Nuclear Astrophysics

à Nuclear physics plays a special role in astronomy Nuclear structure: the DNA of chemical evoluon (Woosley) Nuclear structure The composion of the solar system ) 6 Abundance (Si = 10

Element number (Z)

The DNA of the cosmos

Dillmann et al. 2003

Basic quesons in Nuclear Astrophysics:

1. What is the origin of the elements E0102 (SMC) - origin of elements in our solar composion SNR 0103-72.6 - Understanding composional fingerprints of astrophysical events - Understanding composional effects in stars, supernovae, neutron stars

2. How do stars and stellar explosions generate energy - Understand photon, neutrino emission - Understand how stars explode Supernova Arst’s view

3. What is the nature of neutron stars

Neutron Star Arst’s view

JINA a NSF Physics Froners Center – www.jinaweb.org • Idenfy and address the crical open quesons and needs of the field • Form an intellectual center for the field • Overcome boundaries between astrophysics and nuclear physics and between theory and experiment • Aract and educate young people

Nuclear Physics Experiments Astronomical Observations

Astrophysical Models Associated: Nuclear Theory ANL, ASU, Princeton Core instuons: UCSB, UCSC, WMU • Notre Dame LANL, Victoria (Canada), • MSU EMMI (Germany), • U. of Chicago INPP Ohio, Minnesota Munich Cluster (Germany), http://www.jinaweb.org MoCA Monash (Australia) X-ray burst (RXTE) Supernova (Chandra,HST,..) 4U1728-34 331 Mass known 330 Half-life known nothing known 329 p process

Frequency (Hz) 328 s-process E0102-72.3 327 10 15 20 Time (s) r process Nova (Chandra) νp-process

V382 Vel Ne EC Metal poor halo star (Keck, HST) CS22892-052 1 solar r abundance observed

0

10 20 30 Wavelength ( ) Α abundance -1 n-Star (Chandra) KS 1731-260 -2 stellar burning 40 50 60 70 80 90 Z protonsBig Bang Crust and finally: processes neutrons ν-process Cosmic Rays Based on National Academy of Science Report

[Committee for the Physics of the Universe (CPU)]

Queson 3 How were the elements from iron to uranium made ?

à “Old problems” Sll unsolved !!! Summary

of the 2012 Nuclear Astrophysics Town Meeng October 9-10, 2012 at the Wesn, Detroit Metro Airport

Organized by the Sponsors: Joint Instute for Nuclear Astrophysics • JINA • Naonal Superconducng Cyclotron Lab Local Organizers: at Michigan State University • Hendrik Schatz • European Physical Journal • Sheila Balliet-Miles • Linna Leslie • Zach Meisel • Fernando Montes • Artemis Spyrou • Chris Wrede Disclaimer: - Opinions of community, not of JINA - Preliminary and incomplete; working groups not finished, personal impressions Town Meeng

Twier Feed Follow: @NucAstroTown12

• 150 Parcipants from Nuclear Physics, Astrophysics, and Astronomy • 22 Plenary Talks, 13 2h working groups Goals: Generate a white paper with vision of the field in light of NP2010, ASTRO2010, .. (previous nuclear astrophysics white paper from 1999) Stars

SNO+ Accelerator Facilies Mul-messenger GAIA Observaons DIANA

KEPLER à Neutrinos à Luminosity

à How do stars mix, rotate, and LENA, HIgS, StAna generate magnec fields? LANSCE, FRANZ, nTOF à Seismology àWhich stars go supernova? FRIB, CARIBU Samples of stars Structure before it explodes? àWhat are the elements stars make? Stardust As a funcon of metallicity? Theory: à A new process? i-process • 3D Modeling • Nuclear cross secon à What is the sun’s metallicity? extrapolaon Big Theme: • Validaon Woodward Pre-solar grains Core Collapse Supernovae

Mul-messenger Observaons Accelerator Facilies LIGO à Grav. Waves FRIB

àNeutrinos à What is the supernova mechanism? CARIBU, TRIUMF à What is the ν and grav. wave signal? RIBF, FAIR à What are the sites of the r-processes? NOVA The LEPP process? SuperK, HALO, SNO+, … à Which stars go supernova? GRB? Astro Theory: - Full 3D models à Elements in Stars Giant Magellan - Realisc progenitors SDSS/APOGEE Telescope Nuclear Theory AEGIS - ν-oscillaons LAMOST Hammer, understand & implement Janka, Mueller GAIA - EOS GALAH VLT, HST, Subaru, … - r-process nuclei HST, VLT, Subaru, PTF

Novae and Ia Supernovae

Accelerator Facilies à What are the progenitors of type Ia? FRIB à What phenomena occur on accreng white dwarfs? Novae, type Ia, … ? Mul-messenger à Nucleosynthesis contribuon? Observaons à White dwarf masses of Novae? (LSST) NUSTAR TRIUMF For weak rates also FAIR/RIBF RCNP, TU Tandem LENA, StAna, ATLAS, … à SNIa radioacvity Astro Theory: ASTRO-H - Use nucleosynthesis Pakmor et al. as probe of ignion LSST and progenitors - Realisc progenitors GMT, JWST - Mul-D models PTF IRTF, VLT, Gemini, Subaru Nuclear Theory à New types of explosions à SN Ia composion (also IR !) - Electron capture rates Neutron stars

Mul-messenger Accelerator Facilies Observaons à What are the properes of cold dense maer? What is its maximum density? FRIB à How can we determine Radii, M&R, crust properes from observaons? LIGO à What powers superbursts? à Origin of burst oscillaons? LOFT à Are NS Mergers GRBs? r-process site? TRIUMF EOS: FRIB,RIBF,FAIR NICER X-rays à thermal Astro Theory: à radii - Realisc NS mergers ASTROSAT - 2D/3D X-ray bursts RXTE, XMM, Chandra, Swi, ASTROSAT - X-ray burst templates INTEGRAL, MINBAR archive For parameter range Green Bank - Crust models Nuclear Theory - Crust nuclear physics Radio - EOS constraints ASTROSAT Square Km Array à pulsars, masses (symmetry energy) Big Bang, First Stars, and Chemical Evoluon

High z Observaons Nuclear physics: à What is the chemical evoluon of JWST For reliable predicons of Li, F, Ti, 15N, O-Na, r-process ? nucleosynthesis yields of: à What are the first stars like? - First stars, other stars à How did dwarf galaxies evolve? - Ia Supernovae à 6 Big Bang: Is there primordial Li? - Core collapse Supernovae search for signatures beyond SBB - Low mass stars - Neurton star mergers

Near field Observaons Astro Theory: SDSS/APOGEE Giant Magellan - Nucleosynthesis of AEGIS Telescope first stars LAMOST - Beer GCE models GAIA - Nucleosynthesis grids GALAH - Chemistry/Opacies Turk, Abel, O’Shea VLT, HST, Subaru, … at high density Summary

Observatories: Accelerators: Key point: mul messenger Unique capabilies of FRIB Opcal: Giant Magellan Telescope, • In many presentaons, very broad spectrograph impact UV spectroscopy capability • FRIB + SECAR only real chance X-ray Next Gen.: LOFT, … for a major step in measurements γ-ray: NUSTAR, next γ-ray telescope? of reacon rates on unstable nuclei Radio: GBT, Square Kilometer Array Mul beam: GW: LIGO – GW networks [Underground] stable beams (DIANA), γ-beams, IR: IRTF neutron beams, ν-beams ν-detectors

Compung/Theory: Centers: Need for centers (JINA) Mul-D is path forward across field - Connect subfields – data exchange - People to adapt codes so they - Enable mul-messenger, mul-beam can run at forefront of compung mul-disciplinary approaches - Open source needed for the future - Make nuclear theory progress - Voice for the field applicable to astrophysics