David Lunney – CSNSM (IN2P3/CNRS) – Université de Paris Sud, Orsay
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•
•
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masses in the cosmos
measurement programs
comparisons
mass models
facing the challenge
Nuclei in the Cosmos – IX
25-30 June 2006
CERN, Geneva
Some introductory remarks on history
High resolution mass spectrographs
F.W.Aston (~1920‘s): 212 isotopes discovered
Packing fraction
E = mc2
How the sun shines,”
J. Bahcall
http://nobelprize.org/physics/
A. Eddington (~1920)
Stellar combustion
Motivation from “fundamental” physics
metrology:
the kilogram: 28Si atomic mass standard
and other fundamental constants
(what if they vary with time?!)
nuclear structure from the mass surface
nuclear structure from the mass surface
stable isotopes
s-process path
r-process path
b - decay path
known masses
Stellar Nucleosynthesis
(A  200)
p-isotope
s-isotope
r-isotope
At
Po
Bi
Pb
Tl
Hg
Au
Pt
Ir
Os
Re
W
Ta
Hf
Lu
Yb
Tm
Er
b decay
one / two
b -delayed
neutron decay
neutron number
126
Techniques
Direct
(energy)
(mass spectrometry)
time of flight:
TOF = (m/q) (L/Br )
FIFS
(MeV)
gas cell
RFQ
decays:
AB+a
Qa = MB- MA
cyclotron frequency:
fc = qB/m
ISOL
(keV)
‘the best of both worlds’
better precision
reactions:
A(a,b)B
Q = MA+ Ma- Mb- MB
PRODUCTION
SCHEME
better sensitivity
Indirect
UW-PTMS
FSUTRAP
(MIT)
SPEG
CSS2
(GANIL)
ISOLTRAP (CERN)
MISTRAL (CERN)
ESR-FRS (GSI)
mass measurement programs at GANIL
CSS1
SPEG
time-of-flight
+ magnetic rigidity
m = q Br T / L
Y
Z
Z
X
Y
X
SPEG
Resolving power: 104
extremely sensitive
H. Savajols et al., EPJ A 25 (2005) 23
and B. Jurado et al., submitted (2006)
mass measurement programs at GANIL
CSS2
time-of-flight:
phase difference
with acceleration
(longer flight path)
M. Chartier et al.,
J. Phy. G 31 (2005) S1771
CSS1 CSS2
mass measurement programs at GANIL
CIME (SPIRAL)
time-of-flight:
variable RF
acceleration
(longer flight path)
M.-B. Gomes Hornillos et al.,
J. Phy. G 31 (2005) S1869
mass measurement programs at GSI
Experimental Storage Ring:
D(m/q)/(m/q) = Dv/v (gt2 - g2) - Df/f gt2
Schottky Mode
very precise
but cooling slow
Isochronous Mode
very fast
but not as precise
Yu. Litvinov, Ph.D. (2003):
~ 600 species in the ring
466 masses measured
(117 calibration masses)
139 masses from links
200 improved masses
75 new mass values
Yu. Novikov et al.,
Nucl Phys A (2002)
SMS 2002
E. Kaza, Ph.D
(2004)
Yu. Litvinov
et al., (2005)
IMS
J. Stadlmann (Ph.D)
and
Phys. Lett. B
(2004)
IMS 2002
M. Matos, Ph.D
(2004)
see talk of
F. Bosch
Booster
1.4 GeV
PS
Linac2
50 MeV
ISOLTRAP
10 m
REX-ISOLDE
GPS
HRS
ISOLDE
CERN, Geneva
MISTRAL
Quadrupole
Doublet
ISOLDE
Beam
Reference
Source
25120
25100
Alburger 78
*
MISTRAL 2005
1m
Mass Excess (keV)
MISTRAL
COLETTE
Paul trap
25080
25060
25040
Detector
12Be
(T1/2 = 21 ms)
25020
* D.E. Alburger et al. Phys. Rev. C 18, 2727 (1978)
The mass spectrometer ISOLTRAP
see talk of A. Herlert
hyperbolic
Penning trap:
precision mass
measurement
cylindrical
Penning trap:
isobar separation & cooling
1m
2 cm
20
cm
low energy bunches
continuous
60 keV
ISOLDE beam
Gas-filled RF-Paul trap:
universal beam
collector
TITAN (TRIUMF)
(RIKENRING)
CPT (ANL)
LEBIT (NSCL)
JYFLTRAP
SMILETRAP (MSI)
ISOLTRAP (CERN) SHIPTRAP (GSI)
MATS (FAIR)
MAFFTRAP
or “what ISOLTRAP hath wrought”
Canadian Penning Trap (CPT) facility at ANL
- 46Ti: Savard et al., PRL (2005)
(not available from ISOLDE)
See poster here.
46V
beam
JYFLTRAP at the Jyväskylä IGISOL
trap
cooler
cooler
mass
separator
ISOLDE elements
IGISOL elements
See poster of A. Jokinen
ion
guide
SHIPTRAP facility at GSI
ISOL facility for
transuranium nuclides

92Mo (58Ni,xpyn) 147Ho
new masses for 147Ho, 147,148Er (10-6)
(M. Block et al., ENAM04) see poster here
Low Energy Beam & Ion Trap (LEBIT) facility at NSCL/MSU
G. Bollen et al., PRL 96 (2006)
http://www.nscl.gov/lebit
TOF stop
TOF start
K500
S800
ha
r
e
f
s
tran
ll
Br meas.
10m
K1200
A1900
dE [a.u.]
1000
86Kr
primary beam
Ge
Ga
Zn
Cu
800
M. Matoš (CGS-12, Notre Dame)
AIP Conf. Proc. 819 (2006) 164
See poster of A. Estrade
Ni
Co
Fe
Mn
Cr
V
Ti
Sr
Ca
K
Ar
Cl
S
600
400
200
20
30
40
DTOF[ns]
50
60
70
postaccelerator
magnet
target
cyclotron
10
-4
relative uncertainty
SPEG
10
10
-5
ESR
SMS
1995
-6
ESR
IMS
ESR
SMS
1997
CSS2
MISTRAL
10
-7
ISOLTRAP
10
-8
10
-9
0
1
2
3
4
relative isobaric distance from stability
Reviews of Modern Physics, 75 (2003) 1021
relative uncertainty
10
-4
10
-5
10
-6
CSS2
ESR
IMS
SPEG
ESR SMS
MISTRAL
10
-7
10
-8
10
-9
CPT
ISOLTRAP
0
1
2
3
4
relative isobaric distance from stability
ENAM04 Proc., Eur. Phys. J. A, 25 (2005) 3
relative uncertainty
10
-4
10
-5
10
-6
(CSS2)
(ESR
IMS)
ORNL
MISTRAL
(ESR SMS)
10
SPEG
JYFLTRAP
-7
SHIPTRAP
10
-8
10
-9
ISOLTRAP LEBIT
CPT
0
1
2
3
4
relative isobaric distance from stability
Proc. Nuclei in the Cosmos IX, PoS (2006) ?
10
Performance of the various methods
-4
relative uncertainty
SPEG
10
-5
10
-6
ESR
IMS
CSS2
JYFL COOL
MISTRAL
ESR SMS
10
-7
10
-8
10
-9
CPT
ISOLTRAP

10
6
10
3
10
0
half life (seconds)
See: Lunney, Pearson & Thibault, Rev. Mod. Phys. 75 (2003) 1021
10
-3
relative uncertainty
10
-4
10
-5
10
-6
neutron-rich
proton-rich
(ESR
IMS)
(CSS2)
SPEG
ORNL
MISTRAL
(ESR SMS)
10
-7
JYFLTRAP
SHIPTRAP
ISOLTRAP
10
-8
CPT
LEBIT
10
-9
-20
-10
0
10
20
30
(left) neutron- (right) proton-separation energy (MeV)
stable
indirect
100
GANIL
SPEG
CSS2
80
GSI
ESR-SMS
ESR-IMS
SHIPTRAP
proton dripline
(FRDM95)
ISOLDE
MISTRAL
ISOLTRAP
Z
60
neutron dripline
(FRDM95)
40
Other Penning traps
CPT (ANL)
LEBIT (MSU)
JYFLTRAP
20
0
0
50
100
N
150
MAFF facility at FRM-II
trap
Münich Accelerator for Fission Fragments
funnel
Bavarium
n-rich nuclides
D. Habs et al., ENAM 2004
(MAFF workshop 04/2005)
trap
TRIUMF Ion Trap (TITAN) facility
EBIT
Rapid charge
breeding (2-30 ms)
Wien filter
m/q selection
fc = qB/m
Paul trap
Cooling and
Mass measurements
Bunching (1-5ms)
Penning trap
Precision mass measurement
(~ 10-100ms)
ISAC
beam
• T1/2 ≈10 ms
•m/m < 110-8
•Operational 2006
J. Dilling et al. ENAM04
Beyond the horizon
Beyond the horizon
FAIRTRAP
(MATS)
GSI ’s future
Facility for
Antiproton and
Ion Research
(FAIR)
FAIR RINGS
(ILIMA)
stable nuclei
nuclides with known masses
G.Audi et al., Nucl. Phys. A729 (2003) 3
to be
be measured
measured with
with FAIR
the FRS-ESR
to
facility
measured with FRS-ESR
observed nuclei
observed nuclei
82
r-process
126
50
82
28
50
20
8
28
20
8
stellar nucleosynthesis
The atomic mass evaluation*
Not a compilation !
S
P
Si
Al
16
15
14
13
27Al
(p,g) 28Si
28Si (3He,8Li) 23Al
28Si (4He,8He) 24Si
28Si (p,t) 26Si
28Si (p,n) 28P
28Si
(d,p) 29Si
28Si (p,g) 29P
28Si (+,-) 28S
31P (p,a) 28Si
and 28Si / 12C
10 11 12 13 14 15 16
* G. Audi and A.H. Wapstra, Nuclear Physics 1988, 1993, 1995, 2003
The Mass Evaluation
.
.
.
28Si
.
.
.
. . . 28Si . . .
.
.
.
=
1
.
.
.
least squares mass adjustment (1993)
•
•
•
•
•
5520 experimental data (186 rejected)
plus 601 estimated data
3652 equations; 3017 parameters
1920 ground state masses
plus 730 recommed values
Audi-Wapstra mass table
A simplified overview of mass models
physics input
algebraic
formulas
(Garvey-Kelson; IMME)
microscopic
sculpturings of a
macroscopic blob
microscopic
nucleon-nucleon
interaction
(FRDM)
(RMF / HFB)
ease of use
now full HFB
Extended Thomas-Fermi Strutinki Integral model
macro: TF Skyrme approximation
micro: Strutinski correction (folded Skyrme)
9 parameters
good mass fit
most nuclear properties
HFBCS:
HFB 1:
HFB 2:
HFB 3:
HFB 4-7:
HFB 8:
HFB ...
S. Goriely et al., At. Nuc. Data (2001)
M. Samyn et al., Nucl. Physics (2002)
S. Goriely et al., Phys. Rev. C (2002)
M. Samyn et al., Nucl. Physics (2003)
S. Goriely et al., Phys. Rev. C (2003)
M. Samyn et al., Phys. Rev. C (2004)
Fit to 1995 AME (1768 masses)
15+4
15+4
18+4
19+12
34+81
21+12
28
mass data parameters
+ other data parameters
0.8
local models
0.6
0.5
0.4
0.3
0.2
0.1
Chaos-limited mass prediction?
Only 60%
masses fit
LZ
JM
G
K
NS
KU
TY
DZ
CS
-1
HF
B1
HF
B2'
FR
D
M
TF
-F
R
DM
0
HF
B
rms error (MeV)
0.7
mass model comparisons
D. Lunney et al., ENAM 1995 (Arles)
From: D. Lunney,
“Nuclear masses:
Experimental programs,
theoretical models and
astrophysical interest,”
p. 296
Conclusions
Mass Measurements
higher performance;
programs multiplying
 more data,
better quality
Mass Evaluation
global benchmark
(last judgement)
Mass Models
microscopic era;
real need for data
(diagnostic tool)
“A false balance is
abomination to
the Lord:
but a just weight
is his delight.”
— Proverbs 11.1
Lichtenberg:
To find something new,
must build something new.
“The construction of the universe is certainly
much easier to explain than that of a plant”.
Kierkegaard:
I must find a truth
that is true for me.