scholarly journals Determination of the time scale of photoemission from the measurement of spin polarization

2018 ◽  
Vol 5 (6) ◽  
Author(s):  
Mauro Fanciulli ◽  
Hugo Dil

The Eisenbud-Wigner-Smith (EWS) time delay of photoemission depends on the phase term of the matrix element describing the transition. Because of an interference process between partial channels, the photoelectrons acquire a spin polarization which is also related to the phase term. The analytical model for estimating the time delay by measuring the spin polarization is reviewed in this manuscript. In particular, the distinction between scattering EWS and interfering EWS time delay will be introduced, providing an insight in the chronoscopy of photoemission. The method is applied to the recent experimental data for Cu(111) presented in M. Fanciulli et al., PRL 118, 067402 (2017), allowing to give better upper and lower bounds and estimates for the EWS time delays.

2002 ◽  
Vol 36 (4) ◽  
pp. 390-393
Author(s):  
O. Yu. Shevchenko ◽  
V. F. Radantsev ◽  
A. M. Yafyasov ◽  
V. B. Bozhevol’nov ◽  
I. M. Ivankiv ◽  
...  

2019 ◽  
Vol 211 ◽  
pp. 04007
Author(s):  
Anabella Tudora

The results of the PbP and sequential emission modellings describe very well the recent experimental data of 235U(n,f). The application of the sequential emission treatment to 49 fission cases has emphasized systematic behaviours of different quantities characterizing the fragments and the prompt emission. These allowed the determination of a general form of the residual temperature distribution for each emission sequence and the inclusion of sequential emission into the Los Alamos model.


2005 ◽  
Vol 201 ◽  
pp. 455-456
Author(s):  
Christopher. Fassnacht ◽  
Emily. Xanthopoulos ◽  
David. Rusin ◽  
Leon. Koopmans

The gravitational lens CLASS B1608+656 is one of the most promising lens systems for the measurement of H0 on cosmological scales. The three independent time delays between the four lensed images have been measured, and the extended lensed optical emission holds the promise for a very well-constrained model. The published time delay measurements are based on the first season of VLA monitoring, in which the background source varied by only 5% in flux density. The small level of variation leads to relatively large uncertainties in the determination of the time delays (10-20%). Two more seasons of monitoring have now been completed and the source flux density has changed by ˜25% during that time. We present the results of the continued VLA monitoring and the resulting time-delay analysis. The new data have significantly reduced the uncertainties on the time delays and, hence, reduced the uncertainties on the resulting determination of H0 from this system.


1994 ◽  
Vol 43 (4) ◽  
pp. 289-293 ◽  
Author(s):  
Masayoshi KIYOKAWA ◽  
Hitoshi YAMAGUCHI ◽  
Ryosuke HASEGAWA

2012 ◽  
Vol 8 (S289) ◽  
pp. 331-338
Author(s):  
S. H. Suyu

AbstractThe time delays between the multiple images of a strong gravitational-lens system, together with a model of the lens-mass distribution, provide a one-step determination of the time-delay distance, and thus a measure of cosmological parameters, particularly the Hubble constant, H0. I review the recent advances in measuring time-delay distances, and present the current status of cosmological constraints based on gravitational-lens time delays. In particular, I report the time-delay distance measurements of two gravitational lenses and their implication for cosmology from a recent study by Suyuet al.


2004 ◽  
Vol 19 (18) ◽  
pp. 1379-1390 ◽  
Author(s):  
W. Y. WANG ◽  
Y. L. WU ◽  
Y. A. YAN ◽  
M. ZHONG ◽  
Y. B. ZUO

The more precise extraction for the CKM matrix element |Vcb| in the heavy quark effective field theory (HQEFT) of QCD is studied from both exclusive and inclusive semileptonic B decays. The values of relevant nonperturbative parameters up to order [Formula: see text] are estimated consistently in HQEFT of QCD. Using the most recent experimental data for B decay rates, |Vcb| is updated to be |Vcb|=0.0395±0.0011expt±0.0019theorfrom B→D*lν decay and |Vcb|=0.0434±0.0041expt±0.0020theorfrom B→Dlν decay as well as |Vcb|=0.0394±0.0010expt±0.0014theorfrom inclusive B→Xclν decay.


2019 ◽  
Vol 114 ◽  
pp. 07004
Author(s):  
A. Safarov ◽  
A. Levin

This paper studies prediction of the boiling crisis onset under conditions of the rapid temperature growth of the heat releasing surface washed by a water flow subcooled to the saturation temperature. We obtained experimental data on time delay for rapid vapor formation and showed that the existing technique can be extended to the case with a forced flow. It is shown that the characteristic layer thickness is smaller than the thickness of superheated layer.


Author(s):  
M. Bahrami ◽  
M. M. Yovanovich ◽  
J. R. Culham

This paper provides an overview of the important physical phenomena necessary for the determination of effective thermal conductivity of nanofluids. Through an investigation, a large degree of randomness and scatter has been observed in the experimental data published in the open literature. Given the inconsistency in the data, it is impossible to develop a comprehensive physical-based model that can predict all the trends. This also points out the need for a systematic approach in both experimental and theoretical studies. Upper and lower bounds are developed for steady-state conduction in stationary nanofluids. Comparisons between these bounds and the experimental data indicate that all the data (except for carbon nanotube data) lie between the lower and upper bounds.


2019 ◽  
Vol 89 (2) ◽  
pp. 169
Author(s):  
С.Г. Ястребов ◽  
М.С. Чекулаев ◽  
A. Siklitskaya

AbstractCalculation results of the electronic spectrum of carbon nanospiroid C_300 are presented. The π-electron structure of the spiroid is calculated using the strong coupling method, in which the matrix element of the exchange interaction of neighboring electrons (the resonance integral) is considered as being dependent on the local curvature of the spiroid surface. The optical absorption coefficient is calculated in the framework of the Tautz model and the result is compared with experimental and astrophysical observational data. The calculated and experimental data are in good agreement.


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