Nuclear Astrophysics
à Nuclear physics plays a special role in astronomy Nuclear structure: the DNA of chemical evolu on (Woosley) Nuclear structure The composi on of the solar system ) 6 Abundance (Si = 10
Element number (Z)
The DNA of the cosmos
Dillmann et al. 2003
Basic ques ons in Nuclear Astrophysics:
1. What is the origin of the elements E0102 (SMC) - origin of elements in our solar composi on SNR 0103-72.6 - Understanding composi onal fingerprints of astrophysical events - Understanding composi onal effects in stars, supernovae, neutron stars
2. How do stars and stellar explosions generate energy - Understand photon, neutrino emission - Understand how stars explode Supernova Ar st’s view
3. What is the nature of neutron stars
Neutron Star Ar st’s view
JINA a NSF Physics Fron ers Center – www.jinaweb.org • Iden fy and address the cri cal open ques ons and needs of the field • Form an intellectual center for the field • Overcome boundaries between astrophysics and nuclear physics and between theory and experiment • A ract and educate young people
Nuclear Physics Experiments Astronomical Observations
Astrophysical Models Associated: Nuclear Theory ANL, ASU, Princeton Core ins tu ons: 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)]
Ques on 3 How were the elements from iron to uranium made ?
à “Old problems” S ll unsolved !!! Summary
of the 2012 Nuclear Astrophysics Town Mee ng October 9-10, 2012 at the Wes n, Detroit Metro Airport
Organized by the Sponsors: Joint Ins tute for Nuclear Astrophysics • JINA • Na onal Superconduc ng 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 Mee ng
Twi er Feed Follow: @NucAstroTown12
• 150 Par cipants 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 Facili es Mul -messenger GAIA Observa ons DIANA
KEPLER à Neutrinos à Luminosity
à How do stars mix, rotate, and LENA, HIgS, StAna generate magne c 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 func on of metallicity? Theory: à A new process? i-process • 3D Modeling • Nuclear cross sec on à What is the sun’s metallicity? extrapola on Big Theme: • Valida on Woodward Pre-solar grains Core Collapse Supernovae
Mul -messenger Observa ons Accelerator Facili es 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 - Realis c progenitors SDSS/APOGEE Telescope Nuclear Theory AEGIS - ν-oscilla ons LAMOST Hammer, understand & implement Janka, Mueller GAIA - EOS GALAH VLT, HST, Subaru, … - r-process nuclei HST, VLT, Subaru, PTF
Novae and Ia Supernovae
Accelerator Facili es à What are the progenitors of type Ia? FRIB à What phenomena occur on accre ng white dwarfs? Novae, type Ia, … ? Mul -messenger à Nucleosynthesis contribu on? Observa ons à White dwarf masses of Novae? (LSST) NUSTAR TRIUMF For weak rates also FAIR/RIBF RCNP, TU Tandem LENA, StAna, ATLAS, … à SNIa radioac vity Astro Theory: ASTRO-H - Use nucleosynthesis Pakmor et al. as probe of igni on LSST and progenitors - Realis c progenitors GMT, JWST - Mul -D models PTF IRTF, VLT, Gemini, Subaru Nuclear Theory à New types of explosions à SN Ia composi on (also IR !) - Electron capture rates Neutron stars
Mul -messenger Accelerator Facili es Observa ons à What are the proper es of cold dense ma er? What is its maximum density? FRIB à How can we determine Radii, M&R, crust proper es from observa ons? LIGO à What powers superbursts? à Origin of burst oscilla ons? LOFT à Are NS Mergers GRBs? r-process site? TRIUMF EOS: FRIB,RIBF,FAIR NICER X-rays à thermal Astro Theory: à radii - Realis c 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 Evolu on
High z Observa ons Nuclear physics: à What is the chemical evolu on of JWST For reliable predic ons 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 Observa ons Astro Theory: SDSS/APOGEE Giant Magellan - Nucleosynthesis of AEGIS Telescope first stars LAMOST - Be er GCE models GAIA - Nucleosynthesis grids GALAH - Chemistry/Opaci es Turk, Abel, O’Shea VLT, HST, Subaru, … at high density Summary
Observatories: Accelerators: Key point: mul messenger Unique capabili es of FRIB Op cal: Giant Magellan Telescope, • In many presenta ons, 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 reac on 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
Compu ng/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 compu ng mul -disciplinary approaches - Open source needed for the future - Make nuclear theory progress - Voice for the field applicable to astrophysics