Nuclear Astrophysics in the new era of multi-messenger Astronomy LIGO Detects a Neutron Star Merger Astronomy.com PRL 119, 161101 (2017) Detailed analyses of the gravitational-wave data, together with observations of electromagnetic emissions, are providing new insights into the astrophysics of compact binary systems and γ-ray bursts, dense matter under extreme conditions, the nature of gravitation, and independent tests of cosmology. National Science Foundation/LIGO/Sonoma State University/A. Simonnet Two Stars: Pele' and Cassiopeia A Jorge Piekarewicz Florida State University Outline … Neutron stars as unique cosmic laboratories Heaven and Earth: Laboratory constraints on NS Earth and Heaven: NS constrains on laboratory observables The BIG questions? The creation of the heavy elements New states of matter at low and high densities The equation of state of neutron-rich matter The Anatomy of a Neutron Star Atmosphere (10 cm): Shapes Thermal Radiation (L=4psR2T4) Envelope (100 m): Huge Temperature Gradient (108K 4106K) Outer Crust (400 m): Coulomb Crystal (Exotic neutron-rich nuclei) Inner Crust (1 km): Coulomb Frustration (“Nuclear Pasta”) Outer Core (10 km): Uniform Neutron-Rich Matter (n,p,e,µ) Inner Core (?): Exotic Matter (Hyperons, condensates, quark matter) The composition of the outer crust - as well as the r-process - is extremely sensitive to nuclear masses of exotic, neutron-rich nuclei. RIBFs will help — but only to some extent. Theory (e.g., DFT+BNN) is essential to predict the masses of nuclei that will never be measured in the laboratory The unknown EOS of the inner crust (especially in the nuclear pasta phase) is essential to understand the tidal polarizability in BNS mergers The neutron skin of lead has been identified as a proxy for the slope of the symmetry energy (“L”) which in turn largely determines the size of the neutron star — objects that differ by 18 orders of magnitude! Neutron Stars as Nuclear Physics Gold Mines Neutron Stars are the remnants of massive stellar explosions Are bound by gravity NOT by the strong force Satisfy the Tolman-Oppenheimer-Volkoff equation (v /c 1/2) esc ⇠ Only Physics sensitive to: Equation of state of neutron-rich matter EOS mustThe span Holy about Grail:11 orders The ofEquation magnitude ofin baryon density Increase fromState 0.7 of2 MNeutron-Starmust be explained Matter byLETTER NuclearRESEARCH Physics! ! Received 7 July; accepted 1 September 2010. MS0 dM 2 2.5 GR MPA1 ∞ AP3 1. Lattimer, J. M. & Prakash,= M.4 The⇡ physicsr of neutron(r) stars. Science 304, 536–542 < PAL1 P ENG (2004). dr E AP4 MS2 2. Lattimer, J. M. & Prakash, M. Neutron star observations: prognosis for equation of Causality state constraints.dP Phys. Rep. 442, 109–165(r (2007).)M(r) P(r) 2.0 J1614-2230 3. Glendenning, N. K. &= Schaffner-Bielich,G E J. Kaon condensation and1 dynamical+ SQM3 MS1 nucleons in neutron stars. Phys. Rev. Lett. 81, 4564–45672 (1998). J1903+0327 FSU 4. Lackey, B. D.,dr Nayyar, M. &− Owen, B. J. Observationalr constraints on hyperons in (r) ) ( SQM1 PAL6 GM3 neutron stars. Phys. Rev. D 73, 024021 (2006). E M 1.5 J1909-3744 5. Schulze, H., Polls, A., Ramos, A. & Vidan3 ˜a, I. Maximum mass of neutron stars. Phys. 1 GS1 − Double neutron sstar systemssy Rev. C 73, 058801 (2006).4⇡r P(r) 2GM(r) Mass ( 6. Kurkela, A., Romatschke,1 + P. & Vuorinen, A. Cold quark matter.1 Phys. Rev. D 81, 105021 (2010). 1.0 M(r) − r 7. Shapiro, I. I. Fourth test of general relativity. Phys. Rev. Lett. 13, 789–791 (1964). 8. Jacoby, B. A., Hotan, A., Bailes, M., Ord, S. & Kulkarni, S. R. The mass of a millisecond pulsar. Astrophys. J. 629, L113–L116 (2005). 0.5 9. Verbiest,Need J. P. W. et al. Precision an timing EOS: of PSR J0437–4715:P =P an accurate( ) pulsarrelation Rotation distance, a high pulsar mass, and a limit on the variation of Newton’s gravitational constant. Astrophys. J. 679, 675–680 (2008). E 10. Hessels, J. et al. in Binary Radio Pulsars (eds Rasio, F. A. & Stairs, I. H.) 395 (ASP Conf. 0.0 Ser. 328, AstronomicalNuclear Society of the Pacific, Physics 2005). Critical 7 8 9 10 11 12 13 14 15 11. Crawford, F. et al. A survey of 56 midlatitude EGRET error boxes for radio pulsars. Radius (km) Astrophys. J. 652, 1499–1507 (2006). 12. O¨ zel, F., Psaltis, D., Ransom, S., Demorest, P. & Alford, M. The massive pulsar PSR Figure 3 | Neutron star mass–radius diagram. The plot shows non-rotating J161422230: linking quantum chromodynamics, gamma-ray bursts, and mass versus physical radius for several typical EOSs27: blue, nucleons; pink, gravitational wave astronomy. Astrophys. J. (in the press). nucleonsJ. plus Piekarewicz exotic matter; green, (FSU) strange quark matter. The horizontal bands 13.Neutron Hobbs, G. Stars B., Edwards, R. T. & Manchester, R. N. TEMPO2, a newMazurian pulsar-timing Lakes 2015 4 / 15 Many nuclear models packagethat - I. Anaccurately overview. Mon. Not. R. Astron. predict Soc. 369, 655–672 the (2006). show the observational constraint from our J1614-2230 mass measurement of 14. Damour, T. & Deruelle, N. General relativistic celestial mechanics of binary 8,28 (1.97 6 0.04)M[, similar measurementsproperties for two other of millisecond finite pulsars nucleisystems. yield II. The post-Newtonianenormous timing formula. variationsAnn. Inst. Henri Poincare ´inPhys. and the range of observed masses for double neutron star binaries2. Any EOS The´or. 44, 263–292 (1986). line that does not intersectthe the J1614-2230 prediction band is ruled out of by this neutron-star15. Freire, P. C. C. radii & Wex, N. The and orthometric maximum parameterisation of the Shapiromass delay and measurement. In particular, most EOS curves involving exotic matter, such as an improved test of general relativity with binary pulsars. Mon. Not. R. Astron. Soc. kaon condensates or hyperons, tend to predict maximum masses well below (in the press). What 16.is Iben, missing? I. Jr & Tutukov, A. V. On the evolution of close binaries with components of 2.0M[ and are therefore ruled out. Including the effect of neutron star rotation initial mass between 3 solar masses and 12 solar masses. Astrophys. J Suppl. Ser. increases the maximum possible mass for each EOS. For a 3.15-ms spin period, 58, 661–710 (1985). this is a =2% correction29 and does not significantly alter our conclusions. The 17. O¨ zel, F. Soft equations of state for neutron-star matter ruled out by EXO 0748 - grey regions show parameter space that is ruled out by other theoretical or 676. Nature 441, 1115–1117 (2006). observational constraints2. GR, general relativity; P, spin period. 18. Ransom, S. M. et al. Twenty-one millisecond pulsars in Terzan 5 using the Green Bank Telescope. Science 307, 892–896 (2005). 19. Freire, P. C. C. et al. Eight new millisecond pulsars in NGC 6440 and NGC 6441. Astrophys. J. 675, 670–682 (2008). common feature of models that include the appearance of ‘exotic’ 20. Freire, P. C. C., Wolszczan, A., van den Berg, M. & Hessels, J. W. T. A massive neutron 4,5 3 star in the globular cluster M5. Astrophys. J. 679, 1433–1442 (2008). hadronic matter such as hyperons or kaon condensates at densities 21. Alford,M.etal.Astrophysics:quarkmatterincompactstars?Nature445,E7–E8(2007). of a few times the nuclear saturation density (ns), for example models 22. Lattimer, J. M. & Prakash, M. Ultimate energy density of observable cold baryonic GS1 and GM3 in Fig. 3. Almost all such EOSs are ruled out by our matter. Phys. Rev. Lett. 94, 111101 (2005). 23. Podsiadlowski, P., Rappaport, S. & Pfahl, E. D. Evolutionary sequences for low- and results. Our mass measurement does not rule out condensed quark intermediate-mass X-ray binaries. Astrophys. J. 565, 1107–1133 (2002). matter as a component of the neutron star interior6,21, but it strongly 24. Podsiadlowski, P. & Rappaport, S. Cygnus X-2: the descendant of an intermediate- constrains quark matter model parameters12. For the range of allowed mass X-Ray binary. Astrophys. J. 529, 946–951 (2000). 25. Hotan, A. W., van Straten, W. & Manchester, R. N. PSRCHIVE and PSRFITS: an open EOS lines presented in Fig. 3, typical values for the physical parameters approach to radio pulsar data storage and analysis. Publ. Astron. Soc. Aust. 21, of J1614-2230 are a central baryon density of between 2ns and 5ns and a 302–309 (2004). radius of between 11 and 15 km, which is only 2–3 times the 26. Cordes, J. M. & Lazio, T. J. W. NE2001.I. A new model for the Galactic distribution of free electrons and its fluctuations. Preprint at Æhttp://arxiv.org/abs/astro-ph/ Schwarzschild radius for a 1.97M[ star. It has been proposed that 0207156æ (2002). the Tolman VII EOS-independent analytic solution of Einstein’s 27. Lattimer, J. M. & Prakash, M. Neutron star structure and the equation of state. equations marks an upper limit on the ultimate density of observable Astrophys. J. 550, 426–442 (2001). 22 28. Champion, D. J. et al. An eccentric binary millisecond pulsar in the Galactic plane. cold matter . If this argument is correct, it follows that our mass mea- Science 320, 1309–1312 (2008). surement sets an upper limit on this maximum density of 29. Berti, E., White, F., Maniopoulou, A. & Bruni, M. Rotating neutron stars: an invariant (3.74 6 0.15) 3 1015 g cm23, or ,10n . comparison of approximate and numerical space-time models. Mon. Not. R. s Astron. Soc. 358, 923–938 (2005). Evolutionary models resulting in companion masses .0.4M[ gen- erally predict that the neutron star accretes only a few hundredths of a Supplementary Information is linked to the online version of the paper at www.nature.com/nature.