scholarly journals Testing nonlinear vacuum electrodynamics with Michelson interferometry

2015 ◽  
Vol 92 (2) ◽  
Author(s):  
Gerold O. Schellstede ◽  
Volker Perlick ◽  
Claus Lämmerzahl
2011 ◽  
Vol 2011 ◽  
pp. 1-9 ◽  
Author(s):  
Stefano Lupi

Through the coupling of Synchrotron Radiation and Michelson interferometry, one may obtain in the terahertz (THz) range transmittance and reflectivity spectra with a signal-to-noise ratio (S/N) up to 103. In this paper we review the application of this spectroscopic technique to novel superconductors with an increasing degree of complexity: the single-gap boron-doped diamond; the isotropic multiband V3Si, where superconductivity opens two gaps at the Fermi energy; the CaAlSi superconductor, isostructural to MgB2, with a single gap in the hexagonal ab plane and two gaps along the orthogonalcaxis.


1997 ◽  
Vol 04 (05) ◽  
pp. 1047-1050 ◽  
Author(s):  
G. DEGAND ◽  
P. MÜLLER ◽  
R. KERN

In a recent publication, we proposed a new experimental method for measuring the absolute surface stress of a thin crystalline sheet based on the deformation of very thin sheets (thickness e<10 μm) submitted to disymmetrical surface stresses (S1 on one side of the sheet, S2 on the other). This paper demonstrates that Michelson interferometry can be used to measure a surface stress change of 2–3 10-3 J·m -2 if the thickness and the Young modulus of the sheet are accurately known. Using a silicon substrate sample we found that one fourth of a monolayer of silver reduces the surface stress by 0.45 J·m -2.


1997 ◽  
Vol 189 ◽  
pp. 127-136
Author(s):  
Michael S. Bessell

The empirical temperatures scale for cool stars is generally well established. Temperatures are now known with reasonable precision for stars covering the range of spectral types from A to M. In the historical paper by Code, Davis, Bless and Hanbury Brown (Code et al. 1976), six stars between 10000K and 6500K had radii measured by the intensity interferometer and these six, together with the sun formed the basis of the empirical temperature calibration at the time. Since then, many temperatures have been derived for A-K stars (Blackwell & Lynas-Gray 1994; Alonso et al. 1996a) using the Infra-Red Flux Method (see Megessier 1994,5 and this volume), while lunar occultations (Ridgway et al. 1980) and more recently Michelson interferometry (Di Benedetto & Rabbia 1987; Dyck et al. 1996), have been used to measure the radii of K and M giants. It is a tribute to Hanbury Brown's Intensity Interferometer that temperature scales based on its measurements are essentially unchanged by the new data.


2013 ◽  
Vol 47 (1) ◽  
pp. 97-108
Author(s):  
O. Sarmiento Martinez ◽  
D. Mayorga Cruz ◽  
J. Uruchurtu Chavarin ◽  
J. A. Marban ◽  
E. Sarmiento

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