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

2. 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 ~ ly)
HST

3. 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”

4. OBSERVATIONS
mass fraction in ejecta
José and Hernanz (1998)

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

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

7. 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)

8. 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

9. 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

10. 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 = MeV):
22Na(p,)23Mg, 20Ne(p,)21Na, 23Na(p,a)20Ne, 23Na(p,)24Mg, 21Na(p,)22Mg
26Al (t1/2 = 0.7 My, E = MeV):
23Mg(p,)24Al, 26Al(p,)27Si, 23Na(p,)24Mg, 23Na(p,a)20Ne, 20Ne(p,)21Na

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

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

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

14. 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

15. 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 TRIUMF

16. 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 TRIUMF
Or indirectly:

17. 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 TRIUMF
Or indirectly:
Need proton C2S and Jπ to calculate (ωγ) indirectly

18. 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 TRIUMF
Or indirectly:
Vogelaar et al. (1996), Princeton Q3D, ΔE ~ 12 keV, 26Al(3He,d)27Si

19. Maier-Leibnitz-Laboratorium (Garching, Germany)

20. Maier-Leibnitz-Laboratorium (Garching, Germany)

21. Maier-Leibnitz-Laboratorium (Garching, Germany)

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

23. Maier-Leibnitz-Laboratorium (Garching, Germany)

24. 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!

25. 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):
ANL-Gammasphere
energies, spins (high-spin states), new state
30P+p
Q = 6133
Ma et al. (2007):
32S(p,d)31S, angular ORNL
energies, spins
Wrede et al. (2007, 2009):
31P(3He,t)31S* → p + Yale
energies, new states, Γp /Γ for Ex > 6719 keV
31S
30P (1+, t1/2 = 2.5 min)

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

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

28. Using 31P(3He,t)31S for 30P(p,)31S
E3He = 20 MeV
1.5°
Yale Split-Pole
ΔE = 25 keV
5 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 nA
ΔE = 10 keV
AP et al. (accepted)
counts
30P+p
Q = 6133
31S
Etriton

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

30. 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
6 750 nA
ΔE ~ 8 keV
PRELIMINARY
A. A. Chen et al.

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

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

33. 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 nA
Endt (1990)
AP et al. (2009)

34. 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
1 500 nA
Endt (1990)
AP et al.

35.
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