Nuclear astrophysics with the Munich Q3D spectrograph Anuj Parikh Universitat Politècnica de Catalunya (UPC) Institut d'Estudis Espacials de Catalunya (IEEC)

Classical nova explosions Compact object: white dwarf (CO / ONe) Lmax: ~ 104 – 105 Lsol tlightcurve: ~ days – months trec: ~ 104 – 105 yr Tp: ~ 0.1 – 0.4 GK #Galaxy: ~ 30 / yr Ejecta: ~ 10-4 – 10-5 Msol / nova Hardy and PPARC ~1011 km nucleosynthesis: H – Ca nuclear reactions:  mostly experimental Most of the thermonuclear reaction rates involved are constrained by experiments Nova Cygni 1992 (d ~ 10 000 ly) HST

OBSERVATIONS Nova Her 1934 (optical), d ~ 500 ly March 1934 May 1934 1974 0.1 ly Vanlandingham et al. (1997) Nova V693 CrA 1981 “typical”

OBSERVATIONS mass fraction in ejecta José and Hernanz (1998)

MODELS 13C, 15N, 17O José, Casanova, Moreno, García-Berro, AP, and Iliadis (2010)

MODELS 13C, 15N, 17O solar José and Hernanz (2007)

MODELS Convection via 12C abundance (2D model) ~500 km 800 km t = 214 s t = 234 s ~500 km 800 km t = 279 s t = 498 s Casanova et al. (2010)

NUCLEAR PHYSICS Nova sensitivity study (Iliadis et al. (2002)) : ■ T-ρ-t profiles from 5 different hydrodynamic nova simulations ■ Variation of each of 175 reaction rates within errors

NUCLEAR PHYSICS Nova sensitivity study (Iliadis et al. (2002)) : ■ T-ρ-t profiles from 5 different hydrodynamic nova simulations ■ Variation of each of 175 reaction rates within errors Fox et al. 2004,2005; Chafa et al. 2005,2007 Parete-Koon et al. 2003 Bardayan et al. 2001, 2005; Graulich et al. 2001, de Sereville 2003, 2005, 2007; Kozub et al. 2005, Chae et al. 2006, Beer et al. 2011 Davids et al. 2003, Bishop et al. 2003, D’Auria et al. 2004 Hale et al. 2002 Rowland et al. 2004, Hale et al. 2004 Visser et al. 2007, Zegers et al. 2008, Lotay et al. 2008 Ruiz et al. 2006 Lewis et al. 2005, Deibel et al. 2008, Lotay et al. 2009 Jenkins et al. 2006, Ma et al. 2007, Wrede et al. 2007, 2009; Parikh et al. 2009

NUCLEAR PHYSICS Nova sensitivity study (Hix et al. (2003)) : ■ T-ρ-t profile from one hydrodynamic nova simulation ■ Monte-Carlo: Variation of all rates by random factors…10000 trials 22Na (t1/2 = 2.6 y, E = 1.275 MeV): 22Na(p,)23Mg, 20Ne(p,)21Na, 23Na(p,a)20Ne, 23Na(p,)24Mg, 21Na(p,)22Mg 26Al (t1/2 = 0.7 My, E = 1.809 MeV): 23Mg(p,)24Al, 26Al(p,)27Si, 23Na(p,)24Mg, 23Na(p,a)20Ne, 20Ne(p,)21Na

NUCLEAR PHYSICS 33S(p,γ)34Cl 26Al(p,γ)27Si 30P(p,γ)31S José, Casanova, Moreno, García-Berro, AP, and Iliadis (2010)

Impact of rate: 30P(p,γ)31S Iliadis et al. 2002 José et al. 2001

Resonant component of the thermonuclear rate: Measure directly or indirectly ERCM and () (masses, spins, partial widths, lifetimes)

CASE STUDY: 26Al(p,)27Si ← Ex (27Si) (keV) Determine ER directly: Buchmann et al. (1984) Münster, Stuttgart, Bochum 26Al target, Ge, NaI Counts Ep (keV) Or indirectly (as Ex): Schmalbrock et al. (1986) Notre Dame 100 cm spectrograph 28Si(3He,a)27Si ← Ex (27Si) (keV) Counts For nova, AGB, WR conditions, all ER are ~known for 27Si

CASE STUDY: 26Al(p,)27Si Determine (ωγ) directly: Ruiz, AP, José et al. (2006) ER = 184 keV resonance 2 weeks of 26Al beam (~3 x 109 pps) 120 27Si events DRAGON recoil separator @ TRIUMF

CASE STUDY: 26Al(p,)27Si Determine (ωγ) directly: Or indirectly: Ruiz, AP, José et al. (2006) ER = 184 keV resonance 2 weeks of 26Al beam (~3 x 109 pps) 120 27Si events DRAGON recoil separator @ TRIUMF Or indirectly:

CASE STUDY: 26Al(p,)27Si Determine (ωγ) directly: Ruiz, AP, José et al. (2006) ER = 184 keV resonance 2 weeks of 26Al beam (~3 x 109 pps) 120 27Si events DRAGON recoil separator @ TRIUMF Or indirectly: Need proton C2S and Jπ to calculate (ωγ) indirectly

CASE STUDY: 26Al(p,)27Si Determine (ωγ) directly: Or indirectly: Ruiz, AP, José et al. (2006) ER = 184 keV resonance 2 weeks of 26Al beam (~3 x 109 pps) 120 27Si events DRAGON recoil separator @ TRIUMF Or indirectly: Vogelaar et al. (1996), Princeton Q3D, ΔE ~ 12 keV, 26Al(3He,d)27Si

Maier-Leibnitz-Laboratorium (Garching, Germany)

Maier-Leibnitz-Laboratorium (Garching, Germany)

Maier-Leibnitz-Laboratorium (Garching, Germany)

Maier-Leibnitz-Laboratorium (Garching, Germany) 31P + 3He → 31S + 3H 3H 3H 3H 3H 31P, 31S* 3He

Maier-Leibnitz-Laboratorium (Garching, Germany)

Superior energy resolution of the MLL Q3D helps! IDEA: Using magnetic spectrographs in nuclear astrophysics to determine ER, Jπ, C2S, Γx via indirect studies MLL Q3D dΩ ~ 14 msr ΔE/E ~ 2 x 10-4 Δρ ~ 6 cm I3He ~ 500 nA VTmax ~ 14 MV Yale Enge Split-Pole dΩ ~ 3.2 msr ΔE/E ~ 1 x 10-3 Δρ ~ 14 cm I3He ~ 50 nA VTmax ~ 18 MV Superior energy resolution of the MLL Q3D helps!

Nova explosions: 30P(p,γ)31S Direct: hard… For DRAGON, need >106 pps 30P [S1108 – Wrede, Hutcheon et al., Stage 1] Jenkins et al. (2005, 2006): 12C(20Ne,nγ)31S @ ANL-Gammasphere energies, spins (high-spin states), new state 30P+p Q = 6133 Ma et al. (2007): 32S(p,d)31S, angular distributions @ ORNL energies, spins Wrede et al. (2007, 2009): 31P(3He,t)31S* → p + 30P @ Yale energies, new states, Γp /Γ for Ex > 6719 keV 31S 30P (1+, t1/2 = 2.5 min)

Using 31P(3He,t)31S for 30P(p,)31S E3He = 20 MeV 1.5° Yale Split-Pole ΔE ~ 25 keV 5 d @ 50 nA 3 new states! T < 0.4 GK 30P+p Q = 6133 Wrede et al. (2007) 31S

Using 31P(3He,t)31S for 30P(p,)31S E3He = 20 MeV 1.5° Yale Split-Pole ΔE = 25 keV 5 d @ 50 nA 3 new states! T < 0.4 GK 31P(3He,t)31S E3He = 25 MeV 10° MLL Q3D 12 h @ 650 nA ΔE = 10 keV AP et al. (accepted) counts 30P+p Q = 6133 31S Etriton

Using 31P(3He,t)31S for 30P(p,)31S E3He = 20 MeV 1.5° Yale Split-Pole ΔE = 25 keV 5 d @ 50 nA 1/2+ dσ/dΩ (μb/sr) 5/2– dσ/dΩ (μb/sr) ϴCM (deg) ϴCM (deg) 31P(3He,t)31S E3He = 25 MeV 10° MLL Q3D 12 h @ 650 nA ΔE = 10 keV AP et al. (accepted) counts 30P+p Q = 6133 31S Etriton

Using 31P(3He,t)31S for 30P(p,)31S AP et al. (accepted) José et al. 2001

Using 32S(d,t)31S for 30P(p,)31S 31P(3He,t)31S E3He = 20 MeV 1.5° Yale Split-Pole ΔE ~ 25 keV Wrede et al. (2007) 32S(3He,d)31S Ed = 24 MeV 20° MLL Q3D 6 h @ 750 nA ΔE ~ 8 keV PRELIMINARY A. A. Chen et al.

Using 28Si(3He,4He)27Si for 26Al(p,)27Si Schmalbrock+ (1986) Notre Dame E = 25 MeV 20 deg MLL Q3D, 2 h @ 500 nA AP et al. (in prep) ΔE ~ 15 keV PRELIMINARY Ex(27Si)

Using 28Si(3He,4He)27Si for 26Al(p,)27Si Schmalbrock+ (1986) Notre Dame E = 25 MeV 20 deg MLL Q3D, 2 h @ 500 nA AP et al. (in prep) ΔE ~ 15 keV PRELIMINARY

Using 34S(3He,t)34Cl for 33S(p,)34Cl FIRST search for 34Cl p-threshold states with 34S(3He,t)34Cl → 9 new states within 600 keV of Sp(34Cl) 5143 5576 Ex(34Cl) 34S(3He,t)34Cl E3He = 25 MeV; 15° MLL Q3D ΔE = 10 keV 24 h @ 500 nA Endt (1990) AP et al. (2009)

Using 33S(3He,d)34Cl for 33S(p,)34Cl FIRST search for 34Cl p-threshold states with 33S(3He,d)34Cl → for C2S…PRELIMINARY 5143 Ex(34Cl) 33S(3He,d)34Cl E3He = 25 MeV; 10° MLL Q3D ΔE ~ 9 keV 1 h @ 500 nA Endt (1990) AP et al.

www.Q3D.org T. Faestermann, R. Krücken, T. Behrens, V. Bildstein, S. Bishop, K. Eppinger, C. Herlitzius, C. Hinke, O. Lepyoshkina, P. Maierbeck, G. Rugel, M. Schlarb, D. Seiler, K. Wimmer R. Hertenberger, H.-F. Wirth A. A. Chen, K. Setoodehnia J. A. Clark, C. Deibel C. Wrede R. Longland