Classical novaeIndirect reaction study

Summary

The 18Ne(α,p)21Na Hot-CNO cyclebreakout reaction

—an indirect study through deuteron transfer

Christian Aa. Diget

Institute of Physics Nuclear Physics Conference,Birmingham, 6th April 2009

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

ObservationsReactions

Observations of novae

Thermo-nuclearrun-away on surface ofwhite dwarf.

Fueled by envelope ofbinary red-giant.

Observed from radio toX-rays.

Illustration: David Hardy/PPARC

Outburst profile, RS-Ophiuchi 2006

Am. Ass. of Variable Star Obs., Alert notice 335

A. Price, AAVSO, Wikipedia (2006)

Ejected gas shellNova-Cygni 1992Hubble, STScI-PRC1994-06

Asymmetric shock wave,RS-Ophiuchi 2006O’Brien et al., Nature, 442:279 (2006)

Sokoloski et al., Nature, 442:276 (2006)

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

ObservationsReactions

Observations of novae

Thermo-nuclearrun-away on surface ofwhite dwarf.

Fueled by envelope ofbinary red-giant.

Observed from radio toX-rays.

Illustration: David Hardy/PPARC

Outburst profile, RS-Ophiuchi 2006

Am. Ass. of Variable Star Obs., Alert notice 335

A. Price, AAVSO, Wikipedia (2006)

Ejected gas shellNova-Cygni 1992Hubble, STScI-PRC1994-06

Asymmetric shock wave,RS-Ophiuchi 2006O’Brien et al., Nature, 442:279 (2006)

Sokoloski et al., Nature, 442:276 (2006)

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

ObservationsReactions

Observations of novae

Thermo-nuclearrun-away on surface ofwhite dwarf.

Fueled by envelope ofbinary red-giant.

Observed from radio toX-rays.

Illustration: David Hardy/PPARC

Outburst profile, RS-Ophiuchi 2006

Am. Ass. of Variable Star Obs., Alert notice 335

A. Price, AAVSO, Wikipedia (2006)

Ejected gas shellNova-Cygni 1992Hubble, STScI-PRC1994-06

Asymmetric shock wave,RS-Ophiuchi 2006O’Brien et al., Nature, 442:279 (2006)

Sokoloski et al., Nature, 442:276 (2006)

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

ObservationsReactions

Observations of novae

Thermo-nuclearrun-away on surface ofwhite dwarf.

Fueled by envelope ofbinary red-giant.

Observed from radio toX-rays.

Illustration: David Hardy/PPARC

Outburst profile, RS-Ophiuchi 2006

Am. Ass. of Variable Star Obs., Alert notice 335

A. Price, AAVSO, Wikipedia (2006)

Ejected gas shellNova-Cygni 1992Hubble, STScI-PRC1994-06

Asymmetric shock wave,RS-Ophiuchi 2006O’Brien et al., Nature, 442:279 (2006)

Sokoloski et al., Nature, 442:276 (2006)

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

ObservationsReactions

Nuclear synthesis in novae

Gamma-ray lines from radioactivenuclei synthesized in classical no-vae: 13N(β+), 18F(β+), 7Be(EC,γ),22Na(β+γ), 26Al(β+γ)

Clayton & Hoyle., APJ, 187:L101 (1974)

Satellite missions for direct observa-tions of γ-ray lines from novae:

Present: Strong γ-ray emitters:γ-ray bursts, black holes,pulsars.

INTEGRAL (ESA,2002)Fermi/GLAST (NASA,2008)

Next-generation: Sensitivity toweaker γ-ray sources (e.g.novae).

EXIST (NASA)Gamma-Ray Lens: (ESA)ACT (Advanced ComptonTelescope, NASA)

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

ObservationsReactions

Nuclear synthesis in novae

Gamma-ray lines from radioactivenuclei synthesized in classical no-vae: 13N(β+), 18F(β+), 7Be(EC,γ),22Na(β+γ), 26Al(β+γ)

Clayton & Hoyle., APJ, 187:L101 (1974)

Satellite missions for direct observa-tions of γ-ray lines from novae:

Present: Strong γ-ray emitters:γ-ray bursts, black holes,pulsars.

INTEGRAL (ESA,2002)Fermi/GLAST (NASA,2008)

Next-generation: Sensitivity toweaker γ-ray sources (e.g.novae).

EXIST (NASA)Gamma-Ray Lens: (ESA)ACT (Advanced ComptonTelescope, NASA)

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

ObservationsReactions

Nuclear synthesis in novae

Gamma-ray lines from radioactivenuclei synthesized in classical no-vae: 13N(β+), 18F(β+), 7Be(EC,γ),22Na(β+γ), 26Al(β+γ)

Clayton & Hoyle., APJ, 187:L101 (1974)

Satellite missions for direct observa-tions of γ-ray lines from novae:

Present: Strong γ-ray emitters:γ-ray bursts, black holes,pulsars.

INTEGRAL (ESA,2002)Fermi/GLAST (NASA,2008)

Next-generation: Sensitivity toweaker γ-ray sources (e.g.novae).

EXIST (NASA)Gamma-Ray Lens: (ESA)ACT (Advanced ComptonTelescope, NASA)

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

ObservationsReactions

Reaction rates for Novae and X-ray bursters

The CNO and Hot-CNOcycles.

Build-up of waiting-pointnuclei in novae:

14O15O18Ne

Topical review R143

Figure 6. The figure shows the characteristic hot (or !-limited) CNO cycles which contribute tothe energy generation in explosive hydrogen burning scenarios like novae and x-ray bursts.

cycle). The timescale for the fusion of four hydrogen nuclei to helium and subsequently the

associated energy generation is determined by the lifetimes of 14O (t1/2 = 70.59 s) and 15O

(t1/2 = 122 s) and is therefore temperature independent. These isotopes represent waiting

points along the nucleosynthesis path. Figure 5 indicates that the energy generation by the

CNO cycles turns flat at the temperature and conditions where the slowest proton capture

rate (14N(p, " )15N) exceeds the !-decay rates for 14O and 15O. These !-decay limitations fix

the energy production rate adopting a cycle time of # ! 200 s and a total energy release of

QCNO = 26.7 MeV to

$HCNO = 4.6" 1015ZCNO (erg g#1 s#1) (8)

whereZCNO is the mass fraction of the CNOmaterial and!50% of the CNOmaterial is storedin 14O and 15O (see also [6]). The timescale for the consumption of the hydrogen in the hot

CNO cycles is given by

tCNO = ECNO

$HCNO

! 1000

ZCNO

(s) (9)

withECNO = 4.51"1018 erg g#1 (forXH = 0.7). This corresponds to a timescale of about one

day for hydrogen consumption in solar metalicity material (Z$ = 0.02, ZCNO = 0.72 · Z$).Similarily, for the second CNO cycle (see figure 6) at higher temperatures the

proton capture rate on 17F exceeds its !-decay rate and the second hot cycle emerges,16O(p, " )17F(p, " )18Ne(!+%) 18F(p, &)15O. This cycle is again limited by the drip line because19Na is proton unbound. The conversion time in the cycle and the energy generation is again

temperature independent and is determined by the !-decay lifetime of the waiting point isotope18Ne (t1/2 = 1.67 s).

The thermonuclear runaway in novae is driven by the energy release of the hot CNOcycles.

The abundance distribution in the ejecta depends on the associated nucleosynthesis [23–25].

Figure 7 shows as an example the variation with time of temperature and density in the deepest

hydrogen rich zone of the accreted envelope during the thermonuclear runaway [32]. The

corresponding nucleosynthesis of CNO material is shown in figure 8. One can easily observe

the rapid depletion of the initial 16O and the build up of the waiting point nuclei. After a

relatively short time the initial abundances have changed to 14O, 15O and 18Ne which are

enriched due to their slow !-decay. Because the peak temperatures in the thermonuclear

runaway are typically below 3.5"108 K [32], break-out is inhibited due to the limited reactionrates for the break-out processes to be discussed in later sections. Indeed, observation of the

abundance distribution in nova ejecta indicate large overabundances of nitrogen [36] produced

by the slow !-decay of the highly enriched 14O and 15O isotopes.

Wiescher et al., JPG, 25:R133 (1999)

Breakout from CNO-cycles:14O(α, p)17F15O(α, γ)19Ne18Ne(α, p)21Na

Resonant reaction rate:

(2J + 1)ΓinΓout

Γtotexp(− Er

kBT)

Gamow-window: 0.7–2.0 MeVresonance energy fortemperatures of 0.5–1.5 GK.

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

ObservationsReactions

Reaction rates for Novae and X-ray bursters

The CNO and Hot-CNOcycles.

Build-up of waiting-pointnuclei in novae:

14O15O18Ne

Topical review R143

Figure 6. The figure shows the characteristic hot (or !-limited) CNO cycles which contribute tothe energy generation in explosive hydrogen burning scenarios like novae and x-ray bursts.

cycle). The timescale for the fusion of four hydrogen nuclei to helium and subsequently the

associated energy generation is determined by the lifetimes of 14O (t1/2 = 70.59 s) and 15O

(t1/2 = 122 s) and is therefore temperature independent. These isotopes represent waiting

points along the nucleosynthesis path. Figure 5 indicates that the energy generation by the

CNO cycles turns flat at the temperature and conditions where the slowest proton capture

rate (14N(p, " )15N) exceeds the !-decay rates for 14O and 15O. These !-decay limitations fix

the energy production rate adopting a cycle time of # ! 200 s and a total energy release of

QCNO = 26.7 MeV to

$HCNO = 4.6" 1015ZCNO (erg g#1 s#1) (8)

whereZCNO is the mass fraction of the CNOmaterial and!50% of the CNOmaterial is storedin 14O and 15O (see also [6]). The timescale for the consumption of the hydrogen in the hot

CNO cycles is given by

tCNO = ECNO

$HCNO

! 1000

ZCNO

(s) (9)

withECNO = 4.51"1018 erg g#1 (forXH = 0.7). This corresponds to a timescale of about one

day for hydrogen consumption in solar metalicity material (Z$ = 0.02, ZCNO = 0.72 · Z$).Similarily, for the second CNO cycle (see figure 6) at higher temperatures the

proton capture rate on 17F exceeds its !-decay rate and the second hot cycle emerges,16O(p, " )17F(p, " )18Ne(!+%) 18F(p, &)15O. This cycle is again limited by the drip line because19Na is proton unbound. The conversion time in the cycle and the energy generation is again

temperature independent and is determined by the !-decay lifetime of the waiting point isotope18Ne (t1/2 = 1.67 s).

The thermonuclear runaway in novae is driven by the energy release of the hot CNOcycles.

The abundance distribution in the ejecta depends on the associated nucleosynthesis [23–25].

Figure 7 shows as an example the variation with time of temperature and density in the deepest

hydrogen rich zone of the accreted envelope during the thermonuclear runaway [32]. The

corresponding nucleosynthesis of CNO material is shown in figure 8. One can easily observe

the rapid depletion of the initial 16O and the build up of the waiting point nuclei. After a

relatively short time the initial abundances have changed to 14O, 15O and 18Ne which are

enriched due to their slow !-decay. Because the peak temperatures in the thermonuclear

runaway are typically below 3.5"108 K [32], break-out is inhibited due to the limited reactionrates for the break-out processes to be discussed in later sections. Indeed, observation of the

abundance distribution in nova ejecta indicate large overabundances of nitrogen [36] produced

by the slow !-decay of the highly enriched 14O and 15O isotopes.

Wiescher et al., JPG, 25:R133 (1999)

Breakout from CNO-cycles:14O(α, p)17F15O(α, γ)19Ne18Ne(α, p)21Na

Resonant reaction rate:

(2J + 1)ΓinΓout

Γtotexp(− Er

kBT)

Gamow-window: 0.7–2.0 MeVresonance energy fortemperatures of 0.5–1.5 GK.

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

ObservationsReactions

Reaction rates for Novae and X-ray bursters

The CNO and Hot-CNOcycles.

Build-up of waiting-pointnuclei in novae:

14O15O18Ne

Topical review R143

Figure 6. The figure shows the characteristic hot (or !-limited) CNO cycles which contribute tothe energy generation in explosive hydrogen burning scenarios like novae and x-ray bursts.

cycle). The timescale for the fusion of four hydrogen nuclei to helium and subsequently the

associated energy generation is determined by the lifetimes of 14O (t1/2 = 70.59 s) and 15O

(t1/2 = 122 s) and is therefore temperature independent. These isotopes represent waiting

points along the nucleosynthesis path. Figure 5 indicates that the energy generation by the

CNO cycles turns flat at the temperature and conditions where the slowest proton capture

rate (14N(p, " )15N) exceeds the !-decay rates for 14O and 15O. These !-decay limitations fix

the energy production rate adopting a cycle time of # ! 200 s and a total energy release of

QCNO = 26.7 MeV to

$HCNO = 4.6" 1015ZCNO (erg g#1 s#1) (8)

whereZCNO is the mass fraction of the CNOmaterial and!50% of the CNOmaterial is storedin 14O and 15O (see also [6]). The timescale for the consumption of the hydrogen in the hot

CNO cycles is given by

tCNO = ECNO

$HCNO

! 1000

ZCNO

(s) (9)

withECNO = 4.51"1018 erg g#1 (forXH = 0.7). This corresponds to a timescale of about one

day for hydrogen consumption in solar metalicity material (Z$ = 0.02, ZCNO = 0.72 · Z$).Similarily, for the second CNO cycle (see figure 6) at higher temperatures the

proton capture rate on 17F exceeds its !-decay rate and the second hot cycle emerges,16O(p, " )17F(p, " )18Ne(!+%) 18F(p, &)15O. This cycle is again limited by the drip line because19Na is proton unbound. The conversion time in the cycle and the energy generation is again

temperature independent and is determined by the !-decay lifetime of the waiting point isotope18Ne (t1/2 = 1.67 s).

The thermonuclear runaway in novae is driven by the energy release of the hot CNOcycles.

The abundance distribution in the ejecta depends on the associated nucleosynthesis [23–25].

Figure 7 shows as an example the variation with time of temperature and density in the deepest

hydrogen rich zone of the accreted envelope during the thermonuclear runaway [32]. The

corresponding nucleosynthesis of CNO material is shown in figure 8. One can easily observe

the rapid depletion of the initial 16O and the build up of the waiting point nuclei. After a

relatively short time the initial abundances have changed to 14O, 15O and 18Ne which are

enriched due to their slow !-decay. Because the peak temperatures in the thermonuclear

runaway are typically below 3.5"108 K [32], break-out is inhibited due to the limited reactionrates for the break-out processes to be discussed in later sections. Indeed, observation of the

abundance distribution in nova ejecta indicate large overabundances of nitrogen [36] produced

by the slow !-decay of the highly enriched 14O and 15O isotopes.

Wiescher et al., JPG, 25:R133 (1999)

Breakout from CNO-cycles:14O(α, p)17F15O(α, γ)19Ne18Ne(α, p)21Na

Resonant reaction rate:

(2J + 1)ΓinΓout

Γtotexp(− Er

kBT)

Gamow-window: 0.7–2.0 MeVresonance energy fortemperatures of 0.5–1.5 GK.

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

ObservationsReactions

Measurements of 18Ne(α, p)21Na reaction

Direct measurements of 18Ne+α

reaction.Resonances more than 1.8 MeV aboveα threshold in 22Mg.

Bradfield-Smith et al., PRC, 59:3402 (1999)Groombridge et al., PRC, 66:055802 (2002)

Shotter et al., TRIUMF-EEC S870 (2000)

Corresponding to Gamow-window fortemperatures of 1.2 GK or more.Reaction cross sections down by 7orders of magnitude for 0.5 GK.

Indirect measurement by identificationof contributing 22Mg levels.

12C(16O,6He)22Mg.Chen et al., PRC, 63:065807 (2001)

21Na(p,p’)21Na.Jenkins et al., TRIUMF-EEC S1105 (2006)

A. Tuff, P19, IoP-NPC (2009)21Na(p,α)18Ne.

Aliotta et al., TRIUMF-EEC S1103 (2006)

Chen et al., PRC, 63:065807 (2001)

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

ObservationsReactions

Measurements of 18Ne(α, p)21Na reaction

Direct measurements of 18Ne+α

reaction.Resonances more than 1.8 MeV aboveα threshold in 22Mg.

Bradfield-Smith et al., PRC, 59:3402 (1999)Groombridge et al., PRC, 66:055802 (2002)

Shotter et al., TRIUMF-EEC S870 (2000)

Corresponding to Gamow-window fortemperatures of 1.2 GK or more.Reaction cross sections down by 7orders of magnitude for 0.5 GK.

Indirect measurement by identificationof contributing 22Mg levels.

12C(16O,6He)22Mg.Chen et al., PRC, 63:065807 (2001)

21Na(p,p’)21Na.Jenkins et al., TRIUMF-EEC S1105 (2006)

A. Tuff, P19, IoP-NPC (2009)21Na(p,α)18Ne.

Aliotta et al., TRIUMF-EEC S1103 (2006)

Chen et al., PRC, 63:065807 (2001)

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

Deuteron transferTIGRESS

SHARC

The 18Ne(α, p)21Na Hot-CNO breakout reaction

Indirect measurement by identification ofcontributing 22Mg levels.Populated through 20Na(6Li,4He)22Mg∗.

(2J + 1)ΓαΓp

Γtotexp(− Er

kBT)

Er , Jπ: Measured.

Γα: Inferred from mirror levels.

Complete kinematics – coincidentmeasurement of energies and angles of:

Residual α particle from transfer.

Secondary proton emission:22Mg∗(,p)21Na∗.

Subsequent γ decay of 21Na∗.

Requires combination of:

γ spectrometer.

Highly-segmentedcharged-particle array,large angular coverage.

Accelerated 20Na beam(3–5 MeV/u).

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

Deuteron transferTIGRESS

SHARC

The 18Ne(α, p)21Na Hot-CNO breakout reaction

Indirect measurement by identification ofcontributing 22Mg levels.Populated through 20Na(6Li,4He)22Mg∗.

(2J + 1)ΓαΓp

Γtotexp(− Er

kBT)

Er , Jπ: Measured.

Γα: Inferred from mirror levels.

Complete kinematics – coincidentmeasurement of energies and angles of:

Residual α particle from transfer.

Secondary proton emission:22Mg∗(,p)21Na∗.

Subsequent γ decay of 21Na∗.

Requires combination of:

γ spectrometer.

Highly-segmentedcharged-particle array,large angular coverage.

Accelerated 20Na beam(3–5 MeV/u).

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

Deuteron transferTIGRESS

SHARC

The 18Ne(α, p)21Na Hot-CNO breakout reaction

Indirect measurement by identification ofcontributing 22Mg levels.Populated through 20Na(6Li,4He)22Mg∗.

(2J + 1)ΓαΓp

Γtotexp(− Er

kBT)

Er , Jπ: Measured.

Γα: Inferred from mirror levels.

Complete kinematics – coincidentmeasurement of energies and angles of:

Residual α particle from transfer.

Secondary proton emission:22Mg∗(,p)21Na∗.

Subsequent γ decay of 21Na∗.

Requires combination of:

γ spectrometer.

Highly-segmentedcharged-particle array,large angular coverage.

Accelerated 20Na beam(3–5 MeV/u).

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

Deuteron transferTIGRESS

SHARC

TIGRESS detectors

TIGRESS: TRIUMF-ISAC Gamma-RayEscape-Suppressed Spectrometer:

Array of 8-12 HPGe γ detectors.

4 crystals with segmented contacts.

Doppler corrected energies fromposition measurement.

Efficiency: 15–20% at 332keV, less athigher energies. Assume 10 % asaverage value.

Schumaker et al., NIMA, 570:437 (2007)Svensson et al., JPG, 31:S1663 (2005)

21Na states: 332, 1726, 2434, 2798 and 2829 keV.Possible γ rays: 332, 373, 1113, 1384 and 2434 keV.

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

Deuteron transferTIGRESS

SHARC

SHARC array

SHARC: Silicon Highly-segmentedArray for Reactions and Coulex:

Upstream and downstream CDs and boxdetectors in compact configuration aroundreaction target.

Angular coverage: ≈ 50 %.

Angular resolution:δθ = 1.6 deg, δφ = 3.5 deg.

Segmentation: ≈ 10,000 pixels

Energy ranges: 12 MeV, 25 MeV.

Energy resolution: ≈ 40 keV.

Particle identification from δE-E atforward angles.

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

Deuteron transferTIGRESS

SHARC

Indirect measurement of 18Ne(α, p)21Na

α particles from20Na(6Li,α)22Mg∗ at backwardangles.

Protons from 22Mg∗(,p)21Na atforward angles.

Complete 3-body kinematicsfrom missing momentum

Reconstructed 22MgenergyBackground reduction

22Mg spin from p-α correlations.Rae et al., PLB, 156:167 (1985)

Fulton et al., PLB, 267:325 (1991)Freer, NIMA, 383:463 (1996)

0 10 20 30 40 50 60 70

0 20 40 60 80 100 120 140 160 180

E_kin

(MeV

)

Theta (Deg)

22Mg(8MeV)22Mg(10MeV)

20Na(gs)alpha [22Mg(8MeV)]

alpha [22Mg(10MeV)]6Li [20Na(gs)]

0

2

4

6

8

10

12

0 10 20 30 40 50 60 70

E_kin

(MeV

)

Theta (Deg)

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

Summary and status

Indirect measurement:18Ne(α,p)18Ne Hot-CNObreakout reaction.

Through20Na(6Li,α)22Mg(,pγ)21Nad-transfer.

Coincidence measurementof α-p-γ.

TIGRESS (8-12 detectors):Available.

Silicon detectors: 2 delivered.

Silicon detector preamplifiers:7 assembled.

TIGRESS DAQ-upgrade(TIG-64): Spring 2009.

Stable beam commissioning:4th–7th June 2009.

First RIB experiment: 6th–16th

August 2009.Catford et al., TRIUMF-EEC S1107 (2006)

G. Wilson, P22, IoP-NPC (2009)

20Na(6Li,α): Spring 2010.

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

Summary and status

Indirect measurement:18Ne(α,p)18Ne Hot-CNObreakout reaction.

Through20Na(6Li,α)22Mg(,pγ)21Nad-transfer.

Coincidence measurementof α-p-γ.

TIGRESS (8-12 detectors):Available.

Silicon detectors: 2 delivered.

Silicon detector preamplifiers:7 assembled.

TIGRESS DAQ-upgrade(TIG-64): Spring 2009.

Stable beam commissioning:4th–7th June 2009.

First RIB experiment: 6th–16th

August 2009.Catford et al., TRIUMF-EEC S1107 (2006)

G. Wilson, P22, IoP-NPC (2009)

20Na(6Li,α): Spring 2010.

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction

Classical novaeIndirect reaction study

Summary

Collaboration for 20Na(6Li,α)22Mg

C. Aa. Diget(1), R. A. E. Austin(2), G. Ball(3), C. Beer(1), J. Blackmon(4),A. J. Boston(5), H. C. Boston(5), W. N. Catford(6), A. A. Chen(7), J. Chen(7),

M. Djongolov(3), H. al Falou(2), S. P. Fox(1), B. R. Fulton(1), A. Garnsworthy(3),G. Hackman(3), D. G. Jenkins(1), R. Kanungo(2), R. L. Kozub(8), A. M. Laird(1),

L. Linhardt(4), M. Matos(4), P. J. Nolan(5), C. Ouellet(7), S. V. Rigby(5),C. Ruiz(3), F. Sarazin(9), K. Setoodehnia(7), M. Taggart(1), S. Triambak(3),

S. Williams(3), G. Wilson(6)

(1)Department of Physics, University of York, UK(2)Department of Astronomy and Physics, St. Mary’s University, Canada

(3)TRIUMF, Vancouver, Canada(4)Department of Physics and Astronomy, Louisiana State University, USA

(5)Department of Physics, University of Liverpool, UK(6)Department of Physics, University of Surrey, UK

(7)Department of Physics and Astronomy, McMaster University, Canada(8)Physics Department, Tennessee Technological University, USA

(9)Physics Department, Colorado School of Mines, USA

C. Aa. Diget The 18Ne(α,p)21Na Hot-CNO cycle breakout reaction