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Publication

Three-Dimensional Writing of Conducting Polymer Nanowire Arrays by Meniscus-Guided Polymerization

Giorgio Margaritondo
2011
Journal Articles

Abstract

Accurate and versatile three-dimensional writing of individually controlled conducting polymer nanodevices forming dense arrays is demonstrated by guiding a monomer meniscus in pulling a micropipette during oxidative polymerization. We specifically demonstrate well-defined dense arrays of various freestanding nano-components with controlled radius down to similar to 50 nm: straight wires, nanowires with variable radius, branches, and bridges.

Official source

Giorgio Margaritondo
2011
Journal Articles

Abstract

Official source

Related concepts (9)

Variable star

A variable star is a star whose brightness as seen from Earth (its apparent magnitude) changes with time. This variation may be caused by a change in emitted light or by something partly blocking the light, so variable stars are classified as either: Intrinsic variables, whose luminosity actually changes; for example, because the star periodically swells and shrinks. Extrinsic variables, whose apparent changes in brightness are due to changes in the amount of their light that can reach Earth; for example, because the star has an orbiting companion that sometimes eclipses it.

Cepheid variable

A Cepheid variable (ˈsɛfi.ɪd,_ˈsiːfi-) is a type of variable star that pulsates radially, varying in both diameter and temperature. It changes in brightness, with a well-defined stable period and amplitude. Cepheids are important cosmic benchmarks for scaling galactic and extragalactic distances. A strong direct relationship exists between a Cepheid variable's luminosity and its pulsation period. This characteristic of classical Cepheids was discovered in 1908 by Henrietta Swan Leavitt after studying thousands of variable stars in the Magellanic Clouds.

Mira variable

Mira variables ˈmaɪrə (named for the prototype star Mira) are a class of pulsating stars characterized by very red colours, pulsation periods longer than 100 days, and amplitudes greater than one magnitude in infrared and 2.5 magnitude at visual wavelengths. They are red giants in the very late stages of stellar evolution, on the asymptotic giant branch (AGB), that will expel their outer envelopes as planetary nebulae and become white dwarfs within a few million years.