Anuj Parikh
Universitat Politècnica de Catalunya (UPC)
Institut d'Estudis Espacials de Catalunya (IEEC)
Nuclear astrophysics with the Munich Q3D spectrograph
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 nucleosynthesis: H – Ca
nuclear reactions: mostly experimental
Classical nova explosions
Nova Cygni 1992 (d ~ 10 000 ly)
~1011 km
HST
Most of the thermonuclear reaction rates involved are constrained by experiments
Hardy and PPARC
OBSERVATIONSNova Her 1934 (optical), d ~ 500 ly
March 1934 May 1934 1974
0.1 ly
“typical”
Vanlandingham et al. (1997)Nova V693 CrA 1981
OBSERVATIONS
José and Hernanz (1998)
mass fraction in ejecta
MODELS
13C, 15N, 17O
José, Casanova, Moreno, García-Berro, AP, and Iliadis (2010)
MODELS
José and Hernanz (2007)
13C, 15N, 17O
solar
Casanova et al. (2010)
MODELS
t = 214 s
t = 498 s
t = 234 s
t = 279 s
Convection via 12C abundance (2D model)~
500
km
800 km
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
Fox et al. 2004,2005; Chafa et al. 2005,2007
Davids et al. 2003, Bishop et al. 2003, D’Auria et al. 2004
Rowland et al. 2004, Hale et al. 2004
Parete-Koon et al. 2003
Hale et al. 2002
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
Visser et al. 2007, Zegers et al. 2008, Lotay et al. 2008
Ruiz et al. 2006
Jenkins et al. 2006, Ma et al. 2007, Wrede et al. 2007, 2009;
Lewis et al. 2005, Deibel et al. 2008, Lotay et al. 2009
Parikh et al. 2009
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
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
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
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
NUCLEAR PHYSICS
José, Casanova, Moreno, García-Berro, AP, and Iliadis (2010)
33S(p,γ)34Cl
30P(p,γ)31S26Al(p,γ)27Si
NUCLEAR PHYSICS
Impact of rate: 30P(p,γ)31S
José et al. 2001
Iliadis et al. 2002
3/ 2
2 ,( )2( ) exp
CMR i
ii
E
kT kT
Resonant component of the thermonuclear rate:
Measure directly or indirectly
ERCM and ()
(masses, spins, partial widths, lifetimes)
CASE STUDY: 26Al(p,)27Si
Determine ER directly:
Or indirectly (as Ex):
For nova, AGB, WR conditions, all ER are ~known for 27Si
Buchmann et al. (1984)
Münster, Stuttgart, Bochum
26Al target, Ge, NaI
Schmalbrock et al. (1986)
Notre Dame
100 cm spectrograph
28Si(3He,a)27SiCo
un
tsC
ou
nts
Ep (keV)
← Ex (27Si) (keV)
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
Or indirectly:
Determine (ωγ) directly:
3/ 2
2 ,( )2( ) exp
CMR i
ii
E
kT kT
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
Or indirectly:
Determine (ωγ) directly:
3/ 2
2 ,( )2( ) exp
CMR i
ii
E
kT kT
Need proton C2S and Jπ to calculate (ωγ) 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
CASE STUDY: 26Al(p,)27Si
Or indirectly:
Vogelaar et al. (1996), Princeton Q3D, ΔE ~ 12 keV, 26Al(3He,d)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
Maier-Leibnitz-Laboratorium (Garching, Germany)
Maier-Leibnitz-Laboratorium (Garching, Germany)
Maier-Leibnitz-Laboratorium (Garching, Germany)
Maier-Leibnitz-Laboratorium (Garching, Germany)
31P + 3He → 31S + 3H
3He
31P, 31S*
3H3H
3H3H
Maier-Leibnitz-Laboratorium (Garching, Germany)
IDEA: Using magnetic spectrographs in nuclear astrophysics to determine ER, Jπ, C2S, Γx via indirect studies
Superior energy resolution of the MLL Q3D helps!
Yale Enge Split-Pole
dΩ ~ 3.2 msr
ΔE/E ~ 1 x 10-3
Δρ ~ 14 cm
I3He ~ 50 nA
VTmax ~ 18 MV
MLL Q3D
dΩ ~ 14 msr
ΔE/E ~ 2 x 10-4
Δρ ~ 6 cm
I3He ~ 500 nA
VTmax ~ 14 MV
Nova explosions: 30P(p,γ)31S
30P+p
Q = 6133
31S30P (1+, t1/2 = 2.5 min)
Wrede et al. (2007, 2009): 31P(3He,t)31S* → p + 30P @ Yale energies, new states, Γp /Γ for Ex > 6719 keV
Jenkins et al. (2005, 2006): 12C(20Ne,nγ)31S @ ANL-Gammasphere energies, spins (high-spin states), new state
Ma et al. (2007): 32S(p,d)31S, angular distributions @ ORNL energies, spins
Direct: hard…For DRAGON, need >106 pps 30P [S1108 – Wrede, Hutcheon et al., Stage 1]
30P+p
Q = 6133
T <
0.4
GK
31S
3 new states!31P(3He,t)31SE3He = 20 MeV1.5°Yale Split-PoleΔE ~ 25 keV5 d @ 50 nA
Wrede et al. (2007)
Using 31P(3He,t)31S for 30P(p,)31S
30P+p
Q = 6133
T <
0.4
GK
31S
3 new states!
Using 31P(3He,t)31S for 30P(p,)31S
31P(3He,t)31SE3He = 25 MeV10°MLL Q3D12 h @ 650 nAΔE = 10 keVAP et al. (accepted)
31P(3He,t)31SE3He = 20 MeV1.5°Yale Split-PoleΔE = 25 keV5 d @ 50 nA
coun
ts
Etriton
30P+p
Q = 6133
31S
Using 31P(3He,t)31S for 30P(p,)31S
31P(3He,t)31SE3He = 25 MeV10°MLL Q3D12 h @ 650 nAΔE = 10 keVAP et al. (accepted)
31P(3He,t)31SE3He = 20 MeV1.5°Yale Split-PoleΔE = 25 keV5 d @ 50 nA5/2–
1/2+
ϴCM (deg)ϴCM (deg)
dσ
/dΩ
(μ
b/s
r)
dσ
/dΩ
(μ
b/s
r)
coun
ts
Etriton
Using 31P(3He,t)31S for 30P(p,)31S
José et al. 2001
AP et al. (accepted)
A. A. Chen et al.
Using 32S(d,t)31S for 30P(p,)31S
32S(3He,d)31SEd = 24 MeV20°MLL Q3D6 h @ 750 nAΔE ~ 8 keVPRELIMINARY
31P(3He,t)31SE3He = 20 MeV1.5°Yale Split-PoleΔE ~ 25 keVWrede et al. (2007)
E = 25 MeV20 degMLL Q3D, 2 h @ 500 nAAP et al. (in prep)ΔE ~ 15 keVPRELIMINARY
Using 28Si(3He,4He)27Si for 26Al(p,)27Si
Schmalbrock+ (1986)Notre Dame
Ex(27Si)
E = 25 MeV20 degMLL Q3D, 2 h @ 500 nAAP et al. (in prep)ΔE ~ 15 keVPRELIMINARY
Using 28Si(3He,4He)27Si for 26Al(p,)27Si
Schmalbrock+ (1986)Notre Dame
FIRST search for 34Cl p-threshold states with 34S(3He,t)34Cl
→ 9 new states within 600 keV of Sp(34Cl)
Ex(34Cl)
5576 51
43
AP et al. (2009)
34S(3He,t)34ClE3He = 25 MeV; 15°MLL Q3DΔE = 10 keV24 h @ 500 nA
Endt (1990)
Using 34S(3He,t)34Cl for 33S(p,)34Cl
FIRST search for 34Cl p-threshold states with 33S(3He,d)34Cl
→ for C2S…PRELIMINARY
Ex(34Cl)
5143
33S(3He,d)34ClE3He = 25 MeV; 10°MLL Q3DΔE ~ 9 keV1 h @ 500 nA
Endt (1990)
Using 33S(3He,d)34Cl for 33S(p,)34Cl
AP et al.
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
www.Q3D.org
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