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9 Lyncis ...
This is the list of notable stars in the constellation Lynx, sorted by decreasing brightness. See also *List of stars by constellation References * * * {{Stars of Lynx *List Lynx A lynx is a type of wild cat. Lynx may also refer to: Astronomy * Lynx (constellation) * Lynx (Chinese astronomy) * Lynx X-ray Observatory, a NASA-funded mission concept for a next-generation X-ray space observatory Places Canada * Lynx, Ontar ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Star
A star is an astronomical object comprising a luminous spheroid of plasma (physics), plasma held together by its gravity. The List of nearest stars and brown dwarfs, nearest star to Earth is the Sun. Many other stars are visible to the naked eye at night sky, night, but their immense distances from Earth make them appear as fixed stars, fixed points of light. The most prominent stars have been categorised into constellations and asterism (astronomy), asterisms, and many of the brightest stars have proper names. Astronomers have assembled star catalogues that identify the known stars and provide standardized stellar designations. The observable universe contains an estimated to stars. Only about 4,000 of these stars are visible to the naked eye, all within the Milky Way galaxy. A star's life star formation, begins with the gravitational collapse of a gaseous nebula of material composed primarily of hydrogen, along with helium and trace amounts of heavier elements. Its stellar ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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. Many, possibly most, stars have at least some variation in luminosity: the energy output of the Sun, for example, varies by about 0.1% over an 11-year solar cycle. Discovery An ancient Egyptian calendar of lucky and unlucky days composed some 3,200 years ago may be the oldest preserved historical document of the discovery of a variable star, the eclipsing binary Algol. Of the modern astronomers, th ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
12 Lyncis
12 Lyncis, abbreviated 12 Lyn, is a triple star system in the constellation Lynx. It is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of 4.87. When seen through a telescope, it can be separated into three stars: two components with magnitudes 5.4 and 6.0 that lie at an angular separation by 1.8 ″ (as of 1992) and a yellow-hued star of magnitude 7.2 at a separation of 8.6″ (as of 1990). The orbit of the two brighter stars is not known with certainty, but appears to have a period of somewhere around 700 to 900 years. The pair have a projected separation of . Parallax Parallax is a displacement or difference in the apparent position of an object viewed along two different lines of sight and is measured by the angle or semi-angle of inclination between those two lines. Due to foreshortening, nearby objects ... indicates the system is light years distant from Earth. References {{DEFAULTSORT:12 Lyncis A-type main-s ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 82741
HD 82741 is a single star in the northern constellation of Lynx. It is visible to the naked eye with an apparent visual magnitude of 4.81. The distance to HD 82741 is 223 light years, as determined from its annual parallax shift of . It is moving further from the Earth with a heliocentric radial velocity of 1 km/s. At the age of 2.74 billion years, this is an evolved giant star with a stellar classification of , where the suffix notation indicates an underabundance of iron in its atmosphere. It belongs to a sub-category of giants called the red clump, indicating that it is on the horizontal branch and is generating energy through the fusion of helium at its core. With 1.62 times the mass of the Sun, it has expanded to 11 times the Sun's radius. It is radiating 58.9 times the Sun's luminosity from its enlarged photosphere at an effective temperature The effective temperature of a body such as a star or planet is the temperature of a black body that would e ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
27 Lyncis
27 Lyncis is a single star in the northern constellation of Lynx. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 4.78. This object is located around 250 light years away from the Sun, as determine from parallax measurements. It is moving further from the Sun with a heliocentric radial velocity of +11 km/s. This is an ordinary A-type main-sequence star with a stellar classification of A2 V, which indicates it is generating energy through hydrogen fusion at its core. It is 157 million years old and is spinning with a projected rotational velocity of 183. The star has 2.24 times the mass of the Sun and is radiating 65 times the Sun's luminosity from its photosphere at an effective temperature of 10,014 K. X-ray emission Astrophysical X-ray sources are astronomical objects with physical properties which result in the emission of X-rays. Several types of astrophysical objects emit X-rays. They incl ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
21 Lyncis
21 Lyncis is a single star in the northern constellation of Lynx. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 4.61. The star is located at a distance of about 274 light years away from the Sun, based on parallax. It is moving further away from the Earth with a heliocentric radial velocity of around +27 km/s. This object is an ordinary A-type main-sequence star with a stellar classification of A0.5Vs, where the 's' suffix indicates "sharp" lines in the spectrum, usually due to slow rotation. It is about 272 million years old with a projected rotational velocity of 18 km/s. The star has 2.22 times the mass of the Sun and is radiating 102 times the luminosity of the Sun from its photosphere at an effective temperature The effective temperature of a body such as a star or planet is the temperature of a black body that would emit the same total amount of electromagnetic radiation. Effective temperature ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 77912
HD 77912 is a single star in the northern constellation of Lynx. It is visible to the naked eye with an apparent visual magnitude of 4.56. The star is located 650 light years from the Sun, as determined from its annual parallax shift of . It is moving further away with a heliocentric radial velocity of +16.6 km/s. HD 77912 has a peculiar velocity of , which may mark it as a runaway star. The stellar classification of HD 77912 is , indicating it is a bright giant with a mild overabundance of barium. It has 4.6 times the mass of the Sun and has expanded to 33 times the Sun's radius. The star is radiating 1,168 times the Sun's luminosity from its enlarged photosphere at an effective temperature The effective temperature of a body such as a star or planet is the temperature of a black body that would emit the same total amount of electromagnetic radiation. Effective temperature is often used as an estimate of a body's surface temperature ... of 4,899 K. R ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Delta Scuti Variable
A Delta Scuti variable (sometimes termed dwarf cepheid when the V-band amplitude is larger than 0.3 mag.) is a subclass of young pulsating star. These variables as well as classical cepheids are important standard candles and have been used to establish the distance to the Large Magellanic Cloud, globular clusters, open clusters, and the Galactic Center. The variables follow a period-luminosity relation in certain passbands like other standard candles such as Cepheids. SX Phoenicis variables are generally considered to be a subclass of Delta Scuti variables that contain old stars, and can be found in globular clusters. SX Phe variables also follow a period-luminosity relation. One last sub-class are the pre-main sequence (PMS) Delta Scuti variables. The OGLE and MACHO surveys have detected nearly 3000 Delta Scuti variables in the Large Magellanic Cloud. Typical brightness fluctuations are from 0.003 to 0.9 magnitudes in V over a period of a few hours, although the amplitude ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Eclipsing Binary
A binary star is a system of two stars that are gravitationally bound to and in orbit around each other. Binary stars in the night sky that are seen as a single object to the naked eye are often resolved using a telescope as separate stars, in which case they are called ''visual binaries''. Many visual binaries have long orbital periods of several centuries or millennia and therefore have orbits which are uncertain or poorly known. They may also be detected by indirect techniques, such as spectroscopy (''spectroscopic binaries'') or astrometry (''astrometric binaries''). If a binary star happens to orbit in a plane along our line of sight, its components will eclipse and transit each other; these pairs are called ''eclipsing binaries'', or, together with other binaries that change brightness as they orbit, ''photometric binaries''. If components in binary star systems are close enough they can gravitationally distort their mutual outer stellar atmospheres. In some cases, these ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
2 Lyncis
2 Lyncis is a binary star system in the northern constellation Lynx. It is visible to the naked eye, having an apparent visual magnitude of 4.44. The distance to this system, judging by an annual parallax shift of , is around 157 light years. It is moving closer to the Sun with a heliocentric radial velocity of −2 km/s. This is a spectroscopic binary star system with an orbital period of around 3.6 years and an eccentricity of 0.5. It is classified as a probable (91% chance) eclipsing binary with the variable star designation UZ Lyn, showing a net magnitude decrease of 0.3 during an occultation. The primary component is an A-type main-sequence star with a stellar classification of A2 Vs, where the 's' indicates narrow (sharp) absorption lines. The orbiting companion may be the source of the X-ray emission Astrophysical X-ray sources are astronomical objects with physical properties which result in the emission of X-rays. Several types o ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
15 Lyncis
15 Lyncis is a binary star system in the northern constellation of Lynx. It is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of 4.35. Based on the system's parallax, it is located 178 light-years (54.7 parsecs) away. The pair are moving away from the Earth with a heliocentric radial velocity of +2 km/s. A telescope reveals it is formed by two yellowish stars of magnitudes 4.7 and 5.8 that are 0.9 arcseconds apart. The two stars orbit each other every 262 years and the orbital eccentricity is 0.74. The components are a magnitude 4.7 evolved giant star of spectral type G8III, and a magnitude 5.8 F-type main-sequence star of spectral type F8V. The former has exhausted the hydrogen at its core, causing it to expand to 8 times the Sun's radius. It is radiating 40 times the luminosity of the Sun from its enlarged photosphere at an effective temperature The effective temperature of a body such as a star or planet is the t ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Semiregular Variable
In astronomy, a semiregular variable star, a type of variable star, is a giant or supergiant of intermediate and late (cooler) spectral type showing considerable periodicity in its light changes, accompanied or sometimes interrupted by various irregularities. Periods lie in the range from 20 to more than 2000 days, while the shapes of the light curves may be rather different and variable with each cycle. The amplitudes may be from several hundredths to several magnitudes (usually 1-2 magnitudes in the V filter). Classification The semiregular variable stars have been sub-divided into four categories for many decades, with a fifth related group defined more recently. The original definitions of the four main groups were formalised in 1958 at the tenth general assembly of the International Astronomical Union (IAU). The General Catalogue of Variable Stars (GCVS) has updated the definitions with some additional information and provided newer reference stars where old examples such ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
