Interfacial misfit dislocation array based growth of III-Sb active regions on GaAs/AlGaAs DBRs for high-power 2 μm VECSELs

2008 ◽  
Author(s):  
G. Balakrishnan ◽  
T. J. Rotter ◽  
A. Jallipalli ◽  
L. R. Dawson ◽  
D. L. Huffaker
Keyword(s):  
Misfit Dislocation ◽  
High Power ◽  
Active Regions ◽  
Dislocation Array

scholarly journals Formation of periodic interfacial misfit dislocation array at the InSb/GaAs interface via surface anion exchange

2016 ◽  
Vol 120 (3) ◽  
pp. 035301 ◽  
Author(s):  
Bo Wen Jia ◽  
Kian Hua Tan ◽  
Wan Khai Loke ◽  
Satrio Wicaksono ◽  
Soon Fatt Yoon
Keyword(s):  
Anion Exchange ◽  
Misfit Dislocation ◽  
Dislocation Array

scholarly journals High power terahertz quantum cascade lasers with symmetric wafer bonded active regions

2013 ◽  
Vol 103 (17) ◽  
pp. 171113 ◽  
Author(s):  
Martin Brandstetter ◽  
Christoph Deutsch ◽  
Michael Krall ◽  
Hermann Detz ◽  
Donald C. MacFarland ◽  
...  
Keyword(s):  
High Power ◽  
Quantum Cascade Lasers ◽  
Active Regions ◽  
Quantum Cascade ◽  
Cascade Lasers

Synoptic Charts of the Solar Eclipses of 1990 and 1991

1994 ◽  
Vol 144 ◽  
pp. 517-521
Author(s):  
Z. Mouradian ◽  
G. Buchholtz ◽  
G. Zlicaric
Keyword(s):  
Solar Limb ◽  
Active Regions ◽  
Solar Eclipses ◽  
Coronal Structures

AbstractThe synoptic charts of solar rotations 1831 and 1844 have been drawn up, corresponding to the eclipses of 22 July 1990 and 11 July 1991. These charts contain the active regions and the filaments, and show the position of the solar limb, at the time of the eclipse. They are for use in studying the coronal structures observed during these eclipses. The variation of these structures is given in the table. The last section of the article contains a formula for identifying the structures out of the limb.

Solar Corona Investigation by the Coronal Line Photometer at Lomnický Peak

1994 ◽  
Vol 144 ◽  
pp. 431-434
Author(s):  
M. Minarovjech ◽  
M. Rybanský
Keyword(s):  
Solar Corona ◽  
Time Resolution ◽  
Active Regions ◽  
High Time ◽  
High Time Resolution ◽  
List Type ◽  
Type Number ◽  
Coronal Line ◽  
Global Cycle

AbstractThis paper deals with a possibility to use the ground-based method of observation in order to solve basic problems connected with the solar corona research. Namely:1.heating of the solar corona2.course of the global cycle in the corona3.rotation of the solar corona and development of active regions.There is stressed a possibility of high-time resolution of the coronal line photometer at Lomnický Peak coronal station, and use of the latter to obtain crucial observations.

Radio Measurements of Coronal Magnetic Fields

1994 ◽  
Vol 144 ◽  
pp. 21-28 ◽  
Author(s):  
G. B. Gelfreikh
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Solar Corona ◽  
Active Regions ◽  
High Sensitivity ◽  
Coronal Magnetic Field ◽  
Transverse Magnetic ◽  
Radio Sources ◽  
Radio Waves ◽  
Solar Active Regions

AbstractA review of methods of measuring magnetic fields in the solar corona using spectral-polarization observations at microwaves with high spatial resolution is presented. The methods are based on the theory of thermal bremsstrahlung, thermal cyclotron emission, propagation of radio waves in quasi-transverse magnetic field and Faraday rotation of the plane of polarization. The most explicit program of measurements of magnetic fields in the atmosphere of solar active regions has been carried out using radio observations performed on the large reflector radio telescope of the Russian Academy of Sciences — RATAN-600. This proved possible due to good wavelength coverage, multichannel spectrographs observations and high sensitivity to polarization of the instrument. Besides direct measurements of the strength of the magnetic fields in some cases the peculiar parameters of radio sources, such as very steep spectra and high brightness temperatures provide some information on a very complicated local structure of the coronal magnetic field. Of special interest are the results found from combined RATAN-600 and large antennas of aperture synthesis (VLA and WSRT), the latter giving more detailed information on twodimensional structure of radio sources. The bulk of the data obtained allows us to investigate themagnetospheresof the solar active regions as the space in the solar corona where the structures and physical processes are controlled both by the photospheric/underphotospheric currents and surrounding “quiet” corona.

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