H. Schatz, September 2012 X-ray bursts X-ray bursts on neutron stars: Most common thermonuclear stellar explosions
Superbursts fuel: deep C rare, hours-days Intermediate long bursts 10s of minutes - hours fuel: deep He? Longer bursts minutes fuel: H, He Short bursts 10 s fuel: He RXTE Galloway et al SLX sec INTEGRAL Falanga 08 RXTE Strohmeyer Open question: How is carbon produced? How can it ignite within a year? Longer vs shorter bursts: Can be explained with nuclear physics from RIB experiments
Open questions Multi-peaked burst rises? Nuclear waiting points? Maurer&Watts U Time (s) Many other open questions: Transition bursts stable burning with increasing accretion rate Short recurrence time bursts Multi-D effects? Burst oscillations Burst raise Spitkovsky 2002
H. Schatz, September X-ray Bursts Models and Observations Need nuclear data now to create set of model templates to analyze observations: otherwise match with wrong parameters Major progress in observations MINBAR archive ~5000 widely varying bursts Burst profiles depend on nuclear rates With accurate model templates: Absolute peak flux, distance H/He composition Redshift + color correction (distance and anisotropy independent) Neutron star compactness Amthor, Cyburt et al Zamfir et al GS Redshift variation
H. Schatz, September Composition of burst nuclear ashes as observable? Absorption edges in X-ray spectrum? Some PRE bursts might bring ashes to the surface: (Weinberg et al. 2001) NASA/Chandra/Wijnands et al. Unknown heat source was added Neutrons drip here? Superfluid? Core? Brown & Cumming 2009 MXB Brown&Cumming 2009 Observations of cooling crusts: -Burst ashes composition sets crust composition -Heating and cooling depend on composition! (Gupta et al. 2007)
Deepest zone of first burst (model zM of Woosley et al. 2007) Model by Heger, Woosley et al.; Similar to other groups: Fisker et al. and Jordi et al. Slowdown creates Burst tails
Nuclear reaction rates matter ! First sensitivity study for full 1D burst model from Heger (Cyburt, Amthor, Keek et al. ) Burst X-ray light curve Final composition of ashes (see also post-processing study by Parikh et al. 2008)
Slid 8 Hendrik Schatz NNPSS 2012, Slide 8 Mass known <10 keV Mass known <100 keV Mass uncertain, half-life known seen Ion Traps ANL, GSI Jyvaskyla Ion Traps ANL, ISOLDE, MSU ORNL -decay Nuclear Data: Decay studies of 100 Sn, 96 Cd (GSI, MSU RFFS) - Decay data - Masses - Reaction rates Stable: ( 3 He,t) Yale, TUM RIB direct ( ,p)(ANL, ORNL, LLN, CRIB…) Direct (p, ): (TRIUMF, ORNL) RIB Indirect: (p,p), ANC (ORNL) RIB Indirect (p,d )/(d,n ) MSU RIB Indirect Coul. Dis. (RIKEN, GSI) RIB indirect (d,n) FSU Stable: (p,t), ( 4 He, 6 He) (Yale, RCNP) Stable: ( 3 He,n) ND Stable: (ANL) fusion-evaporation- we are just at the beginning! ReA3 at NSCL, HELIOS at ANL, ISAC2 at TRIUMF, ESR at GSI RIBF, FAIR, FRIB, SPIRAL, … Nuc. Theory - predict rates (HF,DC) - Interpret experiments
ReA3/6 Science, Hendrik Schatz, 7/19/2012, Slide 9 Direct p-capture measurements: SECAR method successfully applied at TRIUMF/DRAGON SECAR JENSA SECAR under design (G. Berg, M. Couder) (funded by DOE Office of Science) Inspired by St. George at Notre Dame Large multi-institutional collaboration: (JINA, ANL, CSM, LSU, McMaster, MSU, ND, ORNL, PNNL) Goal: finish design in Fall 2012 Initial measurements possible at ReA3 (but need > ~10 7 pps) 22 Na(p, ), 23 Mg(p, ), 25 Al(p, ) 27 Si(p, ), 29 P(p, ), 30 P(p, ), 33 Cl(p, ) 34 Cl(p, ), 34 Ar(p, ), 37 K(p, ), 38 K(p, ) ANASEN AT-TPC Also new opportunities For indirect studies At NSCL/ReA3 and FRIB
FRIB: A Unique Opportunity FRIB only facility offering reaccelerated fragmentation RIBs H. Schatz, September Reaccelerated beams at FRIB: Unique opportunity to remove many major nuclear physics uncertainties for novae and x-ray bursts: Novae and XRBs first explosive scenarios with nuclear physics on par with stable nuclei scenarios SECAR AT-TPC ANASEN
Summary Nuclear physics in X-ray bursts needs to be understood to explain phenomena, to analyze observations, to extract NS properties Decay rates are known experimentally – need stellar corrections from theory Need additional precision mass measurements near p-drip line Challenge for the Future: Need to measure critical reaction rates -Identify critical rates in wide range of sensitivity studies -Use indirect techniques to identify key resonances and to constrain weak resonances/cross sections that cannot be measured directly (New devices: HELIOS, ANASEN, JENSA, AT-TPC, … ) -Measure critical rates directly at astrophysical energies -Build SECAR -Exploit NSCL ReA3 and develop beams at TRIUMF -Build FRIB – use reaccelerated beams -Evaluation and Dissemination Tackle problems in integrated coordinated approach: various burst types, crust, neutron star properties – nuclear, astrophysics, observations (JINA!)