OLLI: the Birth, Life, and Death Of

The Birth, Life, and Death of Stars

The Osher Lifelong Learning Institute Florida State University Jorge Piekarewicz Department of Physics [email protected] Schedule: September 29 – November 3 Time: 11:30am – 1:30pm Location: Pepper Center, Broad Auditorium

J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 1 / 17 Ten Compelling Questions What is the raw material for making stars and where did it come from? What forces of nature contribute to energy generation in stars? How and where did the chemical elements form? ? How long do stars live? How will our Sun die? How do massive stars explode? ? What are the remnants of such stellar explosions? What prevents all stars from dying as black holes? What is the minimum mass of a black hole? ? What is role of FSU researchers in answering these questions?

J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 2 / 17 A Star is Born The Universe was created about 13.7 billion years ago (Big Bang!) H, He, and traces of light elements formed 3 minutes after the Big Bang (BBN) Stars and galaxies form from H and He clouds about 1 billion years after BB In stellar nurseries molecular clouds convert gravitational energy into thermal energy At about 10 million K protons overcome their Coulomb repulsion and fuse (pp chain) + p + p → d + e + νe p + d → 3He + γ 3He + 3He → 4He + p + p

ALL (gravity, strong, electroweak) interactions critical to achieve stardom Thermonuclear fusion halts the gravitational collapse Stellar evolution continues through several thermonuclear stages

J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 3 / 17 Stellar Nucleosynthesis Stars are incredibly efﬁcient thermonuclear furnaces After H-burning terminates the stellar core contracts Gravitational energy is transformed into thermal energy The heavier He-ashes (with a larger Z) can now fuse Thermonuclear fusion continues until the formation of an Iron core Thermonuclear fusion terminates abruptly: Supernova! Every C in our cells, O in the air, and Fe in our blood was made in stars We all truly are “star stuff”...Carl Sagan

J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 4 / 17 Death of a Star — Birth of a Pulsar: Core-Collapse Supernova

Massive stars create all chemical elements: from 6Li to 56Fe Once 56Fe is produced the stellar core collapses Core overshoots and rebounds: Core-Collapse Supernova! 99% of the gravitational energy radiated in neutrinos An incredibly dense object is left behind: A neutron star or a black hole

Neutron stars are solar mass objects with 10 km radii Core collapse mechanism and r-process site remain uncertain!

J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 5 / 17 Some Historical Facts Chandrasekhar shows that massive stars will collapse (1931) Chadwick discovers the neutron (1932) ... predicted earlier by Ettore Majorana but never published! Baade and Zwicky introduce the concept of neutron stars (1933) Oppenheimer-Volkoff compute masses of neutron stars using GR (1939) Predict M? '0.7 M as maximum NS mass or minimum black hole mass Jocelyn Bell discovers pulsars (1967) Gold and Pacini propose basic lighthouse model (1968) Pulsars are rapidly rotating Neutron Stars!

J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 6 / 17 S. Chandrasekhar and X-Ray Chandra White dwarfs resist gravitational collapse through electron degeneracy pressure rather than thermal pressure (Dirac and R.H. Fowler 1926) During his travel to graduate school at Cambridge under Fowler, Chandra works out the physics of the relativistic degenerate electron gas in white dwarf stars (at the age of 19!)

For masses in excess of M =1.4 M electrons becomes relativistic and the degeneracy pressure is insufﬁcient to balance the star’s gravitational attraction (P ∼n5/3 →n4/3) “For a star of small mass the white-dwarf stage is an initial step towards complete extinction. A star of large mass cannot pass into the white-dwarf stage and one is left speculating on other possibilities” (S. Chandrasekhar 1931) Arthur Eddington (1919 bending of light) publicly ridiculed Chandra’s on his discovery Awarded the Nobel Prize in Physics (in 1983 with W.A. Fowler) In 1999, NASA lunches “Chandra” the premier USA X-ray observatory

J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 7 / 17 Jocelyn Bell Worked with Anthony Hewish on constructing a radio telescope to study quasars In 1967 as a graduate student (at the age of 24!) detected a bit of “scruff”

The Sounds of Pulsars Jocelyn Bell discovers amazing regularity in the radio signals( P =1.33730119 s) Speculated that the signal might be from another civilization (LGM-1) Paper announcing the ﬁrst pulsar published in Nature (February 1968) A Hewish, S J Bell, J D H Pilkington, P F Scott, R A Collins Antony Hewish and Martin Ryle awarded the Nobel Prize in Physics in 1974 The “No-Bell” roundly condemned by many astronomers (Fred Hoyle) “I believe it would demean Nobel Prizes if they were awarded to research students, except in very exceptional cases, and I do not believe this is one of them”

J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 8 / 17 Jocelyn Bell Worked with Anthony Hewish on constructing a radio telescope to study quasars In 1967 as a graduate student (at the age of 24!) detected a bit of “scruff”

J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 8 / 17 Biography of a Neutron Star: The Crab Pulsar SN 1054 ﬁrst observed as a new “star” in the sky on July 4, 1054 Event recorded in multiple Chinese and Japanese documents Event also recorded by Anasazi residents of Chaco Canyon, NM Crab nebula and pulsar became the SN remnants Name: PSR B0531+21 Distance: 6,500 ly POB: Taurus Temperature: 106 K 14 3 Mass: 1.4 M Density: 10 g/cm Radius: 10 km Pressure: 1029 atm Period: 33 ms Magnetic Field: 1012 G

J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 9 / 17 A Grand Challenge: How does subatomic matter organize itself? “Nuclear Physics: Exploring the Heart of Matter” (2010 Committee on the Assessment and Outlook for Nuclear Physics) Consider A nucleons and Z electrons in a ﬁxed volume V at T ≡0 ... cold fully catalyzed matter in thermal and chemical equilibrium Enforce charge neutrality protons = electrons + muons Enforce chemical (i.e., beta) equilibrium: n→p+e− +¯ν; p+e− →n+ν

Impossible to answer such a question under normal laboratory conditions — as such a system is in general unbound!

J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 10 / 17 Gravitationally Bound Neutron Stars as Physics Gold Mines Neutron Stars are bound by gravity NOT by the strong force Neutron Stars satisfy the Tolman-Oppenheimer-Volkoff equation GR extension of Newtonian gravity: vesc/c ∼ 1/2 Only Physics sensitive to is: Equation of State EOS must span 10-11 orders of magnitude in baryon density

Increase from 0.7→2M must be explained byLETTER NuclearRESEARCH Physics!

Received 7 July;dM accepted 1 September 2010. MS0 2 2.5 GR MPA1 = 4πr E(r) ∞ AP3 1. Lattimer, J. M. & Prakash, M. The physics of neutron stars. Science 304, 536–542 < PAL1 P ENG (2004). dr AP4 MS2 2. Lattimer, J. M. & Prakash, M. Neutron star observations: prognosis for equation of Causality state constraints.dP Phys. Rep. 442, 109–165E(r (2007).)M(r) P(r) 2.0 J1614-2230 3. Glendenning, N. K. &= Schaffner-Bielich,−G 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 hyperonsE in (r) )

( SQM1 PAL6 GM3 neutron stars. Phys. Rev. D 73, 024021 (2006). 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).4πr 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(E) pulsarrelation Rotation distance, a high pulsar mass, and a limit on the variation of Newton’s gravitational constant. Astrophys. J. 679, 675–680 (2008). 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 FigureJ. Piekarewicz 3 | Neutron star mass–radius (FSU-Physics) diagram. The plot shows non-rotatingThe Birth, Life,J1614 and22230: Death linking of quantum Stars chromodynamics, gamma-ray bursts, and Fall 2014 11 / 17 mass versus physical radius for several typical EOSs27: blue, nucleons; pink, gravitational wave astronomy. Astrophys. J. (in the press). nucleons plus exotic matter; green, strange quark matter. The horizontal bands 13. Hobbs, G. B., Edwards, R. T. & Manchester, R. N. TEMPO2, a new pulsar-timing package - I. An overview. Mon. Not. R. Astron. Soc. 369, 655–672 (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 measurements for two other millisecond pulsars systems. II. The post-Newtonian timing formula. Ann. Inst. Henri Poincare´ Phys. and the range of observed masses for double neutron star binaries2. Any EOS The´or. 44, 263–292 (1986). line that does not intersect the J1614-2230 band is ruled out by this 15. Freire, P. C. C. & Wex, N. The orthometric parameterisation of the Shapiro 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). 16. Iben, 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. solar mass of material, and result in a mildly recycled pulsar23, that is one with a spin period .8 ms. A few models resulting in orbital para- Acknowledgements P.B.D. is a Jansky Fellow of the National Radio Astronomy 23,24 Observatory. J.W.T.H. is a Veni Fellow of The Netherlands Organisation for Scientific meters similar to those of J1614-2230 predict that the neutron star Research. We thank J. Lattimer for providing the EOS data plotted in Fig. 3, and P. Freire, ¨ could accrete up to 0.2M[, which is still significantly less than the F. Ozel and D. Psaltis for discussions. The National Radio Astronomy Observatory is a >0.6M needed to bring a neutron star formed at 1.4M up to the facility of the US National Science Foundation, operated under cooperative agreement [ [ by Associated Universities, Inc. observed mass of J1614-2230. A possible explanation is that some neutron stars are formed massive (,1.9M ). Alternatively, the trans- Author Contributions All authors contributed to collecting data, discussed the results [ and edited the manuscript. In addition, P.B.D. developed the MCMC code, reduced and fer of mass from the companion may be more efficient than current analysed data, and wrote the manuscript. T.P. wrote the observing proposal and models predict. This suggests that systems with shorter initial orbital created Fig. 3. J.W.T.H. originally discovered the pulsar. M.S.E.R. initiated the survey that periods and lower companion masses—those that produce the vast found the pulsar. S.M.R. initiated the high-precision timing proposal. majority of the fully recycled millisecond pulsar population23—may Author Information Reprints and permissions information is available at experience even greater amounts of mass transfer. In either case, our www.nature.com/reprints. The authors declare no competing financial interests. Readers are welcome to comment on the online version of this article at mass measurement for J1614-2230 suggests that many other milli- www.nature.com/nature. Correspondence and requests for materials should be second pulsars may also have masses much greater than 1.4M[. addressed to P.B.D. ([email protected]).

28 OCTOBER 2010 | VOL 467 | NATURE | 1083 ©2010 Macmillan Publishers Limited. All rights reserved The Anatomy of a Neutron Star Atmosphere (10 cm): Shape of Thermal Radiation( L=4πσR2T 4) Envelope (100 m): Huge Temperature Gradient (108K ↔106K ) Outer Crust (400 m): Coulomb crystal of exotic neutron-rich nuclei Inner Crust (1 km): Coulomb frustrated “Nuclear Pasta” Outer Core (10 km): Neutron-rich uniform matter( n, p, e, µ) Inner Core (?): Exotic matter (Hyperons, condensates, quark matter, ...)

J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 12 / 17 −10 −3 14 3 The Outer Crust: 10 ρ0 . ρ . 10 ρ0 (ρ0 ≈2.4×10 g/cm ) Uniform nuclear matter unstable against cluster formation Coulomb Crystal of neutron-rich nuclei immersed in e− Fermi gas Nuclear Crystallography: Dynamics driven by nuclear masses 4/3 E/Atot = M(N, Z)/A + 3/4Ye kFermi + ... bcc Crystal of neutron-rich nuclei immersed in a uniform e− gas 56 62 86 78 124 118 Fe, Ni =⇒ Kr,..., Ni,... =⇒ Mo,..., 36 Kr82(?) N=50 N=82 High-precision mass measurements of exotic unstable nuclei essential 82 ISOLTRAP@CERN: The case of 30Zn52 with a 150 ns half-life!

I NTERNATIONAL JOURNAL OF HIGH-ENERGY PHYSICS CERNCOURIER

WELCOME V OLUME 53 NUMBER 3 A PRIL 2013 CERN Courier – digital edition Welcome to the digital edition of the April 2013 issue of CERN Courier.

Supernova explosions provide a natural laboratory for some interesting nuclear and particle physics, not least when they leave behind neutron stars, the densest known objects in the cosmos. Conversely, experiments ISOLTRAP casts light in physics laboratories can cast light on the nature of neutron stars, just as the ISOLTRAP collaboration is doing at CERN’s ISOLDE facility, as this on neutron stars month’s cover feature describes. Elsewhere at CERN, the long shutdown of the accelerators has begun and a big effort on maintenance and consolidation has started, not only on the LHC but also at the experiments. At Point 5, work is underway to prepare the CMS detector for the expected improvements to the collider. Meanwhile, the Worldwide LHC Computing Grid continues to provide high-performance computing for the experiments 24 hours a day, while it too undergoes a continual process of improvement.

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SN BOSE EXPERIMENTS COMPUTING Kolkata honours How CMS is a great Indian preparing for AT THE LHC EDITOR: CHRISTINE SUTTON, CERN physicist the future Work never stops for DIGITAL EDITION CREATED BY JESSE KARJALAINEN/IOP PUBLISHING, UK p35 p16 the WLCG p21 J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 13 / 17 CERNCOURIER WWW. V OLUME 53 NUMBER 3 A PRIL 2013 The Inner Crust: “Coulomb Frustration and Nuclear Pasta” Frustration emerges from a dynamical (or geometrical) competition Impossibility to simultaneously minimize all elementary interactions Emergence of a multitude of competing (quasi) ground states Universal in complex systems (nuclei, e− systems, magnets, proteins,...) Emergence of fascinating topological shapes “Nuclear Pasta” or “Micro-emulsions" “In 2D-electron systems with Coulomb interactions, a direct transition from a liquid to a crystalline state is forbidden” (Spivak-Kivelson) How do we taste or smell the nuclear pasta?

Coulomb frustration is a fundamental problem in condensed-matter physics with widespread implications in nuclear physics and astrophysics!

J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 14 / 17 The Outer/Inner Core: “Heaven and Earth” Structurally the most important component of the star 90% of the size and all of the mass reside in the core Outer Core: Uniform neutron-rich matter in chemical equilibrium Neutrons, protons, electrons, and muons Inner Core(?): “QCD made simple (color-ﬂavor locking)” Hyperons, meson condensates, color superconductors, ??? Same pressure creates neutron skin and NStar radius Correlation among observables differing by 18 orders of magnitude!

PREX is a fascinating experiment that uses parity violation to accurately determine the neutron radius in 208Pb. This has broad applications to astrophysics, nuclear structure, atomic parity non- conservation and tests of the standard model. The conference will begin with introductory lectures and we encourage new comers to attend. For more information contact [email protected]

Topics Organizing Committee Parity Violation Chuck Horowitz (Indiana) Theoretical descriptions of neutron-rich nuclei and bulk matter Kees de Jager (JLAB) Laboratory measurements of neutron-rich nuclei Jim Lattimer (Stony Brook) and bulk matter Witold Nazarewicz (UTK, ORNL) Neutron-rich matter in Compact Stars / Astrophysics Jorge Piekarewicz (FSU Website: http://conferences.jlab.org/PREX Sponsors: Jefferson Lab, JSA

J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 15 / 17 Conclusions: Neutron Stars as Physics Gold Mines Astrophysics: What is the minimum mass of a black hole? Atomic Physics: Pure neutron matter as a unitary Fermi gas Condensed-Matter Physics: Insights into Coulomb frustration General Relativity: Neutrons stars as a source of gravitational waves Nuclear Physics: What is the equation of state of dense matter? Particle Physics: Quark matter and color superconductors quark matter

It is all connected ...

J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 16 / 17 Ten Compelling Questions What is the raw material for making stars and where did it come from? Hydrogen and Helium originated in the Big Bang What forces of nature contribute to energy generation in stars? All four: Gravitational, Electromagnetic, Strong, and Weak How and where did the chemical elements form? ? Thermonuclear fusion in the hot stellar interior How long do stars live? The lifetime of the star depends exclusively on its mass How will our Sun die? Our Sun will die as a white-dwarf star in about 5 billion years How do massive stars explode? ? Massive stars explode as spectacular Supernova What are the remnants of such stellar explosions? Black holes or neutron stars What prevents all stars from dying as black holes? A subtle quantum mechanical effect called Pauli pressure What is the minimum mass of a black hole? ? Approximately three times the mass of our Sun

J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 17 / 17 Ten Compelling Questions What is the raw material for making stars and where did it come from? Hydrogen and Helium originated in the Big Bang What forces of nature contribute to energy generation in stars? All four: Gravitational, Electromagnetic, Strong, and Weak How and where did the chemical elements form? ? Thermonuclear fusion in the hot stellar interior How long do stars live? The lifetime of the star depends exclusively on its mass How will our Sun die? Our Sun will die as a white-dwarf star in about 5 billion years How do massive stars explode? ? Massive stars explode as spectacular Supernova What are the remnants of such stellar explosions? Black holes or neutron stars What prevents all stars from dying as black holes? A subtle quantum mechanical effect called Pauli pressure What is the minimum mass of a black hole? ? Approximately three times the mass of our Sun

J. Piekarewicz (FSU-Physics) The Birth, Life, and Death of Stars Fall 2014 17 / 17