22 Ne(p,γ) 23 Na MEASUREMENT AT LUNA II AND IMPACT ON ASTROPHYSICAL SCENARIOS MARIE-LUISE MENZEL for the LUNA collaboration
1. INTRODUCTION 1.1 NEON-SODIUM-CYCLE 1.2 THE 22 Ne(p,γ) 23 Na REACTION
INTRODUCTION NEON-SODIUM CYCLE > hydrogen burning process > temperature range: 0.1-0.4 GK 19 20 Mg 21 Mg 22 23 Mg Mg Mg 24 Mg 25 Mg 26 Mg 20 Na 21 Na 22 Na 23 Na Thermonuclear Reaction Rate TNRR (cm 3 /mol/s) 10 2 10 0 10 2 10 4 10 6 10 8 (C. Illiadis et al., Nucl Phys A 841, 251 (2010) 21 Ne(p,γ) 22 Na 23 Na(p,α) 20 Ne 23 Na(p,γ) 24 Mg 22 Ne(p,γ) 23 Na 20 Ne(p,γ) 21 Na 0.1 0.2 0.3 0.4 0.5 Temperature T (10 9 K) Iliadis 20 Ne(p,g) Iliadis 21 Ne(p,g) Iliadis 22 Ne(p,g) Iliadis 23 Na(p,g) Iliadis 23 Na(p,a) 17 18 Ne 19 Ne 20 21 Ne Ne Ne 22 Ne 17 F 18 F 19 F from CNO-cycle (p,α) (p,ɣ) (p,α) (n,p)
INTRODUCTION THE 22 Ne(p,γ) 23 Na REACTION LUNA energy range E CM E Lab E x (kev) Jπ 377±3 353? 319±3 309±3 278±3 245±1 206? 178±3 152±3 394±3 369? 333±3 323±3 291±3 256±1 215? 186±3 159±3 9171±3 9147? 9113±3 9103±3 9072±3 9038.7±1.0 9000? 8972±2 8946±3 3/2, 5/2+ 5/2, 7/2- Thermonuclear Reaction Rate log(n A <σν>) [cm 3 mole 1 sec 1 ] 10 1 10 0 10 1 10 2 10 3 10 4 10 5 10 6 10 7 10 8 E lab = 71 kev E lab =104 kev E lab =159 kev E lab =186 kev E lab =215 kev E lab =436 kev E lab =479 kev (S.E. Hale et al., Phys Rev C 65 (2001)) 0.1 0.2 0.3 0.4 Temperature log(t) [10 9 K] 100? 104? 8894? 1/2+ 68? 35.4±0.5 28±3 71? 37.0±0.5 29±3 8862? 8829.5±0.5 8822±3 1/2+ 1/2+ 8794.11 22 Ne+p 3±3 3±3 8797±3 2076.011±0.022 7/2+ 439.990±0.009 5/2+ 0 23 Na 3/2+
2. 22 Ne(p,γ) 23 Na MEASUREMENT AT LUNA II 2.1 LUNA II SETUP 2.2 SPECTRAL ANALYSIS 2.3 RESULTS
22 Ne(p,γ) 23 Na MEASUREMENT LUNA II SETUP > windowless gas target chamber > proton beam energy: 100-400 kev > HPGe detector (high resolution) beam target chamber > natural neon gas target 9.3% 22 Ne, 0.3% 21 Ne, 90.5% 20 Ne > lead and polyethylene-shielding indentation for HPGe detector back flange for calorimeter
22 Ne(p,γ) 23 Na MEASUREMENT SPECTRAL ANALYSIS 60 50 E γ (kev) 410 420 430 440 450 460 470 low energetic BG signal high energetic BG E x (kev) 8972±2 8945±2 3/2, 5/2 5/2, 7/2- Jπ counts per channel 40 30 20 10 2076.011±0.022 7/2+ 440 kev 1636 kev 439.990±0.009 5/2+ counts per channel 0 410 420 430 440 450 460 470 channel number E γ (kev) 1600 1610 1620 1630 1640 1650 1660 60 low energetic BG signal high energetic BG 50 40 30 20 0 23 Na 3/2+ 10 0 1610 1620 1630 1640 1650 1660 1670 channel number lab Eres = 186 kev
22 Ne(p,γ) 23 Na MEASUREMENT RESULTS: RESONANCE STRENGTHS - PRELIMINARY -0.87. (J. Görres et al., Nucl Phys A 408, 372 (1983) (S.E. Hale et al., Phys Rev C 65 (2001) (C. Illiadis et al., Nucl Phys A 841, 251 (2010)
22 Ne(p,γ) 23 Na MEASUREMENT RESULTS: THERMONUCLEAR REACTION RATE 1 Ratio log(tnrr new /TNRR NACRE ) 0.1 0.01 0.001 Hale with LUNA Iliadis with LUNA 0.1 1 Temperature log (T) [10 9 K]
3. EXPLOSIVE HYDROGEN BURNING IN NOVAE 3.1 ASTROPHYSICAL INTRODUCTION 3.2 NUCLEAR NETWORK CALCULATION FOR NOVAE 3.3 NEON-SODIUM-CYCLE
EXPLOSIVE HYDROGEN BURNING IN NOVAE ASTROPHYSICAL INTRODUCTION > compression of hydrogen matter on white dwarf surface > ignition of hydrogen in degenerated matter > thermonuclear runaway and ejection of outer envelope > 0.1 GK < T < 0.5 GK (120 kev < Ecm < 350 kev) Roche lobe of companion star Roche lobe of white dwarf radiation pressure gravitational pressure matter transfer Lagrange point white dwarf with accretion disk companion star
EXPLOSIVE HYDROGEN BURNING IN NOVAE NUCLEAR NETWORK CALCULATION > public domain libnucnet code (B. S. Meyer, Clemson University) (sourceforge.net/u/mbrandle/nlog/) > Requirements for network calculation: - initial mass composition for 50:50 white dwarf and giant star - temperature-density-profile - thermo-nuclear reaction rates (JINA database) (C. Ritossa et al., ApJ 460, 489 (1996)) (K. Lodders et al., ApJ 591, 1220 (2003) Temperature T (10 9 K) 10 0 10 1 T max = 0.43 GK T max = 0.35 GK T max = 0.30 GK T max = 0.25 GK T max = 0.20 GK 10 5 80 90 100 110 120 130 140 150 160 Density ρ (g/cm 3 ) 10 4 10 3 10 2 10 1 (Starrfield et al., APJSS 127, 458 (2000)) 10 0 80 90 100 110 120 130 140 150 160 Time t (sec)
EXPLOSIVE HYDROGEN BURNING IN NOVAE NEON-SODIUM CYCLE c.) Temperature T (GK) a.) b.) d.) e.) f.) Time t (sec) a.) b.) c.)
EXPLOSIVE HYDROGEN BURNING IN NOVAE NEON-SODIUM CYCLE c.) Temperature T (GK) a.) b.) d.) e.) f.) Time t (sec) d.) c.) e.)
EXPLOSIVE HYDROGEN BURNING IN NOVAE NEON-SODIUM-CYCLE IN CO-TYPE NOVAE > strong influence of the 22 Ne(p,γ) 23 Na TNRR on abundance C. Iliadis et al. AJSS, 142 (2002) TNRR x 100 TNRR x 0.1 (credits to R. Depalo)
4. HYDROSTATIC HYDROGEN BURNING 4.1 RED GIANT BRANCH STARS 4.2. ASYMPTOTIC GIANT BRANCH STARS
HYDROSTATIC HYDROGEN BURNING RGB STARS > inactive He core, H-burning shell (0.015 GK < T < 0.06 GK) E. Carretta et al. A&A, 505 (2009) > CNO and NaNa cycle cause anti-correlation of Na and O abundance of RGB > transport of products to the envelope e.g. meridional circulation in radiative zone (dependent of TNRR)
HYDROSTATIC HYDROGEN BURNING AGB STARS (0.8 < Msolar < 8) > CO core, inactive He inter-shell and thin H-burning shell > hot bottom burning (0.06 GK < T < 0.1 GK) at layer of H-burning shell and convective envelope > thermal pulsing every 10.000-100.000 years: He-shell flash (T > 0.2 GK), H-shell extinction > convective envelope contains H- and He-burning products
5. SUMMARY
SUMMARY 22 Ne(p,γ) 23 Na MEASUREMENT AT LUNA II > analysis of 5 resonances > determination of new resonance strengths for Eres = 186 kev > determination of large TNRR uncertainty in 0.03 GK < T < 0.3 GK ASTROPHYSICAL IMPACT E CM E Lab E x (kev) Jπ > explosive hydrogen burning in novae > hydrostatic hydrogen burning in AGB and RGB stars LUNA energy range 377±3 353? 319±3 309±3 278±3 245±1 206? 178±3 152±3 394±3 369? 333±3 323±3 291±3 256±1 215? 186±3 159±3 9171±3 9147? 9113±3 9103±3 9072±3 9038.7±1.0 9000? 8972±2 8946±3 3/2, 5/2+ 5/2, 7/2-100? 104? 8894? 1/2+ 68? 35.4±0.5 28±3 71? 37.0±0.5 29±3 8862? 8829.5±0.5 8822±3 1/2+ 1/2+ 8794.11 22 Ne+p 3±3 3±3 8797±3 2076.011±0.022 7/2+ 439.990±0.009 5/2+ 0 23 Na 3/2+
MARIE-LUISE MENZEL THANKS FOR YOUR ATTENTION! credits to D. Bemmerer (HZDR) R. Depalo (Università di Padova) F. Cavanna (Università di Genova) Prof. G. Matinez-Pinedo (Universität Darmstadt)