Optical Wireless Communication Channel Measurements and Models Ahmed Al-Kinani, Cheng-Xiang Wang , Fellow, IEEE,Lizhou , and Wensheng Zhang , Member, IEEE

Total Page:16

File Type:pdf, Size:1020Kb

Optical Wireless Communication Channel Measurements and Models Ahmed Al-Kinani, Cheng-Xiang Wang , Fellow, IEEE,Lizhou , and Wensheng Zhang , Member, IEEE IEEE COMMUNICATIONS SURVEYS & TUTORIALS, VOL. 20, NO. 3, THIRD QUARTER 2018 1939 Optical Wireless Communication Channel Measurements and Models Ahmed Al-Kinani, Cheng-Xiang Wang , Fellow, IEEE,LiZhou , and Wensheng Zhang , Member, IEEE Abstract—Optical wireless communications (OWCs) refer to high capacity and high data rates required by new wire- wireless communication technologies which utilize optical car- less applications. Therefore, researchers have been focusing riers in infrared, visible light, or ultraviolet bands of electro- on the fifth generation (5G) wireless communication systems magnetic spectrum. For the sake of an OWC link design and performance evaluation, a comprehensive understanding and an that are expected to be deployed around 2020 [1]. Various accurate prediction of link behavior are indispensable. Therefore, potential promising technologies for 5G systems have been accurate and efficient channel models are crucial for the OWC suggested, such as massive multiple-input multiple-output link design. This paper first provides a brief history of OWCs. (MIMO) [2], cell densification, cognitive radio networks, and It also considers OWC channel scenarios and their utilization millimeter wave (mmWave) communications [3], [4]. Further trade-off in terms of optical carrier, range, mobility, and power efficiency. Furthermore, the main optical channel characteris- shifting beyond mmWave frequencies, there is about 0.3 – tics that affect the OWC link performance are investigated. A 30000 THz of bandwidth that does not fall under the federal comprehensive overview of the most important OWCs channel communications commission (FCC) regulations called optical measurement campaigns and channel models, primarily for wire- spectrum [5]. Wireless communications in optical window is less infrared communications and visible light communications, called optical wireless communications (OWCs). OWCs uti- are presented. OWCs channel models are further compared in terms of computation speed, complexity, and accuracy. The sur- lize three different regions of the electromagnetic spectrum vey considers indoor, outdoor, underground, and underwater (EM), i.e., infrared (IR), visible light, and ultraviolet (UV). communication environments. Finally, future research directions The optical spectrum window is illustrated in Fig. 1. Wireless in OWCs channel measurements and models are addressed. infrared communication (WIRC) systems utilize the near- Index Terms—Wireless infrared communications, visible light infrared (NIR) portion (IR-A) which occupies wavelengths communications, optical wireless channel characteristics, optical from 780 nm to 1400 nm of the entire IR wavelength range wireless channel measurements, optical wireless channel models. (780 –106 nm). IR-A extends from the nominal red edge of the visible spectrum. Originally, IR-A was targeted for short-range I. INTRODUCTION wireless communications. IR-B (1400 – 3000 nm) is used ADIO frequency (RF) wireless systems designers have mainly for long distance communications either guided (opti- been facing the continuously increasing demand for cal fibre) or free space optical communications. While, IR-C R portion (3000 – 106 nm), which is also called thermal imag- Manuscript received June 6, 2017; revised January 19, 2018; accepted ing region, has been extensively used for military applications April 15, 2018. Date of publication May 18, 2018; date of current ver- such as missiles homing and civilian purposes such as remote sion August 21, 2018. This work was supported in part by the EU H2020 RISE TESTBED under Project 734325, in part by the EU H2020 ITN temperature sensing. Visible light communications (VLCs) use 5G Wireless under Project 641985, in part by the EU FP7 QUICK under the entire visible light wavelength region (380 – 780 nm). Project PIRSES-GA-2013-612652, in part by the Science and Technology Wireless ultraviolet communications (WUVCs) employ UV-C Project of Guangzhou under Grant 201704030105, in part by the Key Research and Development Program of Shandong Province under Grant (200 – 280 nm, the deep UV) segment of the entire UV wave- 2016GGX101014, in part by the Fundamental Research Funds of Shandong length range (10 – 380 nm) [6], [7]. Furthermore, UV-A and University under Grant 2017JC029, and in part by the Ministry of Higher UV-B are suitable for a wide range of applications including Education and Scientific Research of Iraq under Grant 790. (Corresponding author: Cheng-Xiang Wang.) commercial, military, medicine, and dentistry applications [8]. A. Al-Kinani was with the Institute of Sensors, Signals and Systems, The last part of the UV spectrum called extreme ultraviolet School of Engineering and Physical Sciences, Heriot-Watt University, (EUV). This range of wavelengths is absorbed almost com- Edinburgh EH14 4AS, U.K. He is now with the Technical Affairs Department, Iraqi Ministry of Communications, Baghdad 10013, Iraq (e-mail: pletely by the earth’s atmosphere [9]. Therefore EUV requiring [email protected]). high vacuum for transmission. C.-X. Wang is with the Mobile Communications Research Laboratory, Looking back into history, OWCs predate RF techniques Southeast University, Nanjing 211189, China, and also with the Institute of Sensors, Signals and Systems, School of Engineering and Physical by many centuries. Each nation had its own way of using Sciences, Heriot-Watt University, Edinburgh EH14 4AS, U.K. (e-mail: fire signals to warn possible invasion or announce victory. [email protected]). About 800 BC, ancient Greeks and Romans used fire bea- L. Zhou is with the School of Microelectronics, Shandong University, Shandong 250100, China (e-mail: [email protected]). cons in order to guide ships toward the mainland. In 1880, W. Zhang is with the Shandong Provincial Key Laboratory of a light based telephone called photophone was innovated by Wireless Communication Technologies, School of Information Science Alexander Graham Bell to send and receive sound clearly and Engineering, Shandong University, Shandong 250100, China (e-mail: [email protected]). over sunlight via unguided channel for a distance of some Digital Object Identifier 10.1109/COMST.2018.2838096 213 m, and shorter ranges were covered using various lamps 1553-877X c 2018 IEEE. Personal use is permitted, but republication/redistribution requires IEEE permission. See http://www.ieee.org/publications_standards/publications/rights/index.html for more information. 1940 IEEE COMMUNICATIONS SURVEYS & TUTORIALS, VOL. 20, NO. 3, THIRD QUARTER 2018 The very latest UV LEDs-based communication test-bed was reported in [18]. The setup can reliably deliver a data rate of 2.4 kbps for a vertically pointing transmitter and receiver of 11 m separation. Rapid development in compound semicon- ductor design and fabrication of LEDs, photodiodes (PDs), and filters, has inspired recent research and development in the OWC technology. Since IR, visible light, and UV bands exhibit differ- ent optical properties, the propagation characteristics of the optical channel between the optical transmitter or source (OTx) and the optical receiver (ORx), are therefore differ- Fig. 1. The optical spectrum. ent. Consequently, an accurate propagation channel model is indispensable to design an accurate and an efficient OWC system. In the literature, many survey papers have been pub- as a light source. Photophone was considered as the first VLC lished in terms of channel measurements and models in IR device [10]. For military purposes, German Army introduced and UV bands, while very few in the visible light band. IR photophones in 1935. The light source was a tungsten The previous work considered each band individually such filament lamp combined with an IR transmitting filter. IR as [7], [11], [19], and [20]–[22] or in a specific environment photophones succeeded in communicating over a range of as in [23]–[25]. This motivates the need to present a compre- 3 km at daylight and a clear weather [11]. In 1955, Rubin hensive survey of optical wireless channel measurements and Braunstein, from the Radio Corporation of America (RCA), models that conducted in IR and visible light bands consid- reported IR emission from a simple diode structured from ering different environments, i.e., indoor, outdoor, underwater gallium arsenide (GaAs). Two years later, in 1957, Braunstein and underground. further demonstrated that such a diode can be used for WIRCs The rest of the survey is organized as follows. Section II through sending an audio signal to be detected by a lead sul- providing an overview of WIRCs, VLCs, and WUVCs tech- fide (PbS) diode some distance away [12]. In 1962, Texas nologies in terms of evolution and growth. In Section III, instruments (TI) manufactured the first commercial infrared various scenarios of OWCs links are presented and the trade- light-emitting diode (IRED) product, which was structured off between their features is thoroughly explained. OWCs from GaAs compound with emission in the 900 nm wave- channels’ characteristics have been detailed in Section IV.An length range [13]. By the fall of 1962, groups at IBM research overview of measurement campaigns and the state-of-the-art laboratory, MIT Lincoln laboratory, and general electric (GE) of indoor OWCs channel models are presented in Section V. succeeded in demonstrating IR laser diode (LD) [14]. During Outdoor OWCs channel models and measurement efforts the same year, unlike others in RCA, Nick Holonyak chose are introduced in Section VI. In Section VII, Underwater gallium arsenide
Recommended publications
  • Observing Photons in Space
    —1— Observing photons in space For the truth of the conclusions of physical science, observation is the supreme court of appeals Sir Arthur Eddington Martin C.E. HuberI, Anuschka PauluhnI and J. Gethyn TimothyII Abstract This first chapter of the book ‘Observing Photons in Space’ serves to illustrate the rewards of observing photons in space, to state our aims, and to introduce the structure and the conventions used. The title of the book reflects the history of space astronomy: it started at the high-energy end of the electromagnetic spectrum, where the photon aspect of the radiation dominates. Nevertheless, both the wave and the photon aspects of this radiation will be considered extensively. In this first chapter we describe the arduous efforts that were needed before observations from pointed, stable platforms, lifted by rocket above the Earth’s atmosphere, became the matter of course they seem to be today. This exemplifies the direct link between technical effort — including proper design, construction, testing and calibration — and some of the early fundamental insights gained from space observations. We further report in some detail the pioneering work of the early space astronomers, who started with the study of γ- and X-rays as well as ultraviolet photons. We also show how efforts to observe from space platforms in the visible, infrared, sub-millimetre and microwave domains developed and led to today’s emphasis on observations at long wavelengths. The aims of this book This book conveys methods and techniques for observing photons1 in space. ‘Observing’ photons implies not only detecting them, but also determining their direction at arrival, their energy, their rate of arrival, and their polarisation.
    [Show full text]
  • 5. Astronomy Through the Atmosphere
    5. Astronomy Through the Atmosphere Ground based observations are affected by: • absorption • refraction • scattering • scintillation In this section we will briefly consider some of the effects of these four phenomena. 1 Absorption The Earth’s atmosphere is opaque to E-M radiation, apart from two windows: in the optical and radio regions of the E-M spectrum. X-rays UV Visible Infrared sub mm Radio mm & microwave hard soft EUV (FIR) Completely opaque Optical window Radio window Molecular transitions (inc. H2O) 0 Ionisation of air molecules (starting with ozone) Ionosphere reflective Fraction of energy absorbed 1 1nm 10nm 100nm 1mm 10mm 100mm 1mm 1cm 10cm 1m 10m2 100m Completely transparent Wavelength Absorption Between the optical and radio windows there are numerous absorption bands due to molecular transitions (mainly of water). It is possible to get above the clouds containing this water vapour because of the 4 temperature structure (km) of the atmosphere. Above about 2 km there can be a thin inversion Altitude 2 layer, where the temperature Inversion increases with height. Clouds layer form at the base of the inversion layer, leaving generally clear, dry 020 Temperature (C) air above. 3 Absorption The world’s best observatories (e.g. La Palma, Hawaii, La Silla, Paranal) are all at altitudes and locations which place them above inversion layers. 4 Absorption How does absorption in the atmosphere affect the apparent brightness of objects? We model the atmosphere as a series of plane-parallel slabs. Consider a thin slab of thickness d
    [Show full text]
  • Appendix a Glossary
    Appendix A Glossary Only brief definitions are given to provide a quicklook reference for the reader with regard to terminology. Bold face type within a definition refers to a subject-related entry. 6788) 6789) 6790) Aberration. Geometrical errors in imagery whereby a perfect image is not formed. Typical aberrations include spherical aberration, astigmatism, coma, and chromatic aberrations. Lens bendings, locations, powers, materials, and increasing the number of lenses and aper­ ture stop positions are all used to minimize aberrations. The aberration theory of images generated by an optical system has been gradually develo­ ped from the seventeenth century on. Early analyses by e.g. Descartes, Roberval and Huy­ gens concern the spherical aberration which arises when imaging an object point through a single refracting or reflecting surface. Absorption band. A range of wavelengths, or frequencies, in the electromagnetic spectrum within which radiant energy is absorbed by a substance (gas, liquid or solid). In the gaseous phase, absorption lines are much narrower than in liquids or solids. In a polyatomic gas, an absorption band is actually composed of discrete absorption lines which appear to overlap. Each line is associated with a particular mode of vibration and rotation induced in a gas mol­ ecule by incident radiation. Examples: • Ozone (O3) has several absorption bands. They are: a) the Hartley bands (2000-3000 Å in UV with max absorption at 2550 Å); b) the Huggins bands (weak absorption between 3200-3600 Å); c) the Chappuis bands (weak and diffuse at 4500 Å and at 6500 Å in VIS); d) IR bands at 4.7, 9.6, and 14.1 mm.
    [Show full text]
  • Atmosphere • Filters Part of the Electromagnetic Radiation • to the Earth's Surface – Optical Window 400 – 800 Nm
    Atmosphere • Filters part of the electromagnetic radiation • To the Earth’s surface – optical window 400 – 800 nm – radiowindow 1mm – 15 m • Disturbances – refraction (light bends in the atmosphere) – skintillation (twinkling star) – seeing Observational tools • Optical telescopes – Observations of visible light • Radio and submillimeter telescopes – Observations of the radio region (radio window) – Satellites and probes – Other parts of the electromagnetic radiation – planet, asteroid and comet probes Telescope types Refracting telescope • A lens acts as the objective, front side of the telescope • First refracting telescopes at the start of the 17th century – chromatic aberration, focal points for different wavelengths don’t connect • correction: achromatic lenses • Structural problem: supporting the lens – Largest diameter 102 cm • Astrographs: size of the image field 5o – mapping of large areas Reflecting telescope • A paraboloid mirror (main mirror) covered with a thin aluminum layer collects the light • Main mirror reflects the light back to the incident direction – Image at the focal point (prime focus) • Difficult to reach – Usually a secondary mirror that has been placed before the prime focus -> directs light somewhere else • Image at the secondary focus • The shape and position of the secondary mirror defines the focus type • Coma error Telescope foci Prime focus • Location where the reflected light forms an image • Observations difficult because focus is in front of the main mirror • Placement of large equipment difficult Newton
    [Show full text]
  • Radio Astronomy: How J.C. Bose's Invention Opened a New Window To
    Radio Astronomy: How J.C. Bose’s invention opened a new window to the Universe Dr. Yashwant Gupta Centre Director, NCRA, TIFR, Pune [email protected] Prologue: Sir J.C. Bose's work in radio microwave optics was specifically directed towards studying the nature of the phenomenon and was not an attempt to develop radio into a communication medium. His experiments took place during the same period (from late 1894 on) when Guglielmo Marconi was making breakthroughs on a radio system specifically designed for wireless telegraphy. In 1895, he demonstrated the generation & reception of radio waves in Kolkata, a good 2 years before the experiment by Marconi. It is thanks to this stellar breakthrough that we are able to probe the Universe in a unique manner using radio wavelengths. 1. Introduction to Radio Astronomy Astronomy is one of the oldest sciences. It started from the time mankind turned its gaze upwards to try and understand the heavens. It began with use of naked eyes which are natural detectors for light waves, but evolved dramatically with the advent of the telescope. Galileo turned the recently invented optical telescope to the heavens and revolutionised astronomy forever (figure 1). Over the times since then, optical telescopes have evolved from the simple ones that Galileo used to the large, sophisticated facilities that modern day astronomers employ. Figure 1: Galileo and the telescope, c.1609 There are two main factors that drive the need for larger telescopes. A bigger telescope is able to collect more light, hence can see fainter sources i.e., they are more sensitive and can see more objects in the Universe.
    [Show full text]
  • Thesis Template
    FREE SPACE OPTICAL COMMUNICATIONS WITH HIGH INTENSITY LASER POWER BEAMING DANIEL EDWARD RAIBLE Bachelor of Science in Electrical Engineering Cleveland State University May 2006 Master of Science in Electrical Engineering Cleveland State University May 2008 submitted in partial fulfillment of requirements for the degree DOCTOR OF ENGINEERING at the CLEVELAND STATE UNIVERSITY June 2011 This dissertation has been approved for the Department of Electrical and Computer Engineering and the College of Graduate Studies by ________________________________________________ Dissertation Committee Chairperson, Taysir H. Nayfeh ________________________________ Department/Date ________________________________________________ Nigamanth Sridhar ________________________________ Department/Date ________________________________________________ Ana V. Stankovic ________________________________ Department/Date ________________________________________________ Petru S. Fodor ________________________________ Department/Date ________________________________________________ John F. Turner ________________________________ Department/Date This work is dedicated to the memory of my dearest friends, Michael Matthews and Jason Adams. It would have been great, and I miss you. ACKNOWLEDGEMENTS There are many people that I would like to express my gratitude towards, starting with my advisor Dr. Taysir Nayfeh, for affording me the opportunity to pursue my education through working at the Industrial Space Systems Laboratory, and for helping me develop my skills as a researcher. I would like to graciously thank my committee for their time and review starting with Dr. Nigamanth Sridhar for providing his background in wireless systems, Dr. Ana V. Stankovic for offering her knowledge in power electronics and systems, Dr. Petru S. Fodor and Dr. John F. Turner for supplying their expertise in optics and general physics, and finally Dr. Joseph A. Svestka for serving as a non-voting member and for sharing his expertise in systems engineering and mathematical programming.
    [Show full text]
  • Optical Wireless Communication Channel Measurements and Models
    Heriot-Watt University Research Gateway Optical Wireless Communication Channel Measurements and Models Citation for published version: Al-Kinani, A, Wang, C-X, Zhou, L & Zhang, W 2018, 'Optical Wireless Communication Channel Measurements and Models', IEEE Communications Surveys and Tutorials. https://doi.org/10.1109/COMST.2018.2838096 Digital Object Identifier (DOI): 10.1109/COMST.2018.2838096 Link: Link to publication record in Heriot-Watt Research Portal Document Version: Peer reviewed version Published In: IEEE Communications Surveys and Tutorials Publisher Rights Statement: © 2018 IEEE. Personal use of this material is permitted. Permission from IEEE must be obtained for all other uses, in any current or future media, including reprinting/republishing this material for advertising or promotional purposes, creating new collective works, for resale or redistribution to servers or lists, or reuse of any copyrighted component of this work in other works. General rights Copyright for the publications made accessible via Heriot-Watt Research Portal is retained by the author(s) and / or other copyright owners and it is a condition of accessing these publications that users recognise and abide by the legal requirements associated with these rights. Take down policy Heriot-Watt University has made every reasonable effort to ensure that the content in Heriot-Watt Research Portal complies with UK legislation. If you believe that the public display of this file breaches copyright please contact [email protected] providing details, and we will
    [Show full text]
  • Basic Principles of Fiber Optics
    Basic Principles of Fiber Optics http://www.corningcablesystems.com/web/college/ fibertutorial.nsf/fibman?OpenForm Copyright ©2006 Corning Incorporated Basic Principles of Fiber Optics Table of Contents Introduction ............................................................................................................................................ 3 What is Fiber Optics? .......................................................................................................................... 4 Fiber Benefits ...................................................................................................................................... 4 Long Distance Signal Transmission ............................................................................................... 4 Large Bandwidth, Light Weight, and Small Diameter ..................................................................... 4 Long Lengths .................................................................................................................................. 5 Easy Installation and Upgrades ...................................................................................................... 5 Non-Conductivity ............................................................................................................................ 5 Security ........................................................................................................................................... 6 Designed for Future Applications Needs .......................................................................................
    [Show full text]
  • An Introduction to Astronomical Photometry Using Ccds
    An Introduction to Astronomical Photometry Using CCDs W. Romanishin University of Oklahoma [email protected] The lastest version of this book (in pdf format) can be downloaded from http://observatory.ou.edu This is version wrccd4a.pdf built on: March 31, 2002 2 Foreword/ Thanks / Production Details This book began as a set of lecture notes for a junior/senior course entitled \Observatory Meth- ods" that I teach each spring at the University of Oklahoma (OU). The book is intended as an introduction for the college astrophysics major to photometry in the optical region of the spectrum of astronomical objects using CCD imaging from groundbased telescopes. Of course, in these times of Giga-buck satellite telescopes of various sorts, groundbased optical astronomy is only a part of observational astronomy. Within groundbased optical astronomy, spectroscopy, only briefly men- tioned here, probably takes up as much or more telescope time as photometry. That said, it is still obvious that imaging photometry is an important part of observational astronomy. With the ready availablity of inexpensive CCDs and computer power, even a small telescope can provide an important \hand on" learning experience not available with remote satellite observatories. This book represents knowledge I have accumulated over 20 years of observing with a wide range of telescopes. My PhD disseration, finished in 1980, was probably one of the last observational dissertations to use photographic emulsions as the primary detector. Since then I have observed with various photomultiplier detectors and many different CCD systems, on telescopes ranging in aperture from 0.4 to 10 meters.
    [Show full text]
  • What Can We Learn from the Electromagnetic Spectrum?
    GENERAL I ARTICLE What can we Learn from the Electromagnetic Spectrum? A W Joshi and A 10k Kumar Electromagnetic radiation is all around us, and essential for A W Joshi was at the the survival of alllifeforms. It provides valuable informa­ Department of Physics, University of Pune, Pune. tion about the physical world around us, feeds us by provid­ ing energy to plants, allows us to maintain human metabo­ Alok Kumar is at the lism, and cures us of various diseases. This article deals Department of Physics, with the various properties of electromagnetic radiation, its State University of New sources and detectors, its nature, and its uses. A brief York, USA. discussion on the absorption spectrum of the Earth's atmo­ sphere and the atmospheric windows, and celestial objects seen through optical and radio telescopes is also provided. Introduction Our perception of the physical world around us is largely based on our interaction with the range of the electromagnetic radia­ tion (EMR) that is called visible light. Most objects scatter visible light that enters through the irises of our eyes, falls on our retina, interacts with the retinal pigment that eventually causes an electrical pulse that is transmitted to our brain through optic nerves. We feel warm in front of a fire partly because of a type of electromagnetic radiation that is called infrared radiation. Simi­ larly; our skin gets tanned when exposed to sunlight because of certain electromagnetic radiation called ultraviolet. However, we cannot· see, feel, or detect X-rays using our sense organs. This radiation does penetrate and affect our body.
    [Show full text]
  • Characterization of Fog and Snow Attenuations for Free-Space Optical Propagation
    JOURNAL OF COMMUNICATIONS, VOL. 4, NO. 8, SEPTEMBER 2009 533 Characterization of Fog and Snow Attenuations for Free-Space Optical Propagation Muhammad Saleem Awan*, Laszlo Csurgai Horwath†, Sajid Sheikh Muhammad**, Erich Leitgeb*, Farukh Nadeem*, Muhammad Saeed Khan* *Graz University of Technology, Graz, Austria †Budapest University of Technology and Economics, Budapest, Hungary **National University of Computer and Emerging Sciences (FAST-NU), Lahore, Pakistan Email: [email protected] Abstract— Free Space Optics (FSO) is now a well backbone and the end users. Recently FSO is identified as established access technology, better known for its an attractive alternative to complement microwave robustness in transmitting large data volumes in an energy (mmW) and radio frequency (RF) links within the access efficient manner. However the BER performance of a FSO network for the backhaul traffic [1, 2]. Although, FSO ground-link is adversely affected by cloud coverage, harsh communication links are best served for short distances weather conditions, and atmospheric turbulence. Fog, clouds but such links are successfully tested for relatively long and dry snow play a detrimental role by attenuating optical energy transmitted in terrestrial free-space and thus distance communication links (from medium to long decrease the link availability and reliability. We measured ranges) between e.g., optical ground stations OGS and the time variation of received optical signal level during terminals in space (un-manned aerial vehicles UAVs, high
    [Show full text]
  • Free Space Optical Communications with High Intensity Laser Power Beaming
    Cleveland State University EngagedScholarship@CSU ETD Archive 2011 Free Space Optical Communications with High Intensity Laser Power Beaming Daniel Edward Raible Cleveland State University Follow this and additional works at: https://engagedscholarship.csuohio.edu/etdarchive Part of the Electrical and Computer Engineering Commons How does access to this work benefit ou?y Let us know! Recommended Citation Raible, Daniel Edward, "Free Space Optical Communications with High Intensity Laser Power Beaming" (2011). ETD Archive. 251. https://engagedscholarship.csuohio.edu/etdarchive/251 This Dissertation is brought to you for free and open access by EngagedScholarship@CSU. It has been accepted for inclusion in ETD Archive by an authorized administrator of EngagedScholarship@CSU. For more information, please contact [email protected]. FREE SPACE OPTICAL COMMUNICATIONS WITH HIGH INTENSITY LASER POWER BEAMING DANIEL EDWARD RAIBLE Bachelor of Science in Electrical Engineering Cleveland State University May 2006 Master of Science in Electrical Engineering Cleveland State University May 2008 submitted in partial fulfillment of requirements for the degree DOCTOR OF ENGINEERING at the CLEVELAND STATE UNIVERSITY June 2011 This dissertation has been approved for the Department of Electrical and Computer Engineering and the College of Graduate Studies by ________________________________________________ Dissertation Committee Chairperson, Taysir H. Nayfeh ________________________________ Department/Date ________________________________________________
    [Show full text]