Nuclear astrophysical reactions by unstable beams and progress of brif and brifii
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Wei-ping Liu 柳卫平 [email protected] China Institute of Atomic Energy, CIAE 中国原子能科学研究院 PowerPoint PPT Presentation


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Nuclear astrophysical reactions by unstable beams and Progress of BRIF and BRIFII 不稳定核束核天体物理反应 北京放射性核束装置的进展. Wei-ping Liu 柳卫平 [email protected] China Institute of Atomic Energy, CIAE 中国原子能科学研究院 6 th China Japan Joint Nuclear Physics Symposium 第六届中日核物理会议 May 16-20, 2006 Shanghai 上海.

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Wei-ping Liu 柳卫平 [email protected] China Institute of Atomic Energy, CIAE 中国原子能科学研究院

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Nuclear astrophysical reactions by unstable beams and progress of brif and brifii

Nuclear astrophysical reactions by unstable beams andProgress of BRIF and BRIFII不稳定核束核天体物理反应北京放射性核束装置的进展

Wei-ping Liu 柳卫平

[email protected]

China Institute of Atomic Energy, CIAE 中国原子能科学研究院

6th China Japan Joint Nuclear Physics Symposium

第六届中日核物理会议

May 16-20, 2006

Shanghai 上海


Study of some key nuclear astrophysical reactions by unstable nuclear beams

Study of some key nuclear astrophysical reactions by unstable nuclear beams


Interplay between astrophysics and nuclear physics

Interplay between astrophysics and nuclear physics

Exp

Exp

The

The

Astro. Model

Nucl. Data

Astro. Obs.

Abundance Dist.

  • Nuclear process

    • Main energy of star to balance gravitational collapse

    • Mechanism of isotope synthesis apart from Hydrogen

    • Rule the evolution process from the first few minutes after big bang to just before the end of star life

  • Nuclear astrophysics

    • Using nuclear physics to explain the energy production and element synthesis in star and cosmos


Nuclear astrophysics and physics of unstable nuclei

Nuclear astrophysics and physics of unstable nuclei

  • primordial and super novae high temperature and density environment, large amount of unstable nuclear involved into nuclear burning

RIKEN RIBF proposal


Nuclear astrophysics lab

Nuclear astrophysics ‘Lab’

B. Pfeiffer, et al., Z. Physik A357, 253 (1997)


Reaction network

Reaction network

b

g

Cross section

Decay half-life


Challenge to experiment

Challenge to experiment

11C(p,)12N

  • Gamow window

  • Extremely low energy

  • Vanishing low cross section


Our solution indirect method

Our solution: indirect method

RIB production

(d,n) or (d,p) measurement

W.P. Liu, NIM B204(2003)62

W.P. Liu, PRL77(1996)611

Astrophysical reaction rates

ANC or Spec factor


Direct capture process of 11 c p g

Direct capture process of 11C(p,g)

  • Key reaction in hot pp chain

  • Dominated by direct capture

N. C. Shu,…, W. P. Liu et al., Nucl. Phys. A 758 (2005) 419c

W. P. Liu et al., NPA728(2003)275


First measurement of primordial 8 li n g 9 li reaction rate

First measurement of primordial 8Li(n,g)9Li reaction rate

  • Destroy reaction of 8Li: 8Li(n,g)9Li, 8Li(d,p)9Li in inhomogeneous big bang,APJ429(1994)499

  • Half-life of 8Li: 0.83 s,direct (n,g) exp. impossible

Z. H. Li, W.P. Liu et al.,PRC 71, 052801(R) (2005)


Comment on our results

Comment on our results

  • The paper presents excellent experimental work and removes a longstanding debate about the absolute cross section of 8Li(n,g)

  • As far as I know, so far, no results have been published to determine a neutron capture rate of astrophysical importance


13 n d n 14 o 13 n p g 14 o

13N(d,n)14O13N(p,g)14O

PRC, submitted


Summary of reaction studied

Summary of reaction studied

18Ne

17F

14O

12N

9C


Opportunities from brif and brif ii

Opportunities from BRIF and BRIF II

BRIF: Beijing Radioactive Ion Facility


Physics why brif

Physics : why BRIF

Intensity 1-109, energy 100 keV-10 MeV/u, RIA proposal


The current tandem lab

The current Tandem lab

  • Beam type, only stable, no noble gas

  • Energy range, less than 14 MeV/q

  • Instrumentation, no RMS, no ISOL

  • Beam time: 100 % overdue


Wei ping liu wpliu iris ciae ac china institute of atomic energy ciae

BRIF

100 MeV 200 mA compact proton cyclotron

20000 mass resolution ISOL, 2 MeV/q super-conducting LINAC


Brif energy and mass resolution

BRIF energy and mass resolution


Brif research opportunities and combinations

BRIF research opportunities and combinations

  • 100 MeV neutron

  • ISOL

  • current terminals

  • limitation of instrument and machine time

  • Tandem with unstable beam, proton-rich, fission

  • heavy ion beam with higher beam energy, 20 MeV/q

  • 100 MeV proton and neutron beams

  • available by the year 2010

Ion Source

Stable Beam

100 MeV, 200 mA

Proton Cyclotron

ISOL

Mass Resolution

20000

Tandem

Accelerator

15 MV

Super

Conducting

LINAC

RIB

Nuclear data

Radiation physics

Nuclear structure

Reaction

Astrophysics

Atomic Physics

Applications

Radiation physics

Nuclear structure

Reaction

Astrophysics

Atomic Physics

Decay data

Material physics

Neutron data

Radiation physics


More n rich beam carrisol

More n-rich beam: CARRISOL

  • Horizontal tube

  • He-jet + ISOL

  • Neutron flux 1X1014 /cm2/s

  • Available in 2007


Wei ping liu wpliu iris ciae ac china institute of atomic energy ciae

Low b RFQ for new injector

17 MeV/q super-conducting LINAC

RMS

Large acceptance spectrometer

Decay measurements


Beam energy

Beam energy


Rfq dtl

RFQ/DTL

36MHz

Low energy normal temp RFQ+ finger type DTL, multi charge heavy ion beam up to the energy accepted by SC LINAC


Sc linac

SC LINAC

QWR

  • Energy gain 17 MeV/q

  • 36 ¼ wave length QWR

  • 9 100 L LHe tank

LHe tank


Large acceptance spectrometer

Large acceptancespectrometer

  • Large D Q + detectors

  • Mass range 100-200,energy 5-10 MeV/u

  • Solid angle 80 mSr,P acceptance 10%

  • Mass resolution 300 via TOF and tracking


Wei ping liu wpliu iris ciae ac china institute of atomic energy ciae

RMS

12 m

Quadruples

Quadruples

Dipole

Electro

Deflector

Electro

Deflector

Target

chamber

Detector

chamber

Beam

diagnostics

Beam

diagnostics


Gamma array

Gamma array

  • 10X BGO+seg. HPGe

  • Eff. 10 % @ 1 MeV

  • resolution 6 keV


Research opportunities

Research opportunities

  • Systematic study of shell evolution

  • Nuclear astrophysics

  • Mechanism of SHE

  • Properties of medium mass neutron rich nuclei

  • New decay modes

  • Gamma array

  • Recoil mass separator

  • Large acceptance spectrometer

  • Decay setup


Conclusion

Conclusion

  • BRIF and BRIFII will open up exciting research opportunities

  • With BRIFII:

    • new experimental terminals

    • higher beam energy of 35 MeV/q

    • 100 % more beam time by separate operation

    • Limit: overall instrumentation usage

    • Available by the year of 2013

  • Chances are still open, and we welcome contributions, suggestions and new proposals

  • We would like to collaborate with major domestic and foreign research groups and world labs to take their full research potential and to do cooperative jobs

  • Call for user communities to build machine and detector and physics task force with more flexible way

  • A nice play ground in Beijing to connect locations


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