HD 6114
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DiamondDiamond is a solid form of the element carbon with its atoms arranged in a crystal structure called diamond cubic. Diamond is tasteless, odourless, strong, brittle solid, colourless in pure form, a poor conductor of electricity, and insoluble in water. Another solid form of carbon known as graphite is the chemically stable form of carbon at room temperature and pressure, but diamond is metastable and converts to it at a negligible rate under those conditions. Diamond has the highest hardness and thermal conductivity of any natural material, properties that are used in major industrial applications such as cutting and polishing tools. Because the arrangement of atoms in diamond is extremely rigid, few types of impurity can contaminate it (two exceptions are boron and nitrogen). Small numbers of defects or impurities (about one per million of lattice atoms) can color a diamond blue (boron), yellow (nitrogen), brown (defects), green (radiation exposure), purple, pink, orange, or red. Diamond also has a very high refractive index and a relatively high optical dispersion. Most natural diamonds have ages between 1 billion and 3.5 billion years. Most were formed at depths between 150 and 250 kilometres (93 and 155 mi) in the Earth's mantle, although a few have come from as deep as 800 kilometres (500 mi). Under high pressure and temperature, carbon-containing fluids dissolved various minerals and replaced them with diamonds. Much more recently (hundreds to tens of million years ago), they were carried to the surface in volcanic eruptions and deposited in igneous rocks known as kimberlites and lamproites. Synthetic diamonds can be grown from high-purity carbon under high pressures and temperatures or from hydrocarbon gases by chemical vapor deposition (CVD). Natural and synthetic diamonds are most commonly distinguished using optical techniques or thermal conductivity measurements.
List of stars in AndromedaThis is the list of notable stars in the constellation Andromeda, sorted by decreasing brightness. Notes
List of brown dwarfsThis is a list of notable brown dwarfs. These are objects that have masses between heavy gas giants and low-mass stars. The first isolated brown dwarf discovered was Teide 1 in 1995. The first brown dwarf discovered orbiting a star was Gliese 229 B, also discovered in 1995. The first brown dwarf found to have a planet was 2M1207, discovered in 2004. As of 2015, more than 2,800 brown dwarfs have been identified. An isolated object with less than about 13 Jupiter masses is technically a sub-brown dwarf or rogue planet. Because the mass of a brown dwarf is between that of a planet and that of a star, they have also been called planetars or hyperjovians. Various catalog designations have been used to name brown dwarfs. Brown dwarfs with names ending in a letter such as B, C, or D are in orbit around a primary star; those with names ending in a lower-case letter such as b, c, or d, may be exoplanets (see Exoplanet naming convention). Some exoplanets, especially those detected by radial velocity, can turn out to be brown dwarfs if their mass is higher than originally thought: most have only known minimum masses because the inclination of their orbit is not known. Examples include HD 114762 b (>11.68 MJ), Pi Mensae b (>10.312 MJ), and NGC 2423-3 b (>10.6 MJ). A complete list of more than 3000 ultracool dwarfs, which includes brown dwarfs and low-mass stars, is being maintained by astronomers. It is called the UltracoolSheet. The same team also produced a list of 1000 ultracool dwarfs with their mass being determined.
HD 8673HD 8673 is a binary star in the northern constellation of Andromeda. It has an apparent magnitude and absolute magnitude of 6.34 and 3.56 respectively. Based upon an annual parallax shift of 26.2 mas, the system is located around 124.5 light years away. The system is moving further from the Earth with a heliocentric radial velocity of +19 km/s. A sub-stellar companion was detected in 2005; it could either be an exoplanet or a brown dwarf. The primary component is an F-type main-sequence star with a stellar classification of F7 V. It has 1.36 times the mass of the Sun and 1.52 times the Sun's radius. The star is around 1.5 billion years old and is spinning with a projected rotational velocity of 26.9 km/s. It is radiating 3.4 times the Sun's luminosity from its photosphere at an effective temperature of 6,340 K. Speckle interferometry measurements of this star between 2001 and 2008 showed a candidate stellar companion to this star, announced in 2011. It was unclear whether the pair formed a visual double or a binary system. The authors of the study estimated a class of K2 V, based upon a visual magnitude difference of 2.3±0.5. Subsequent observations using adaptive options did not spot this companion and it was concluded this was a false detection. However, a low mass stellar companion was detected in a wide orbit. This red dwarf star has 0.33–0.45 times the mass of the Sun and is orbiting with a semimajor axis of 35–60 AU.
HD 6114HD 6114 is a visual binary star system in the northern constellation of Andromeda. With a combined apparent magnitude of 6.46, the star can only be seen with the naked eye by keen-eyed observers even on the best of nights. Based upon an annual parallax shift of 10.4 mas as seen from Earth's orbit, the system is located approximately 108 parsecs (350 ly) distant. The binary nature of this system was discovered by O. Struve in 1864. It consists of a magnitude 6.76 primary component with a dimmer magnitude 8.07 secondary. As of 2015 the pair had an angular separation of 1.30″ along a position angle of 175°. The two stars orbit each other with a period of 450 years with an eccentricity of 0.80. The primary is an A-type main-sequence star with a stellar classification of A9 V. At the estimated age of 863 million years, it is spinning rapidly with a projected rotational velocity of 149 km/s. The star has 1.65 times the mass of the Sun and is radiating 21 times the Sun's luminosity from its photosphere at an effective temperature of 7,611 K.
Skylake (microarchitecture)Skylake is Intel's codename for its sixth generation Core microprocessor family that was launched on August 5, 2015, succeeding the Broadwell microarchitecture. Skylake is a microarchitecture redesign using the same 14 nm manufacturing process technology as its predecessor, serving as a tock in Intel's tick–tock manufacturing and design model. According to Intel, the redesign brings greater CPU and GPU performance and reduced power consumption. Skylake CPUs share their microarchitecture with Kaby Lake, Coffee Lake, Whiskey Lake, and Comet Lake CPUs. Skylake is the last Intel platform on which Windows earlier than Windows 10 are officially supported by Microsoft, although enthusiast-created modifications are available that disabled the Windows Update check and allowed Windows 8.1 and earlier to continue to receive Windows Updates on this and later platforms. Some of the processors based on the Skylake microarchitecture are marketed as sixth-generation Core. Intel officially declared end of life and discontinued Skylake LGA 1151 CPUs (except i3-6100, i5-6500, and Xeon E3 v5) on March 4, 2019.
Helen SwordHelen Claire Sword is a New Zealand academic, specialising in modernist poetry and academic writing, and is an emeritus professor at the University of Auckland. She was elected as a Fellow of the Royal Society Te Apārangi in 2023.
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