Nuclear physics and cosmology. From outer space to deep inside Introduction to Nuclear Astrophysics.

Transcription

1 Nuclear physics and cosmology. From outer space to deep inside Introduction to Nuclear Astrophysics.

2 WHY modern nuclear physics is so COOL? (a short introduction)

3 The nuclear realm Simplicity Hot and dense quark-gluon matter Hadron structure Hadron-Nuclear interface Resolution Nuclear structure Nuclear reactions Nuclear astrophysics Applications of nuclear science LRP Nuclear Science Advisory Committee(2008) Complexity

4 The nuclear realm Simplicity Hot and dense quark-gluon matter Hadron structure Hadron-Nuclear interface Resolution Nuclear structure Nuclear reactions Nuclear astrophysics Applications of nuclear science LRP Nuclear Science Advisory Committee(2008) Complexity

5 SCALES and PHASES of NUCLEAR MATTER Courtesy R.F.Casten (WNSL) OUTWARD LOOKING LOOKING INWARD Hot and Dense Matter Neutron Stars Nuclear Astrophysics Nuclear Structure Hypernuclei Nucleon

6 The SCALES: first constraint QCD in the non-perturbative regime If the Lord Almighty had consulted me before embarking upon creation, I would have recommended something simpler. King Alphonse X. of Castille and Léon ( ), on having the Ptolemaic system of epicycles explained to him F. Wilczek QCD made simple (

7 The SCALES: first constraint Modern nuclear physics is about... Linking QCD to many body systems UNEDF SciDAC Collaboration Universal Nuclear Energy Density Functional

8 Ab initio Nuclear Structure: an experimentalist point of view courtesy R. Roth

9 Ab initio Nuclear Structure courtesy R. Roth

10 Effective Field Theories courtesy R. Roth

11 ! $&,45*6(%&76(8/)*! Two-nucleon Zwei-Nukleon-Kraft force Three-nucleon Drei-Nukleon-Kraft force Four-nucleon Vier-Nukleon-Kraft force Effective Field Theories!!!! 16(*,$$&3&"6(/&*95:(#1&(&*,%(#$,&$/*2(8*!!!!!!!!!!!!! courtesy R. Roth render LO Beitrag (Q 0 ) Zwei-Nukleon-Kraft Drei-Nukleon-Kraft Vier-Nukleon-Kraft tur 1. NLO Ordnung (Q 2 ) Führender Beitrag tur 2. NOrdnung 2 LO (Q 3 ) Korrektur 1. Ordnung tur 3. NOrdnung 3 LO (Q 4 ) Korrektur 2. Ordnung N 4 LO (Q 5 ) Korrektur 3. Ordnung have been worked out and employed (recently, also parts of the N 5 LO NN force have been worked out ) have been worked out but not employed yet [LENPIC, work in progress]! worked out have and not been applied completely worked out out yet and to be applied calculations in progress Ulf-G. Meißner, Chiral Nuclear Dynamics SFB 634 Concl. Conf., June 2015 C < ^ O > B

12 ! $&,45*6(%&76(8/)*! Two-nucleon Zwei-Nukleon-Kraft force Three-nucleon Drei-Nukleon-Kraft force Four-nucleon Vier-Nukleon-Kraft force Effective Field Theories!!!! 16(*,$$&3&"6(/&*95:(#1&(&*,%(#$,&$/*2(8*!!!!!!!!!!!!! courtesy R. Roth render LO Beitrag (Q 0 ) Zwei-Nukleon-Kraft Drei-Nukleon-Kraft Vier-Nukleon-Kraft tur 1. NLO Ordnung (Q 2 ) Führender Beitrag tur 2. NOrdnung 2 LO (Q 3 ) Korrektur 1. Ordnung tur 3. NOrdnung 3 LO (Q 4 ) Korrektur 2. Ordnung N 4 LO (Q 5 ) Korrektur 3. Ordnung have been worked out and employed (recently, also parts of the N 5 LO NN force have been worked out ) have been worked out but not employed yet [LENPIC, work in progress]! worked out have and not been applied completely worked out out yet and to be applied calculations in progress E. Epelbaum et al, PRL 106, (2011) Ulf-G. Meißner, Chiral Nuclear Dynamics SFB 634 Concl. Conf., June 2015 C < ^ O > B

13 The Hoyle State courtesy R. Roth E. Epelbaum et al, PRL 106, (2011)

14 The Hoyle State ( the holy grail)

15 The Hoyle State ( the holy grail)

16 BB The Hoyle State ( the holy grail)

17 The Hoyle State ( the holy grail) BB stellar burning

18 The Hoyle State courtesy R. Roth

19 Ab initio Nuclear Structure courtesy R. Roth

20 Ab initio Nuclear Structure courtesy R. Roth

21 The PHASES: second constraint Jens Rydén It s always just water Corgi Lane ryandury

22 The PHASES: second constraint Each PHASE can exist in a variety of states. Each STATE is characterized by defined properties The EOS summarizes the physically possible combination of states. PV = nrt

23 The PHASES: second constraint It s always just nuclear matter CERN NASA SciencePhotoLibrary

24 The PHASES: second constraint It s always just nuclear matter

25 The PHASES: second constraint Modern nuclear physics is about... Unravelling the phases of nuclear matter LRP Nuclear Science Advisory Committee(2008)

26 The Equation of State of Nuclear Matter SciencePhotoLibrary A heavy nucleus (like 208 Pb) is 18 orders of magnitude smaller and 55 orders of magnitude lighter than a neutron star Yet bounded by the same EOS NASA

27 18-OM smaller 55-OM lighter same EOS symmetry energy

28 18-OM smaller 55-OM lighter same EOS symmetry energy slope parameter curvature parameter

29 18-OM smaller 55-OM lighter same EOS symmetry energy slope parameter curvature parameter

30 18-OM smaller 55-OM lighter same EOS symmetry energy X. Roca-Maza, at al. Phys. Rev. Lett. 106, (2011) slope parameter 0.3 Linear Fit, r = Nonrelativistic models Relativistic models NL3* NL3 PK1 NL-SV2 TM1 NL2 NL1 r np (fm) SkM* FSUGold DD-ME1 DD-ME2 SkMP SkSM* SIV MSL0 MSkA Ska DD-PC1 PK1.s24 Sk-T4 NL3.s25 Sk-Rs RHF-PKO3 G2 SkI2 RHF-PKA1 SV Sk-Gs SkI5 G1 NL-RA1 PC-F1 NL-SH PC-PK1 curvature parameter 0.15 HFB-8 MSk7 v090 SkP SkX Sk-T6 HFB-17 SGII D1N SLy5 SLy4 BCP D1S L (MeV)

31 One example Nuclear charge radii Where do the neutrons go?

32 One example Where do the neutrons go? Pressure forces neutrons out against surface tension EOS

33 One example Where do the neutrons go? Pressure forces neutrons out against surface tension EOS

34 One example Pressure forces neutrons out against surface tension Measures how much neutrons stick out past protons Constrains the pressure of neutron low ρ. i.e. calibrate the EOS of neutron rich matter...

35 The most neutron rich matter in the Universe Neutron skins constraint the EOS ρ] of... Mass 1.4 M Diameter: 20 km Density: kg/m 3 Surface gravity: higher Escape velocity: 0.6c Rotation rate: few to many times per second Magnetic field: Earth's! low ρ Crust thickness

36 The most neutron rich matter in the Universe Find a [NS + White Dwarf] Binary DPSR J

37 The most neutron rich matter in the Universe Find a [NS + White Dwarf] Binary Measure the delay in pulse arrival PB Demorest et al. Nature 467, (2010)

38 The most neutron rich matter in the Universe Find a [NS + White Dwarf] Binary Measure the delay in pulse arrival Determine the mass of the NS M = 1.97± 0.04 M PB Demorest et al. Nature 467, (2010)

39 The most neutron rich matter in the Universe Find a [NS + White Dwarf] Binary Measure the delay in pulse arrival Determine the mass of the NS M = 1.97± 0.04 M PB Demorest et al. Nature 467, (2010)

40 The most neutron rich matter in the Universe Find a [NS + White Dwarf] Binary Measure the delay in pulse arrival Determine the mass of the NS M = 1.97± 0.04 M PB Demorest et al. Nature 467, (2010) J needs enough pressure in the core to support its mass against collapse into a black hole.

41 The most neutron rich matter in the Universe Find a [NS + White Dwarf] Binary Measure the delay in pulse arrival Determine the mass of the NS M = 1.97± 0.04 M PB Demorest et al. Nature 467, (2010) J needs enough pressure in the core to support its mass against collapse into a black hole.

42 The most neutron rich matter in the Universe Find a [NS + White Dwarf] Binary Measure the delay in pulse arrival Determine the mass of the NS M = 1.97± 0.04 M PB Demorest et al. Nature 467, (2010) J needs enough pressure in the core to support its mass against collapse into a black hole. All soft EOS are ruled out!

43 M-R Curve for NS and EOS Measure the mass, assume the radius MR curve and NS matter EOS related by GR hydrostatic equation Tolman-Oppenheimer-Volkoff =GR Hydrostatic Eq. (TOV) Eq. dp dr = G /c 2 P /c 2 M 4 r 3 P / c 2 r 2 1 2GM /rc 2 dm dr =4 r2 /c 2, P=P EOS E/A EOS prediction Mass (M) Observation ρ 0 2ρ 0 Density(ρ B ) Judge Radius (R) MR relation

44 The up-to-date picture Calibrate a low density PREX/JLAB

45 The up-to-date picture Calibrate a low density J with EFT does the rest

46 Trivial? It is a long winding road Calibrate a low density CAUTION NEUTRON SKIN AHEAD...from measurable observables to the neutron skin

47 Trivial? It is a long winding road exponential charge density ρ(r) gaussian sphere with diffuse edge radius r sin qr

48 Trivial? It is a long winding road Non-PV e-scattering Electron scattering γ exchange provides Rp through nucleus FFs PV e-scattering Electron also exchange Z, which is parity violating Primarily couples to neutron

49 Trivial? It is a long winding road...since... 2" N" N"...to measure... N"...construct... N" 2" N" N"

50 N" N" 2" low-to-moderate momentum transfer gets dilu as the uncertainty in the strange-quark contrib Most interestingly, the difference almost dis The shortest of the roads actual PREX point, lending confidence that conditions are ideal for the extraction of rn 208.F the strong correlation between the neutron rad factor is maintained up to the first diffractio q = 1.2 fm 1 in the case of 48 Ca), the CRE point lies safely within this range (figure not Measured#A PV# F w (q) Pb 48 Ca F w 10 SV-min FSUGold PREX qcrex q(fm -1 ) Cr n,fw in 208 Pb PHYSICAL REVIEW C88, (2013) (a) SV-min FSU PREX-II PREX-II SV-min no s with s 0.6 (b) q (fm -1 ) FIG. 4. (Color online) Correlation coefficient (9) between rn 208 and F 208 (q) as a function of the momentum transfer q.panel(a)shows W N" N" N" 2" N" IV. CONCLUSIONS AND OUTLO Correct#for#Coulomb# DistorAons # In this survey, we have studied the potent proposed PREX-II and CREX measurements the isovector sector of the nuclear EDF. I explored correlations between the weak-cha of both 48 Ca and 208 Pb, and a variety of obse Weak#density#at#one#Q 2# to the symmetry energy. We wish to emphas chosen the weak-charge form factor rather th quantities such as the weak-charge (or ne Small#correcAons#for # ###############MEC# since F W is directly accessed by experiment. T tions among observables, two different appro implemented. In both cases we relied exclus that were accurately calibrated to a variety of g onneutron#density#at#one#q finite nuclei. In the trend analysis, 2# the p optimal model were adjusted in order to syste the symmetry energy, and the resulting im observables was monitored. In the covarian Assume#surface#thickness# good#to#25%#(mft)# obtained correlation coefficients by relying ex covariance (or error) matrix that was obtaine of model optimization. From such combined the following: (i) We verified that the neutron skin of fundamental R link to the equation of stat matter. The n# landmark PREX experim very small systematic error on rn 208 th reaching the total error of ±0.06 fm PREX-II is realistic.

51 SCALES of NM QCD-based description of nuclear structure is within reach Complementary experimental approaches will provide stringent test for actual theories PHASES of NM Phase diagram of QCD accessible by different finite density: from the Lab to the star On the wedge of turning qualitative insight into quantitative understanding