JUSTUS-LIEBIG- Stefan Schippers I M P UNIVERSITÄT · 0 10 20 30 40 50 60 70 80 90 10-6 10-4 10-2...

Storage-ring measurements of hyperfine-induced

and two-photon transition rates

in berylliumlike ions

Stefan Schippers

Institut für Atom- und Molekülphysik

JUSTUS-LIEBIG- UNIVERSITÄT GIESSEN

I M PA

www.uni-giessen.de/cms/iamp

Outline

1. Motivation • hyperfine quenching of ns np 3P0 states in divalent atoms and ions

• theoretical and experimental results

• some applications

2. Experiments at heavy-ion storage rings • lifetime measurements

• electron-ion recombination

3. Hyperfine induced 3P0 1S0 transition rate • results for 47Ti18+

• results for 33S12+

4. E1M1 two-photon 3P0 1S0 transition rate • results for 136Xe50+

Stefan Schippers, ICAMDATA 8, Gaithersburg, September 30 - October 4, 2012 2

2s2p 3P – 2s2 1S transitions in Be-like ions

2s2 1S

J=2

J=1

J=0

2s 2p 3P

J=0

ground state

metastable

M2 (medium)

IC (fast)

E1M1 (very slow)

HFI (slow)

hyperfine-interaction

requires

nucleus

with I>0


He-like vs. Be-like ions


Review: W. Johnson, Can. J. Phys. 89 (2011) 429

E1

E1

M1 HFIE1M2

1s2s 1S

0

1s2s 3S

1

1s2p 1P

1

1s2p 3P

2

1s2p 3P

0

1s2p 3P

1

1s2 1S

0

He-like

HFIE1

2s2p 1P

1

2s2p 3P

2

2s2p 3P

1

2s2p 3P

0

2s2 1S

0

E1

M2

Be-like

E1

HFI HFI

Theoretical predictions of 2s2p 3P0 lifetimes

10 20 30 40 50 60 70 80 90

10-5

10-4

10-3

10-2

10-1

100

101

102

103

104

105

106

107

108

109

millisecond

second

minute

hour

year

month

Lifetim

e (

s)

Nuclear charge

E1M1

[Laughlin, PLA 75, 199 (1980)]

HFI [Cheng et al., PRA 77, 052504 (2008)]

day


Ultraprecise optical clocks

Al+ clock transition: 3s 3p 3P0 3s2 1S0

T. Rosenband et al., PRL 98 (2007) 220801


13C/12C abundance ratio in planetary nebulae

R. H. Rubin et al., ApJ 605 (2004) 784

M2

HFI

1S

J=

2 1 0

3P

J=0

IC

shedding light on stellar nucleosynthesis

NGC 2440


„Experimental“ HFI lifetime from a planetary nebula

M2

IC

HFI

istope A=14

rel. abundance 99.63%

nuclear spin I=1

2s2p 3P0 lifetime:

from astrophysical

observation and modeling:

2500800 s

theory:

Brage et al. 2033 s

Marques et al. 7806 s

beryllium-like nitrogen

in the planetary nebula NGC 3918

T. Brage et al., PRL 89 (2002) 281101

1S

J=

2 1 0

3P

J=0


The challenge

measurement of an extremely long lifetime

prediction for the 47Ti18+(2s2p 3P0) state: t = 2.8 s

theory by Marques et al., PRA 47 (1993) 929

needs well defined environment

without significant disturbance

of the long-lived state


The Heidelberg TSR storage ring at MPIK


Decay of excited states

Injection of ions in metastable states

hn

PM

Fe12+(3s2 3p2 1D2)

TSR: Träbert et al.,

JPB 35, 671 (2002)

t = 8.0 ± 0.1 ms

Most photons

miss

the detector!


Electron-ion recombination experiments

e- beam

100% detection efficiency

Aq+ + e- A(q-1)+ + photons

collision experiments with dilute ensembles of particles

tunable relative energy: sub meV to sub MeV

Reaction products

• beams of high directionality

• high particle energies in lab frame


Dielectronic recombination (DR) - viewed as a two-step process -

Ti18+(2s2) + e-

2s

2p

nl

dielectronic

capture (DC)

Ti17+(2s 2p nl)

radiative

stabilization

Ti17+(2s2 2p) + hn

photons


Measuring the 3P0 lifetime using DR as a tool

Idea:

• stored Be-like ion beam contains a 3P0 fraction,

if 3P0 lifetime is sufficiently long (> 1ms)

• 2s 2p 3P0 excitation produces distinct

DR (e.g. 2p2 nl) resonances

• measure the „apparent“ DR resonance strength

as a function of storage time

• deduce 3P0 lifetime


DR of Be-like C2+ - single-pass merged-beams experiment -

N. R. Badnell et al., J. Phys. B 24 (1991) 4441

A

B

C

Resonances of the types

A: 2s2 1S 2s 2p 1P nl

B: 2s 2p 3P 2s 2p 1P nl

C: 2s 2p 3P 2p2 3P nl

mixture

of 75% 2s 2p 3P

and 25% 2s2 1S

in the ion beam


DR spectrum of Be-like 48Ti18+

0 10 20 30 40 50 60 70 80

0

2

4

6

8

10 2p2 1S

1 nl series

2p2 3P

012 nl series

2p2 1D

2 nl series

n=11

2s 2p 3P

0 nl series

2s 2p 3P

1 nl series

2s 2p 3P

2 nl series

Recom

bin

ation r

ate

coeff. (1

0-9 c

m3 s

-1)

Electron-ion collision energy (eV)

2s 2p 1P

1 nl series

n=8

S. Schippers et al., JPCS 58 (2007) 137

A

Where are

series

B and C?


Why are 3P0 resonances missing?

0

1

2

3

4

5

6

7

8

3P

1 c

on

tin

uu

m

3P

0 c

on

tin

uu

m

1S

0 c

on

tin

uu

m

3P

1

3P

2

Energ

y r

ela

tive to 3

P0 level (e

V)

3P

0

resona

nce

sta

tes

resonance states above the 3P1 level have an additional

autoionization decay channel

Look for resonances

at low relative energies!


Ti18+ DR spectrum at low energies

0

1

2

Recom

b. ra

te c

oeff. (1

0-9cm

3 s

-1)

A=48

0.70 0.75 0.80 0.85 0.900

1

2A=47


AUTOSTRUCTURE

5% 3P0: (2s 2p 1P1) 11d

(2s 2p 3P2) 26l

95% 1S0: (2s 2p 3P) 11p

11f

RR

A=47

A=48

Next step: measure

recombination

signal vs. time

S. Schippers et al., JPCS 58 (2007) 137


0 2 4 6 8200

400

600

800

1000

0 50 100 15010

100

1000

Re

co

mb

ina

tio

n c

ou

nt

rate

(s

-1)

Storage time (s)

Recombination signal at 0.75 eV vs. time

A=48

A=47

A=48

A=47

S. Schippers et al.,

PRL 98 (2007) 033001


m = 3P0

g = 1S0 Fit:

Data analysis

0 2 4 6 8200

400

600

800

1000

Storage time (s)

Re

co

mb

ina

tio

n c

ou

nt

rate

(s

-1)

A=48

A=47

largest contribution to the experimental uncertainty

essential feature of the method

usage of two isotopes

47Ti18+: AHFI = 0.56(3) s-1

2s2 1S

2 1

J=0 2s2p 3P

J=0

HFI


Theoretical and experimental 2s2p 3P0 HFI lifetimes

0 10 20 30 40 50 60 70 80 9010

-6

10-4

10-2

100

102

104

nuclear spin

1/2 1

3/2 3

5/2 5

7/2 7

9/2 9

2s 2

p 3

P0 L

ifetim

e (

s-1)

Nuclear charge Z

present

experimental

value

J. P. Marques, F. Parente & P. Indelicato, PRA 47 (1993) 929

Ti18+ values

1993 theory: 2.812 s Marques et al. PRA 47 (1993) 929

2007 experiment: 1.8(1) s Schippers et al., PRL 98 (2007) 033001

2008 theory: 1.487 s Cheng et al., PRA 77 (2008) 052504

2009 theory: 1.476 s Andersson et al., PRA 79 (2009) 032501

2010 theory: 1.51 s Li & Dong, Plas. Sci. Technol. 79 (2010) 032501

What about

the remaining

discrepancy?


Influence of external fields

dipole magnets

with B up to 1.3 T

B-field

Zeeman effect: tHFI becomes mF dependent

effect too weak to explain discrepancies

Li et al., Phys. Lett. A 375 (2011) 914

E-field (via v x B)

Stark mixing of 3P0 and 3P1 levels:

effect much too weak to explain discrepancies

Maul et al., J. Phys. B 31 (1998) 2725


New measurements with Be-like AS12+ ions

10

20

30

40

506070

Co

unt

rate

(1

00 s

-1)

10

100

100

10

100

1

1

0 100 200

-0.2

-0.1

0.0

0.1

0.2

0 100 200

-0.2

-0.1

0.0

0.1

0.2

Storage time (s)

-5

0

5

-2

0

2

-2

0

2

-2

0

2

A=32 A=33

B = 0.44 T

tHFI = 10.5(7) s

B = 0.44 T

tHFI = 10.5(1.4) s

B = 0.88 T

tHFI = 10.2(7) s

S12+ values

theory: 27.69 s Marques et al. (1993)

theory: 10.73 s Cheng et al. (2008)

theory: 10.69 s Andersson et al. (2009)

experiment: 10.4(5) s TSR (2011)

S. Schippers et al., PRA 85 (2012) 012513


DR of Be-like 132Xe50+

n= 1/23/25/2j=7/2j=9/2j=11/2; n = 6j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2; n = 7 j=7/2 9/2 11/2 13/2 15/2 j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2; n = 9j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2; n = 10j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=21/2; n = 11j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=23/2; n = 12j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=25/2; n = 13j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=27/2; n = 14j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=29/2; n = 15j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=31/2; n = 16j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=33/2; n = 17j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=35/2; n = 18j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=37/2; n = 19j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=39/2; n = 20j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=41/2; n = 21j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=43/2; n = 22j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=45/2; n = 23j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=47/2; n = 24j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=49/2; n = 25j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=51/2; n = 26j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=53/2; n = 27j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=55/2; n = 28j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=57/2; n = 29j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=59/2; n = 30j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=61/2; n = 31j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=63/2; n = 32j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=65/2; n = 33j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=67/2; n = 34j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=69/2; n = 35j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=71/2; n = 36j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=73/2; n = 37j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=75/2; n = 38j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=77/2; n = 39j=1/2j=3/2j=5/2j=7/2j=9/2j=11/2j=13/2j=15/2j=17/2j=19/2j=79/2; n = 40n=111 j=223/2

n= 81/2

83/2

85/2

j=9/2 11/2 13/2 15/2 91/2

93/2

95/2

97/2

99/2

911/2

913/2

915/2

917/2

101/2

103/2

105/2

107/2

109/2

1011/2

1013/2

1015/2

1017/2

1019/2

111/2

113/2

115/2

117/2

119/2

1111/2

1113/2

1115/2

1117/2

1119/2

1121/2

121/2

123/2

125/2

127/2

129/2

1211/2

1213/2

1215/2

1217/2

1219/2

1223/2

131/2

133/2

135/2

137/2

139/2

1311/2

1313/2

1315/2

1317/2

1319/2

1325/2

141/2

143/2

145/2

147/2

149/2

1411/2

1413/2

1415/2

1417/2

1419/2

1427/2

151/2

153/2

155/2

157/2

159/2

1511/2

1513/2

1515/2

1517/2

1519/2

1529/2

161/2

163/2

165/2

167/2

169/2

1611/2

1613/2

1615/2

1617/2

1619/2

1631/2

171/2

173/2

175/2

177/2

179/2

1711/2

1713/2

1715/2

1717/2

1719/2

1733/2

181/2

183/2

185/2

187/2

189/2

1811/2

1813/2

1815/2

1817/2

1819/2

1835/2

191/2

193/2

195/2

197/2

199/2

1911/2

1913/2

1915/2

1917/2

1919/2

1937/2

201/2

203/2

205/2

207/2

209/2

2011/2

2013/2

2015/2

2017/2

2019/2

2039/2

211/2

213/2

215/2

217/2

219/2

2111/2

2113/2

2115/2

2117/2

2119/2

2141/2

221/2

223/2

225/2

227/2

229/2

2211/2

2213/2

2215/2

2217/2

2219/2

2243/2

231/2

233/2

235/2

237/2

239/2

2311/2

2313/2

2315/2

2317/2

2319/2

2345/2

241/2

243/2

245/2

247/2

249/2

2411/2

2413/2

2415/2

2417/2

2419/2

2447/2

251/2

253/2

255/2

257/2

259/2

2511/2

2513/2

2515/2

2517/2

2519/2

2549/2

261/2

263/2

265/2

267/2

269/2

2611/2

2613/2

2615/2

2617/2

2619/2

2651/2

271/2

273/2

275/2

277/2

279/2

2711/2

2713/2

2715/2

2717/2

2719/2

2753/2

281/2

283/2

285/2

287/2

289/2

2811/2

2813/2

2815/2

2817/2

2819/2

2855/2

291/2

293/2

295/2

297/2

299/2

2911/2

2913/2

2915/2

2917/2

2919/2

2957/2

301/2

303/2

305/2

307/2

309/2

3011/2

3013/2

3015/2

3017/2

3019/2

3059/2

311/2

313/2

315/2

317/2

319/2

3111/2

3113/2

3115/2

3117/2

3119/2

3161/2

321/2

323/2

325/2

327/2

329/2

3211/2

3213/2

3215/2

3217/2

3219/2

3263/2

331/2

333/2

335/2

337/2

339/2

3311/2

3313/2

3315/2

3317/2

3319/2

3365/2

341/2

343/2

345/2

347/2

349/2

3411/2

3413/2

3415/2

3417/2

3419/2

3467/2

351/2

353/2

355/2

357/2

359/2

3511/2

3513/2

3515/2

3517/2

3519/2

3569/2

361/2

363/2

365/2

367/2

369/2

3611/2

3613/2

3615/2

3617/2

3619/2

3671/2

371/2

373/2

375/2

377/2

379/2

3711/2

3713/2

3715/2

3717/2

3719/2

3773/2

381/2

383/2

385/2

387/2

389/2

3811/2

3813/2

3815/2

3817/2

3819/2

3875/2

391/2

393/2

395/2

397/2

399/2

3911/2

3913/2

3915/2

3917/2

3919/2

3977/2

401/2

403/2

405/2

407/2

409/2

4011/2

4013/2

4015/2

4017/2

4019/2

4079/2

411/2

413/2

415/2

417/2

419/2

4111/2

4113/2

4115/2

4117/2

4119/2

4181/2

421/2

423/2

425/2

427/2

429/2

4211/2

4213/2

4215/2

4217/2

4219/2

4283/2

431/2

433/2

435/2

437/2

439/2

4311/2

4313/2

4315/2

4317/2

4319/2

4385/2

441/2

443/2

445/2

447/2

449/2

4411/2

4413/2

4415/2

4417/2

4419/2

4487/2

451/2

453/2

455/2

457/2

459/2

4511/2

4513/2

4515/2

4517/2

4519/2

4589/2

461/2

463/2

465/2

467/2

469/2

4611/2

4613/2

4615/2

4617/2

4619/2

4691/2

471/2

473/2

475/2

477/2

479/2

4711/2

4713/2

4715/2

4717/2

4719/2

4793/2

481/2

483/2

485/2

487/2

489/2

4811/2

4813/2

4815/2

4817/2

4819/2

4895/2

491/2

493/2

495/2

497/2

499/2

4911/2

4913/2

4915/2

4917/2

4919/2

4997/2

501/2

503/2

505/2

507/2

509/2

5011/2

5013/2

5015/2

5017/2

5019/2

5099/2

111223/2

0.5 1.0 1.5 2.0

1

10

2s2 1S

0 (2s2p

1P

1) 8

j

DR

rate

coeffic

ient (1

0-8 c

m3 s

-1)


2s2p 3P

0 (2p

2 3P

1) 8

j

D. Bernhardt et al., in preparation


Time dependence of 3P0 DR resonance strength

D. Bernhardt et al., JPCS (in print)

Measurement of the E1M1 two-photon transition rate should be feasible


Comparison with theory

10 20 30 40 50 60 70 80 90

10-1

100

101

102

103

104

105

106

107

108

109

1010

1011

month

decade

millennium

second

minute

hour

century

year

Lifetim

e (

s)

Nuclear charge

E1M1

[Laughlin, PLA 75, 199 (1980)]

dayour

preliminary

value

nonrelativistic theory


Summary

Hyperfine-induced (HFI) transitions have specific applications

- accurate atomic clocks

- astrophysics: isotope specific abundances

HFI 2s2p 3P02s2 1S0 transition in Be-like ions

- does not compete with any other one-photon transition

First laboratory experiments with Be-like ions in a storage ring

- comparision of measurements with two istopes

- lifetimes determined with 5% accuracy

- 47Ti18+: 20% discrepancy with recent theoretical results

- 33S12+: Agreement with recent theoretical results

- in the future determination of nuclear magnetic moments?

E1M1 two-photon transition rate

- measurements will be pursued for heavy Be-like ions at the ESR


Collaborators & Funding

TSR - HFI transitions

D. Bernhardt, A. Müller, D. Yu

IAMP, Justus-Liebig-Universität Giessen

M. Lestinsky

GSI Helmholtzzentrum für Schwerionenforschung

M. Hahn, O. Novotný, D. W. Savin

Columbia Astrophysics Laboratory, Columbia University, New York

M. Grieser, C. Krantz, D. A. Orlov, R. Repnow, and A. Wolf

MPI für Kernphysik, Heidelberg, Germany

ESR – E1M1 transitions

D. Bernhardt, S. Böhm, J Jacobi, S Kieslich, H Knopp, P. H. Mokler, A. Müller, W. Shi

IAMP, Justus-Liebig-Universität Giessen

F. Bosch, C. Brandau, C. Kozhuharov, F. Nolden, M. Steck, T. Stöhlker

GSI Helmholtzzentrum für Schwerionenforschung

Z. Stachura

Instytut Fizyki Jadrowej, Krakow

Z. Harman

MPI für Kernphysik, Heidelberg, Germany

F. Fratini, S. Fritzsche, A. Surzhykov

Physikalisches Institut, Universität Heidelberg


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