Quantitative Phase Shift Analysis for 3D Defect Localization Using Lock-in Thermography

Author(s):  
Christian Schmidt ◽  
Frank Altmann

Abstract It was already demonstrated, that the method of Lock-in Thermography (LIT) enables 3D localization of thermal active defects, e.g. electrical shorts and resistive opens, on die level and within fully packaged single and multichip devices [1,2]. The depth of a defect can be derived from phase shift measurements of the defective compared to a reference device For a general approach of this method, thermal modeling is used and verified by experimental data to investigate the internal heat propagation under periodic stimulation in correlation to the LIT measuring process. [3]. A basic requirement for the successful application of the method is a precise and reproducible measurement of both the thermal material properties of each material layer and the phase shift between the internal heat excitation and thermal response measured by LIT. Significant influences from the material and measurement setup to the detected phase shift have to be identified and taken into account. However, to identify and distinguish the relevant influences measurements with defined internal heat sources are necessary which are presented in this paper. First, the relationship between geometrical thickness of a material layer and the resulting thermal parameters for both homogeneous and heterogeneous materials are measured and discussed. A new measurement setup generating a defined point heat source will be presented to calibrate the LIT system for quantitative phase shift measurements and to determine the phase shift to thickness parameters of single material layers. In addition the variation of the phase shift caused by the defect geometry and the defect environment will be investigated. Finally, a case study is presented comparing the experimental results to the obtained results from a real stacked die device.

2020 ◽  
Author(s):  
Edoardo Rognini ◽  
Alessandro Mura ◽  
Maria Teresa Capria ◽  
Angelo Zinzi ◽  
Anna Milillo ◽  
...  

<div> <p>The BepiColombo mission is the first European mission to Mercury; the spacecraft will reach its destination in December 2025, and will study in detail the surface, the exosphere and the magnetosphere of the planet. </p> </div> <div> <p>We have developed a thermophysical model with the aim to analyze the dependence of the temperature of the surface and of the layers close to it on the assumptions on the thermophysical properties of the soil. The code solves the one-dimensional heat equation, assumes purely conductive heat propagation and no internal heat sources; the surface is assumed to be composed of a regolith layer with high porosity and density increasing with depth. The illumination conditions are calculated by using a Mercury shape model and the SPICE routines [1]. </p> </div> <div> <p>The model will help us to interpret the data that will be provided by the instruments onboard the BepiColombo mission. Preliminary calculations have been carried out to analyze the thermal response of the soil as a function of thermal conductivity. The model is currently also used to study the sodium content in the planet's exosphere, whose origin is under investigation [2]; the MESSENGER mission has measured the exospheric sodium content as a function of time, detecting an increase at the "cold poles" (so called because of their lower than average temperature). We therefore want to study the effect of surface temperatures on the sodium content in the exosphere; for this purpose, the temperature distribution calculated with the code is used together with an atmospheric circulation model that calculates the exospheric sodium content [3]. </p> </div> <div> <p>A simplified version of the thermophysical code is almost ready to be available to the scientific community through MATISSE [4], the software developed at the SSDC in ASI and available at https://tools.ssdc.asi.it/Matisse. </p> </div> <p>[1] Acton, C. H. (1996), Planetary and Space Science, 44, 65-70<br />[2] Cassidy, T., et al. (2016), GRL, 43, 11 121-128<br />[3] Mura, A., et al. (2009), Icarus, 1, 1-11<br />[4] Zinzi, A., et al. (2016), Astronomy & Computing, 15, 16-28</p>


1975 ◽  
Vol 38 (9) ◽  
pp. 1099-1141 ◽  
Author(s):  
J E Bowcock ◽  
H Burkhardt

1970 ◽  
Vol 20 (2) ◽  
pp. 301-319 ◽  
Author(s):  
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P. Lugaresi-Serra ◽  
G. Mandrioli ◽  
A.M. Rossi ◽  
F. Griffiths ◽  
...  

1973 ◽  
Vol 44 (1) ◽  
pp. 1-4 ◽  
Author(s):  
R. Vinh Mau ◽  
J.M. Richard ◽  
B. Loiseau ◽  
M. Lacombe ◽  
W.N. Cottingham

1963 ◽  
Vol 129 (5) ◽  
pp. 2311-2322 ◽  
Author(s):  
Olav T. Vik ◽  
Hugo R. Rugge

2013 ◽  
Author(s):  
Aamod Shanker ◽  
Martin Sczyrba ◽  
Brid Connolly ◽  
Andy Neureuther ◽  
Laura Waller

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