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Angel, Roger

Publications and source records attributed to Angel, Roger.

Static metrology of the meter-scale deformable heliostat

This paper describes a heliostat metrology system which is developed based on deflectometry, utilizing a static perforated panel instead of conventional dynamic monitor displays to provide incident rays. The developed method is named static screen deflectometry (SSD). This robust and scalable method is especially valuable for outdoor tests of large reflectors used in concentrating solar-thermal power (CSP) systems. The developed method has been successfully demonstrated on a 2.4 𝑚 × 3.3 𝑚 float glass deformable reflector bent to focus sunlight at 113 𝑚 distance throughout a day. From images obtained from a camera at 50𝑚 distance, the reflector surface was measured to an accuracy of less than 1 𝑚𝑟𝑎𝑑 rms slope error in the full test scope.

14 SOLAR ENERGY↗

A new class of tandems: Optically coupled III-V/silicon module with outdoor efficiency exceeding 30%

The aim of this project was to introduce a new class of technology—that of high-efficiency silicon-based tandem photovoltaic (PV) modules—that, with follow-on development, has a clear path to reduced levelized cost of electricity (LCOE) for utility-scale power generation. In particular, the objective of the project was to demonstrate the first 30%-efficient III-V/silicon module in outdoor conditions using a tandem geometry in which the sub-cells are detached physically but coupled optically. In present PV power plants installed in the US, the module makes up only approximately one-third of the cost; area-dependent balance-of-systems (BOS) costs such as installation materials, labor, land, and site prep made up an additional third, and area-independent BOS costs round out the final third. With this pricing structure, (annually averaged) module efficiency is a clear market driver: increase the annual energy output per module and the effective costs translated into $/W of both the module and the area-dependent BOS—two-thirds of the total cost—decrease proportionately. However, the dominant PV technology—flat-plate silicon modules—is reaching its theoretical efficiency limit, and thus a tandem technology in which silicon is coupled with a wider-bandgap cell is a promising route to remain responsive to market forces. As it is not trivial to couple silicon with other cells in conventional two-terminal geometries due to, e.g., lattice mismatch, this project introduced a new, four-terminal configuration using a “PVMirror.” A PVMirror utilizes PV cells as a three-in-one technology—they act as a concentrating mirror, spectrum splitter, and high-efficiency light-to-electricity converter. Light is incident upon a full-aperture dichroic mirror that reflects visible light and transmits infrared light. The transmitted light is absorbed in silicon PV cells that are placed behind the dichroic mirror and that convert IR photons to electricity with high efficiency. The dichroic mirror and silicon PV cells are affixed to a curved glass trough that tracks the sun about a single, North-South axis such that the reflected VIS light is concentrated at a common line focus, at which is placed a second, wider-bandgap GaAs PV cell having high efficiency at shorter wavelengths. The innovation of PVMirrors lies in their design, which maximizes annual energy output and minimizes the constraints placed on the sub-cells. In particular, the cells are free of lattice- and current-matching restrictions, neither cell requires a transparent rear electrode, and either sub-cell can be placed at the focus depending on their relative costs. Furthermore, the greatest benefit of PVMirrors is that they make use of a portion of the diffuse light whereas concentrator tandems cannot. This results in a benefit in energy yield and extends PVMirrors’ competitive range. Over the course of this one-year project, a silicon PVMirror and GaAs receiver were fabricated, characterized, and placed outdoors on a sun tracker, where the efficiency of the tandem “module” was measured for three days. Notable results include the first demonstration of this flexible tandem configuration, a maximum tandem efficiency of 29.6% (just shy of the 30% overall project goal), successful conversion of diffuse light into electricity, a thorough loss analysis indicating a path to over 31% efficiency, and a roadmap to cost-competitive PVMirror tandems using a wide-bandgap polycrystalline PVMirror and a silicon receiver. Development of a >18%-efficient wide-bandgap polycrystalline cell—the key enabler of this envisioned tandem—should be a future research focus. This project has laid the groundwork for a PV technology that, with continued development, has the potential to reach LCOEs as low as $0.03/kWh according to our calculations. Such a system would provide the public with inexpensive, clean solar power.

32 ENERGY CONSERVATION, CONSUMPTION, AND UTILIZATI↗

Sensitivity of nulling interferometers to extra-solar zodiacal emission (EZE)

It should be possible to discover and to analyze the atmospheres of Earth-like planets of nearby stars, provided their thermal emission is not overwhelmed by a bright zodiacal cloud in the same system. Nulling interferometers in space, such as the Terrestrial Planet Finder, can efficiently suppress a stellar point source, but there is no way to suppress diffuse emission underlying the planet under study. A cloud much brighter than solar level would cause serious reduction in sensitivity, by its photon shot noise. Since some clouds have been detected that are orders of magnitude brighter, zodiacal measurements of TPF candidates to solar level are critically needed. These could be obtained relatively soon with the largest aperture ground-based interferometers observing in the 10 micron atmospheric window. A cloud would be detectable as an infrared excess, provided the stellar emission (some 10(exp 4) times brighter) is adequately suppressed by destructive interference. Ideally, the ground interferometer should have angular response similar to that of TPF, so as to measure directly the troublesome zodiacal component. The individual elements must be large, for even with approx. 8 m apertures, star cancellation and low thermal background, integration times of at least several hours will be needed to sense the clouds against shot noise from telescope thermal emission. In this paper we compare the sensitivity of TPF and ground based interferometers to a twin of the solar system at 10 pc, using Good's (1994) model of the zodiacal cloud.

Angel, Roger↗

A Road Map for the Exploration of Neighboring Planetary Systems (ExNPS)

A brown dwarf star having only 20-50 times the mass of Jupiter is located below and to the left of the bright star GL 229 in this image from the Hubble Space Telescope. At the 19 light year distance to GL 229, the 7.7-arcsec separation between the star and the brown dwarf corresponds to roughly the separation between Pluto and the Sun in our Solar System. The goal of the program described in this report is to detect and characterize Earth-like planets around nearby stars where conditions suitable for life might be found. For a star like the Sun located 30 light years away, the appropriate star-planet separation would be almost 100 times closer than seen here for GL 229B.

Elachi, Charles↗

Fabrication

What aspects of optical fabrication technology need to be developed so as to facilitate existing planned missions, or enable new ones? Throughout the submillimeter to UV wavelengths, the common goal is to push technology to the limits to make the largest possible apertures that are diffraction limited. At any one wavelength, the accuracy of the surface must be better than lambda/30 (rms error). The wavelength range is huge, covering four orders of magnitude from 1 mm to 100 nm. At the longer wavelengths, diffraction limited surfaces can be shaped with relatively crude techniques. The challenge in their fabrication is to make as large as possible a reflector, given the weight and volume constraints of the launch vehicle. The limited cargo diameter of the shuttle has led in the past to emphasis on deployable or erectable concepts such as the Large Deployable Reflector (LDR), which was studied by NASA for a submillimeter astrophysics mission. Replication techniques that can be used to produce light, low-cost reflecting panels are of great interest for this class of mission. At shorter wavelengths, in the optical and ultraviolet, optical fabrication will tax to the limit the most refined polishing methods. Methods of mechanical and thermal stabilization of the substrate will be severely stressed. In the thermal infrared, the need for large aperture is tempered by the even stronger need to control the telescope's thermal emission by cooled or cryogenic operation. Thus, the SIRTF mirror at 1 meter is not large and does not require unusually high accuracy, but the fabrication process must produce a mirror that is the right shape at a temperature of 4 K. Future large cooled mirrors will present more severe problems, especially if they must also be accurate enough to work at optical wavelengths. At the very shortest wavelengths accessible to reflecting optics, in the x-ray domain, the very low count fluxes of high energy photons place a premium on the collecting area. It is not necessary to reach or even approach the diffraction limit, which would demand subnanometer fabrication and figure control. Replication techniques that produce large very lightweight surfaces are of interest for x-ray optics just as they are for the submillimeter region. Optical fabrication requirements are examined in more detail for missions in each of the three spectral regions of interest in astrophysics.

Angel, Roger↗