HYPERSATELLITE AND SATELLITE ENERGY SHIFTS AND INTENSITY RATIOS

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HYPERSATELLITE AND SATELLITE ENERGY SHIFTS AND INTENSITY RATIOS

V. Horvat, K. Ilakovac, M. Vesković, S. Kaučić

To cite this version:

V. Horvat, K. Ilakovac, M. Vesković, S. Kaučić. HYPERSATELLITE AND SATELLITE ENERGY

SHIFTS AND INTENSITY RATIOS. Journal de Physique Colloques, 1987, 48 (C9), pp.C9-629-C9-

631. �10.1051/jphyscol:19879106�. �jpa-00227213�

JOURNAL D E PHYSIQUE

Colloque C9, supplement au n012, Tome 48, decembre 1987

V. HORVAT*

,

,

' ~ a c u l t y of Science and Mathematics, University of Zagreb.

Zagreb, POB 162. Yugoslavia

"

**'~nstitute o f Physics, University Novi Sad, Yugoslavia

ABSTRACT - Measurements of the decay of xenon and silver atoms with double K-shell vacancies (vacant K shell) were performed using a pair of germanium detectors and a three-parameter pulse-height analyzer. In xenon Kci hypersatellite shift and relative intensities of K hypersatellite and K satellite transitions were obtained. In silver the same quantities and also K B hypersatellite s h i f t , K a and Kf3 satellite shifts with L- s p e c t a t o r vacancy and iQ? satellite shift with M- and N- spectator vacancy were de- termined.

1. INTRODUCTION

Accurate measurements of hypersatellite e n e r g y s h i f t s and transition r a t e s seem to be a v e r y sensitive t e s t of magnetic and retardation effects i n atoms. These dynamical relativistic effects were first formulated b y G . Breit in 1932 ( 1 ) in a form applicable to light atoms, and more recently reformulated b y Mann and Johnson ( 2 ) to include the dependence on t h e e n e r g y of exchange photons. Extensive calculations of hypersatellite e n e r g y shifts and transition r a t e s were made b y Chen, Crasemann, and Mark ( 3 ) . The experimental investigations of the hypersatellite transitions were initiated by von Oertzen ( 4 ) by :he diffraction method and by Briand e t a1 ( 5 ) using coincidence tech- nique and semiconductor d e t e c t o r s . Since t h e n many measurements were made (3) for Z from 25 to 82. The latter method was applied by o u r group to redetermine t h e hyper- satellite e n e r g y shift in silver ( 6 ) . Additional measurements and improved methods of.

analysis yielded new data and smaller e r r o r s . Also the measurements with xenon atoms were made. From either s e t of d a t a the intensity ratios of hypersatellite transitions were determined. T h e hypersatellite transitions occur i n atoms which initially have a double K-shell vacancy. While one electron is t r a n s f e r e d from a higher shell to one vacancy s t a t e in the K shell, the o t h e r vacancy is a spectator. The following t r a n s f e r of an electron from a higher shell to t h e o t h e r vacancy s t a t e in the K shell occurs with a s p e c t a t o r vacancy i n a higher shell (formed i n the f i r s t t r a n s i t i o n ) . Results on these satellite transitions with s p e c t a t o r vacancies i n L , M, and N shells have also been derived. Calculations of the satellite e n e r g y shifts were made by Burch e t a1 ( 7 ) .

("1" part supported by US NSP (project PN-734)

Article published online by EDP Sciences and available at http://dx.doi.org/10.1051/jphyscol:19879106

JOURNAL

DE

2. MEASUREMENTS

Radioactive sources of 131-Cs and 109-Cd were used as generators of double-K-shell- vacancy atoms of xenon and silver, respectively. The measurements were made with a p a r of hgn-purity germanium detectors with the source between them in a close 180°

geometry. The data were recorded in a fast-slow coincidence system with a three- parameter 128 x 512 x 542 pulse-height analyser.

3. ANALYSIS OF DATA AND RESULTS

The data on xenon were analysed by the same methods as described in ref. 6. I n the analysis of data on silver an improved method was applied: the complete region of K hypersatellite peaks was analysed as one set of data (previously i t was divided into 4 p a r t s ) ; the relative intensities of transitions were calculated directly; the background was not assumed constant, but modelled in a refined way.

Our results, results of previous measurements and the theoretical values for the hyper- satellite and satellite energy shifts are shown in Table 1. The results for hypersatellite and satellite intensity ratios for xenon are shown in Table 2, and for silver in Table 3.

Table l.Energy shifts of the hypersatellite and satelIite transitions in xenon and silver (in eV)

Table 2 . Intensity ratios of the hypersatellite and satellite transitions in xenon Ka-h

KB-h

Ka-s KB-s KB-s

spectator- vacancy shell

K K

L L M o r N

. ^{I ( X )} I I ( Y )

this experiment theory1 ref.

.47 k. 02 .603 (1)

,175k. 036 .I79 (1)

.050+. 020 .042 (1)

.163+. 47 .050

+.

.044+. 012

<.

vacancy shell

K K K L L M M N N X

KaTh Kgl-h Kg2-h K BL-s K &YS K B r s K 81-s K 51-s K B r s

xenon

Y Ka-h K w h Ka-h K a-s Ka-s Ka-s Ka-s Ka-s Ka-s

r

"

ref.

(1)

( 2 ) . experiment

656k19

84 -1. 10

silver ref.

*

*

experiment 532k6 519.7+7.8 674.8-1.6.0

39.2+4.6 137.9+ 5.7 61 k 19 theory

639.4

80

ref.

8

*

*

* *

theory 534.8 681.0

67 155

ref.

( 1 ) ( 1 )

(2) ( 2 )

C9-631

Table 3. Intensity ratios of the hypersatellite and satellite transitions in silver

REFERENCES X

Ka2-h KBl-h K

B

B

Ka2-s KB1-s K

B

1. B r e i t G., Phys. Rev. 39 (1932) 616

2. Mann J. B. and Johnson W. R . , Phys. Rev. A4 (1971) 41

3. Chen M. H., Crasernann B., and M a r k H., Phys. Rev. A25 (1982) 391 4. von O e r t z e n W . , Z. Phys. 182 (1964) 130

5. Briand J. P . , Chevallier P., T a v e r n i e r M . , and Rozet J. P . , Phys. Rev. Lett. 27 (1971) 777

6. Horvat V. and Ilakovac K . , Phys. Rev. A31 (1985) 1543

7. B u r c h D., Wilets L . , and Meyerhof W. E . , Phys. Rev. A9 (1974) 1007 8. van Eijk C. W. E., Wijnhorst J., and P o p e l i e r M.A. , P h y s . Rev.

C19 (1979) 1047 Y

Kal-h

"

I 1

Kctl-s

11 11

Kal-s

II II

spectator- vacancy shell

K K K

L L L M or N M or N M o r N

I ( X ) /I(Y)

'

this experiment

.617?. 055 .332+. 020 .063+. 006 .701+.. 055 .294+. 010 .060t. 005 .363+.078 .293+. 028 .040+0.17

,

theory .746 .340 . .051

r e f . (1) (1) (1)