldhaber and E. Teller, Phys.
More informationStructure properties of medium and heavy exotic nuclei
Journal of Physics: Conference Series Structure properties of medium and heavy exotic nuclei To cite this article: M K Gaidarov 212 J. Phys.: Conf. Ser. 381 12112 View the article online for updates and
More informationNuclear physics and cosmology. From outer space to deep inside Introduction to Nuclear Astrophysics.
Nuclear physics and cosmology. From outer space to deep inside Introduction to Nuclear Astrophysics. WHY modern nuclear physics is so COOL? (a short introduction) The nuclear realm Simplicity Hot and dense
More informationNuclear Symmetry Energy Constrained by Cluster Radioactivity. Chang Xu ( 许昌 ) Department of Physics, Nanjing University
Nuclear Symmetry Energy Constrained by Cluster Radioactivity Chang Xu ( 许昌 ) Department of Physics, Nanjing University 2016.6.13-18@NuSym2016 Outline 1. Cluster radioactivity: brief review and our recent
More informationSome new developments in relativistic point-coupling models
Some new developments in relativistic point-coupling models T. J. Buervenich 1, D. G. Madland 1, J. A. Maruhn 2, and P.-G. Reinhard 3 1 Los Alamos National Laboratory 2 University of Frankfurt 3 University
More informationTheory of neutron-rich nuclei and nuclear radii Witold Nazarewicz (with Paul-Gerhard Reinhard) PREX Workshop, JLab, August 17-19, 2008
Theory of neutron-rich nuclei and nuclear radii Witold Nazarewicz (with Paul-Gerhard Reinhard) PREX Workshop, JLab, August 17-19, 2008 Introduction to neutron-rich nuclei Radii, skins, and halos From finite
More informationClusters in Low-Density Nuclear Matter
Clusters in Low-Density Nuclear Matter Excellence Cluster Universe, Technische Universität München GSI Helmholtzzentrum für Schwerionenforschung, Darmstadt Helmholtz International Summer School: Nuclear
More informationNuclear equation of state for supernovae and neutron stars
Nuclear equation of state for supernovae and neutron stars H. Shen 申虹 In collaboration with Nankai University, Tianjin, China 南開大学 天津 中国 H. Toki RCNP, Osaka University, Japan K. Sumiyoshi Numazu College
More informationNuclear symmetry energy and Neutron star cooling
Nuclear symmetry energy and Neutron star cooling Yeunhwan Lim 1 1 Daegu University. July 26, 2013 In Collaboration with J.M. Lattimer (SBU), C.H. Hyun (Daegu), C-H Lee (PNU), and T-S Park (SKKU) NuSYM13
More informationNuclear Symmetry Energy and its Density Dependence. Chang Xu Department of Physics, Nanjing University. Wako, Japan
Nuclear Symmetry Energy and its Density Dependence Chang Xu Department of Physics, Nanjing University 2016.8.17-21@RIKEN, Wako, Japan Outline 1. Brief Review: Nuclear symmetry energy 2. What determines
More informationSymmetry Energy within the Brueckner-Hartree-Fock approximation
Symmetry Energy within the Brueckner-Hartree-Fock approximation Isaac Vidaña CFC, University of Coimbra International Symposium on Nuclear Symmetry Energy Smith College, Northampton ( Massachusetts) June
More informationThe oxygen anomaly F O
The oxygen anomaly O F The oxygen anomaly - not reproduced without 3N forces O F without 3N forces, NN interactions too attractive many-body theory based on two-nucleon forces: drip-line incorrect at 28
More informationHeavy-ion reactions and the Nuclear Equation of State
Heavy-ion reactions and the Nuclear Equation of State S. J. Yennello Texas A&M University D. Shetty, G. Souliotis, S. Soisson, Chen, M. Veselsky, A. Keksis, E. Bell, M. Jandel Studying Nuclear Equation
More informationStructure of Atomic Nuclei. Anthony W. Thomas
Structure of Atomic Nuclei Anthony W. Thomas JLab Users Meeting Jefferson Lab : June 2 nd 2015 The Issues What lies at the heart of nuclear structure? Start from a QCD-inspired model of hadron structure
More informationAn extended liquid drop approach
An extended liquid drop approach Symmetry energy, charge radii and neutron skins Lex Dieperink 1 Piet van Isacker 2 1 Kernfysisch Versneller Instituut University of Groningen 2 GANIL, Caen, France ECT,
More informationInvestigation of the Giant Monopole Resonance in the Cd and Pb Isotopes: The Asymmetry Term in Nuclear Incompressibility and the MEM Effect
460 Progress of Theoretical Physics Supplement No. 196, 2012 Investigation of the Giant Monopole Resonance in the Cd and Pb Isotopes: The Asymmetry Term in Nuclear Incompressibility and the MEM Effect
More informationDipole Polarizability, parity violating asymmetry and the neutron skin thickness Xavier Roca-Maza Università degli Studi di Milano and INFN
Dipole Polarizability, parity violating asymmetry and the neutron skin thickness Xavier Roca-Maza Università degli Studi di Milano and INFN Institute of Theoretical Physics Chinese Academy of Sciences
More informationComputational Advances in Nuclear and Hadron Physics, Kyoto, Constraining the Relativistic Nuclear Energy Density Functional
Computational Advances in Nuclear and Hadron Physics, Kyoto, 21.09.-30.10. 2015 Constraining the Relativistic Nuclear Energy Density Functional N. Paar Department of Physics, Faculty of Science, University
More informationNeutron matter from chiral effective field theory interactions
Neutron matter from chiral effective field theory interactions Ingo Tews, In collaboration with K. Hebeler, T. Krüger, A. Schwenk, JINA Neutron Stars, May 26, 2016, Athens, OH Chiral effective field theory
More informationElectric Dipole Response of 208 Pb and Constraints on the Symmetry Energy. Atsushi Tamii
Electric Dipole Response of 208 Pb and Constraints on the Symmetry Energy Atsushi Tamii Research Center for Nuclear Physics (RCNP) Osaka University, Japan I.Poltoratska, P. von Neumann Cosel and RCNP E282
More informationNeutron Rich Nuclei in Heaven and Earth
First Prev Next Last Go Back Neutron Rich Nuclei in Heaven and Earth Jorge Piekarewicz with Bonnie Todd-Rutel Tallahassee, Florida, USA Page 1 of 15 Cassiopeia A: Chandra 08/23/04 Workshop on Nuclear Incompressibility
More informationElectromagnetic reactions from few to many-body systems Giuseppina Orlandini
Electromagnetic reactions from few to many-body systems Giuseppina Orlandini ECT* Workshop on Recent advances and challenges in the description of nuclear reactions at the limit of stability, March 5-9,
More informationIAS and Skin Constraints. Symmetry Energy
IS and Skin Constraints on the Pawel Natl Superconducting Cyclotron Lab, US 32 nd International Workshop on Nuclear July, 2013, East Lansing, Michigan ρ in Nuclear Mass Formula Textbook Bethe-Weizsäcker
More informationThe uncertainty quantification in covariant density functional theory.
The uncertainty quantification in covariant density functional theory. Anatoli Afanasjev Mississippi State University (MSU), USA 1. Motivation. 2. Basic features of CDFT 3. Assessing statistical errors
More informationarxiv: v1 [nucl-th] 29 Jun 2009
Neutron/proton ratio oucleon emissions as a probe of neutron skin arxiv:0906.5281v1 [nucl-th] 29 Jun 2009 X. Y. Sun a,b, D. Q. Fang a, Y. G. Ma a, X. Z. Cai a, J. G. Chen a, W. Guo a, W. D. Tian a, H.
More informationCollective excitations in nuclei away from the valley of stability
Collective excitations in nuclei away from the valley of stability A. Horvat 1, N. Paar 16.7.14, CSSP 14, Sinaia, Romania 1 Institut für Kernphysik, TU Darmstadt, Germany (for the R3B-LAND collaboration)
More informationBetty Tsang, NSCL/MSU 曾敏兒. collaboration
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,
More informationPeter Ring. ISTANBUL-06 New developments in covariant density functional theory. Saariselkä April 20, 2009
ISTANBUL-06 New developments in covariant density functional theory Saariselkä April 20, 2009 Peter Ring Technical University Munich Universidad Autónoma de Madrid 1 Content Covariant density functionals
More informationFAIR. Reiner Krücken for the NUSTAR collaboration
NUSTAR @ FAIR Reiner Krücken for the NUSTAR collaboration Physik Department E12 Technische Universität München & Maier-Leibnitz-Laboratory for Nuclear and Particle Physics NUSTAR @ FAIR Nuclear Structure
More informationNuclear Structure for the Crust of Neutron Stars
Nuclear Structure for the Crust of Neutron Stars Peter Gögelein with Prof. H. Müther Institut for Theoretical Physics University of Tübingen, Germany September 11th, 2007 Outline Neutron Stars Pasta in
More informationLaboratory, Michigan State University, East Lansing, MI 48824, USA. East Lansing, MI 48824, USA. Abstract
Constraints on the density dependence of the symmetry energy M.B. Tsang( 曾敏兒 ) 1,2*, Yingxun Zhang( 张英逊 ) 1,3, P. Danielewicz 1,2, M. Famiano 4, Zhuxia Li( 李祝霞 ) 3, W.G. Lynch( 連致標 ) 1,2, A. W. Steiner
More informationThree-nucleon forces and neutron-rich nuclei
Three-nucleon forces and neutron-rich nuclei Achim Schwenk Facets of Strong Interaction Physics Hirschegg 40 + Bengt 60, Jan. 18, 2012 Happy Birthday Bengt! Outline Understanding three-nucleon forces Three-body
More informationProbing Nuclear Structure of Medium and Heavy Unstable Nuclei and Processes with Helium Isotopes
Probing Nuclear Structure of Medium and Heavy Unstable Nuclei and Processes with Helium Isotopes M.K. Gaidarov Institute for Nuclear Research and Nuclear Energy, Bulgarian Academy of Sciences, Sofia 1784,
More informationQRPA Calculations of Charge Exchange Reactions and Weak Interaction Rates. N. Paar
Strong, Weak and Electromagnetic Interactions to probe Spin-Isospin Excitations ECT*, Trento, 28 September - 2 October 2009 QRPA Calculations of Charge Exchange Reactions and Weak Interaction Rates N.
More informationNucelon self-energy in nuclear matter and how to probe ot with RIBs
Nucelon self-energy in nuclear matter and how to probe ot with RIBs Christian Fuchs University of Tübingen Germany Christian Fuchs - Uni Tübingen p.1/?? Outline relativistic dynamics E/A [MeV] 6 5 4 3
More informationNuclear symmetry energy and neutron skin thickness
Nuclear symmetry energy and neutron skin thickness M. Warda arxiv:1202.4612v1 [nucl-th] 21 Feb 2012 Katedra Fizyki Teoretycznej, Uniwersytet Marii Curie Sk lodowskiej, ul. Radziszewskiego 10, 20-031 Lublin,
More informationEquation of state for supernovae and neutron stars
Equation of state for supernovae and neutron stars H. Shen Nankai University, Tianjin, China 申虹南開大学天津中国 In collaboration with H. Toki RCNP, Osaka University, Japan K. Sumiyoshi Numazu College of Technology,
More informationNuclear Equation of State for High Density Matter. Matthias Hempel, Basel University NuPECC meeting Basel,
Nuclear Equation of State for High Density Matter, Basel University NuPECC meeting Basel, 12.06.2015 Equation of State for Compact Stars neutron stars core-collapse supernova explosions MH Liebendörfer
More informationLinking nuclear reactions and nuclear structure to on the way to the drip lines
Linking nuclear reactions and nuclear structure to on the way to the drip lines DREB18 6/5/2018 Motivation Green s functions/propagator method Wim Dickhoff Bob Charity Lee Sobotka Hossein Mahzoon (Ph.D.2015)
More informationThe isospin dependence of the nuclear force and its impact on the many-body system
Journal of Physics: Conference Series OPEN ACCESS The isospin dependence of the nuclear force and its impact on the many-body system To cite this article: F Sammarruca et al 2015 J. Phys.: Conf. Ser. 580
More informationPhotopion photoproduction and neutron radii
Photopion photoproduction and neutron radii Dan Watts, Claire Tarbert University of Edinburgh Crystal Ball and A2 collaboration at MAMI Jefferson Lab PREX workshop, August 2008 Talk Outline Nuclear (π
More informationThe Nuclear Many-Body Problem
The Nuclear Many-Body Problem relativistic heavy ions vacuum electron scattering quarks gluons radioactive beams heavy few nuclei body quark-gluon soup QCD nucleon QCD few body systems many body systems
More informationRelativistic Hartree-Bogoliubov description of sizes and shapes of A = 20 isobars
Relativistic Hartree-Bogoliubov description of sizes and shapes of A = 20 isobars G.A. Lalazissis 1,2, D. Vretenar 1,3, and P. Ring 1 arxiv:nucl-th/0009047v1 18 Sep 2000 1 Physik-Department der Technischen
More informationThe crust-core transition and the stellar matter equation of state
The crust-core transition and the stellar matter equation of state Helena Pais CFisUC, University of Coimbra, Portugal Nuclear Physics, Compact Stars, and Compact Star Mergers YITP, Kyoto, Japan, October
More informationNeutron Halo in Deformed Nuclei
Advances in Nuclear Many-Body Theory June 7-1, 211, Primosten, Croatia Neutron Halo in Deformed Nuclei Ó Li, Lulu Ò School of Physics, Peking University June 8, 211 Collaborators: Jie Meng (PKU) Peter
More informationInvestigations on Nuclei near Z = 82 in Relativistic Mean Field Theory with FSUGold
Plasma Science and Technology, Vol.14, No.6, Jun. 2012 Investigations on Nuclei near Z = 82 in Relativistic Mean Field Theory with FSUGold SHENG Zongqiang ( ) 1,2, REN Zhongzhou ( ) 1,2,3 1 Department
More informationConstraining the nuclear EoS by combining nuclear data and GW observations
Constraining the nuclear EoS by combining nuclear data and GW observations Michael McNeil Forbes Washington State University (Pullman) and University of Washington A Minimal Nuclear Energy Density Functional
More informationExtracting symmetry energy information with transport models
Extracting symmetry energy information with transport models Yingxun Zhang China Institute of Atomic Energy Collaborator: Zhuxia Li (CIAE) M.B.Tsang, P. Danielewicz, W.G. Lynch (MSU/NSCL) Fei Lu (PKU)
More informationSymmetry Energy Constraints From Neutron Stars and Experiment
Symmetry Energy Constraints From Neutron Stars and Experiment Department of Physics & Astronomy Stony Brook University 17 January 2012 Collaborators: E. Brown (MSU), K. Hebeler (OSU), C.J. Pethick (NORDITA),
More informationarxiv:astro-ph/ v2 24 Apr 2001
Neutron Star Structure and the Neutron Radius of 208 Pb C. J. Horowitz Nuclear Theory Center and Dept. of Physics, Indiana University, Bloomington, IN 47405 J. Piekarewicz Department of Physics Florida
More informationInteraction cross sections for light neutron-rich nuclei
PHYSICAL REVIEW C, VOLUME 65, 014612 Interaction cross sections for light neutron-rich nuclei B. A. Brown and S. Typel Department of Physics and Astronomy and National Superconducting Cyclotron Laboratory,
More informationModeling the EOS. Christian Fuchs 1 & Hermann Wolter 2. 1 University of Tübingen/Germany. 2 University of München/Germany
Modeling the EOS Christian Fuchs 1 & Hermann Wolter 2 1 University of Tübingen/Germany 2 University of München/Germany Christian Fuchs - Uni Tübingen p.1/20 Outline Christian Fuchs - Uni Tübingen p.2/20
More informationNuclear Reactions with light ion and photon beams; Contributions to Neutrino Astrophysics
Nuclear Reactions with light ion and photon beams; Contributions to Neutrino Astrophysics 1. Incompressibility and Giant Resonances (ISGMR, ISGDR) 2. Charge exchange reactions 3. Photon Beams for (g,g
More information