anuj parikh universitat politècnica de catalunya (upc) institut d'estudis espacials de...

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