FRIB Workshop/Nov.2008. 112 Sn FRIB Workshop/Nov.2008

FRIB Workshop/Nov.2008

ωh2

2∑ irωh3

1

3Yri∑

⟩⟨=

2rm

KE AGMR h ⟩⟨

+=

2

2527

3

7

rm

KE

FA

ISGDR

εh






112Sn



From EGMR and EISGDR to K∞

><=

2

2

rm

KE AGMR

h

342

2

31 −−

∞ +⎟⎠

⎞⎜⎝

⎛ −++= AZK

AZNKAKKK cousymsurA

However, the available GMR data can lead to a wide range of values for K∞ (100--500 MeV!)So, "microscopic approach":

Select "suitable" effective interactions.

Calculate the GMR strength distributions in an RPA approach

Compare with the experimental EGMR and EISGDR

K∞


This number is consistent with both GMR and ISGDR Data and with non-relativistic and relativistic calculations



Excitation energy spectra at 0 deg





112 114 116 118 120 122 12414

15

16

17

This work Colo Piekarewicz Texas A& M

m1/m0 (MeV)

A

Why are tins so “Fluffy”?





K = -500 (50)


Data from H. Sagawa et al., Phys. Rev. C 76, 034327 (2007)Data from H. Sagawa et al., Phys. Rev. C 76, 034327 (2007)


G. Colo’s talk on Saturday


G. Colo’s talk on Saturday


Towards very neutron-rich nuclei

K

Kcore and Kskin

“soft GMR” akin to pigmy GDR’s.

Need inverse reactions2H, 4He, or 6Li targetsbeams of 35-100 MeV/A

First experiment performed at

GANIL

56Ni + 2H, with active target MAYA


MAYA

Drift

chamberMoving flap

Si wall

CsI wall

Diamond

Ionization

chamber

Au foil

MAYA @ GANIL


d break-up

# co

unts

/MeV

C. Monrozeau et al., Phys. Rev. Lett. 100, 042501 (2008)

58Ni (d, d’)

MAYA @ GANIL


Analysis with Gaussian fits


Multipole Decomposition Analysis



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FRIB Workshop/Nov.2008. 112 Sn FRIB Workshop/Nov.2008