The rapid proton capture process (rp-process). Nova Cygni 1992 with HST Sites of the rp-process KS 1731-260 with Chandra E0102-73.3 composite Novae -wind.

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Presentation transcript:

The rapid proton capture process (rp-process)

Nova Cygni 1992 with HST Sites of the rp-process KS with Chandra E composite Novae -wind in supernovae ? X-ray binaries “ r”p-process (not really a full rp-process) makes maybe 26 Al makes maybe 45 Sc and 49 Ti if n accelerated ( interactions) maybe a major nucleosynthesis process? full rp-process unlikely to contribute to nucleosynthesis This lecture

D.A. Smith, M. Muno, A.M. Levine, R. Remillard, H. Bradt 2002 (RXTE All Sky Monitor) X-rays in the sky

0.5-5 keV (T=E/k=6-60 x 10 6 K) Cosmic X-rays: discovered end of 1960’s: Nobel Price in Physics 2002 for Riccardo Giacconi

Discovery First X-ray pulsar: Cen X-3 (Giacconi et al. 1971) with UHURU First X-ray burst: 3U (Grindlay et al. 1976) with ANS Today: ~50 Today: ~70 burst sources out of 160 LMXB’s Total ~230 X-ray binaries known T~ 5s 10 s H. Schatz Discovery of X-ray bursts and pulsars

Typical X-ray bursts: erg/s duration 10 s – 100s recurrence: hours-days regular or irregular Frequent and very bright phenomenon ! (stars erg/s) H. Schatz Burst characteristics

Accreting neutron stars

Neutron Star Donor Star (“normal” star) Accretion Disk The Model Neutron stars: 1.4 M o, 10 km radius (average density: ~ g/cm 3 ) Typical systems: accretion rate / M o /yr ( kg/s/cm 2 ) orbital periods days orbital separations AU’s H. Schatz The model

NASA

Energy generation: thermonuclear energy Ratio gravitation/thermonuclear ~ 30 – 40 (called  ) 4H 4 He 5 4 He + 84 H 104 Pd 6.7 MeV/u 0.6 MeV/u 6.9 MeV/u Energy generation: gravitational energy E = G M m u R = 200 MeV/u 3 4 He 12 C (“triple alpha”) (rp process) H. Schatz Energy sources

Unstable, explosive burning in bursts (release over short time) Burst energy thermonuclear Persistent flux gravitational energy H. Schatz Observation of thermonuclear energy

Burst trigger rate is “triple alpha reaction”3 4 He 12 C Ignition: d  nuc dT d  cool dT >  nuc  cool ~ T 4 Ignition < 0.4 GK: unstable runaway (increase in T increases  nuc that increases T …) degenerate e-gas helps ! Triple alpha reaction rate BUT: energy release dominated by subsequent reactions ! Nuclear energy generation rate Cooling rate H. Schatz Burst ignition

Triple alpha reaction rate at high local accretion rates m > m edd (m edd generates luminosity L edd ) Stable nuclear burning H. Schatz At large (local) accretion rates

> Gauss ! High local accretion rates due to magnetic funneling of material on small surface area H. Schatz X-ray pulsar

RXTE XMM Chandra XMM Newton RXTE Constellation X Golden Age for X-ray Astronomy ?

4U Rossi X-ray Timing Explorer Picture: T. Strohmeyer, GSFC Neutron Star spin frequency Origin of oscillations ? Why frequency drift ? Now proof from 2 bursting pulsars (SAX J , XTE J ) (Chakrabarty et al. Nature 424 (2003) 42 Strohmayer et al. ApJ 596 (2003)67) H. Schatz Open question I: ms oscillations

Seconds since burst D. Chakrabarty et al. Nature 424 (2003) 42 SAX J Pulsar Frequency H. Schatz The bursting pulsar Origin of frequency drift in normal bursting systems ??? (rotational decoupling ? Surface pulsation modes ?)

Anatoly Spitkovsky (Berkeley) H. Schatz Open question II: ignition and flame propagation

Regular burst rate /day Accretion rate (Edd units) Cornelisse et al superbursts Regular burst duration (s)     superbursts Accretion rate (Edd units) H. Schatz Open question III: burst behavior at large accretion rates

4U Normal Burst X 1000 duration ( can last ½ day) X 1000 energy 11 seen in 9 sources Recurrence ~1 yr ? Often preceeded by regular burst H. Schatz Open question IV: superbursts

Cottam, Paerels, Mendez 2002 EXO H. Schatz Open question V: abundance observations ?

Galloway et al Precision X-ray observations (NASA’s RXTE) Woosley et al astro/ph But only with precision nuclear physics Uncertain models due to nuclear physics Burst models with different nuclear physics assumptions  GS burst shape changes ! (Galloway 2003 astro/ph ) H. Schatz New era of precision astrophysics

Neutron star surface Accreted matter (ashes) Neutron star surface Fate of matter accreted onto a neutron star accretion rate: ~10 kg/s/cm 2  Accreted matter is incorporated deeper into the neutron star  As the density increases interesting things happen

Accreting Neutron Star Surface fuel ashes ocean Inner crust outer crust H,He gas core ’s X-ray’s ~1 m ~10 m ~100 m ~1 km 10 km Thermonuclear H+He burning (rp process)  X-ray bursts Deep burning ?  superbursts Crust processes (EC, pycnonuclear fusion)  crust heating  crust conductivity Spallation of heavy nuclei ? H. Schatz Nuclear physics overview

Neutron star surface ocean Inner crust outer crust H,He gas Step 1: Thermonuclear burning in atmosphere ~ 4m,  =10 6 g/cm 3 X-ray burst

depth time Kippenhahn diagram Woosley et al. 2003

Ignition layer surface ocean Ignition Burst cooling J. Fisker Thesis (Basel, 2004) H. Schatz Conditions during an X-ray burst

27 Si neutron number 13 Proton number 14 (p,  ) ( ,p) (,)(,) (,   ) Lines = Flow = H. Schatz Visualizing reaction networks

Burst Ignition: Prior to ignition : hot CNO cycle ~0.20 GK Ignition : 3  : Hot CNO cycle II ~ 0.68 GK breakout 1: 15 O(  ) ~0.77 GK breakout 2: 18 Ne( ,p) (~50 ms after breakout 1) Leads to rp process and main energy production

N=41 38 (Sr) 39 (Y) 40 (Zr) 41 (Nb) 42 (Mo) 43 (Tc) Z Proton number Nuclear lifetimes: (average time between a …) A+p  B+  proton capture :  = 1/(Y p  N A )   decay :  = T 1/2 /ln2 B+   A+p photodisintegration :  = 1/  p  (for  =10 6 g/cm 3, Yp=0.7, T=1.5 GK) H. Schatz How the rp-process works  Endpoint ?

Possibilities: Cycling (reactions that go back to lighter nuclei) Coulomb barrier Runs out of fuel Fast cooling Possibilities: Cycling (reactions that go back to lighter nuclei) Coulomb barrier Runs out of fuel Fast cooling Proton capture lifetime of nuclei near the drip line Event timescale H. Schatz The endpoint of the rp-process

Slow reactions  extend energy generation  abundance accumulation (steady flow approximation Y=const or Y ~ 1/ ) Critical “wating points” can be easily identified in abundance movie H. Schatz Waiting points

The Sn-Sb-Te cycle Known ground state  emitter Endpoint: Limiting factor I – SnSbTe Cycle Collaborators: L. Bildsten (UCSB) A. Cumming (UCSC) M. Ouellette (MSU) T. Rauscher (Basel) F.-K. Thielemann (Basel) M. Wiescher (Notre Dame) (Schatz et al. PRL 86(2001)3471)