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List Of Stars In Canes Venatici ...
This is the list of notable stars in the constellation Canes Venatici, sorted by decreasing brightness. See also *List of stars by constellation References * * * * * * {{Stars of Canes Venatici *List Canes Venatici Canes Venatici () is one of the 88 constellations designated by the International Astronomical Union (IAU). It is a small northern constellation that was created by Johannes Hevelius in the 17th century. Its name is Latin for 'hunting dogs', and ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Star
A star is an astronomical object comprising a luminous spheroid of plasma held together by its gravity. The nearest star to Earth is the Sun. Many other stars are visible to the naked eye at night, but their immense distances from Earth make them appear as fixed points of light. The most prominent stars have been categorised into constellations and 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 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 total mass is the main factor determining its evolution and eventual fate. A star shines for most of its active life due t ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Alpha2 Canum Venaticorum Variable
An Alpha2 Canum Venaticorum variable (or α2 CVn variable) is a type of variable star. These stars are chemically peculiar main sequence stars of spectral class B8p to A7p. They have strong magnetic fields and strong silicon, strontium, or chromium spectral lines. Their brightness typically varies by 0.01 to 0.1 magnitudes over the course of 0.5 to 160 days. In addition to their intensities, the intensities and profiles of the spectral lines of α2 CVn variables also vary, as do their magnetic fields. The periods of these variations are all equal and are believed to equal the period of rotation of the star. It is thought that they are caused by an inhomogeneous distribution of metals in the atmospheres of these stars, so that the surface of the star varies in brightness from point to point. The type-star which this class is named after is α² Canum Venaticorum, a star in the binary system of Cor Caroli, which is in the northern constellation of Canes Venatici Canes Ven ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HR 5110
HR 5110, also known as BH Canum Venaticorum, is a binary star system in the northern constellation of Canes Venatici. It is visible to the naked eye with an apparent visual magnitude of 4.91. Based upon an annual parallax shift of , it is located 149 light-years away. The system is moving further from the Sun with a heliocentric radial velocity of 6.4 km/s. This is a close binary system with an orbital period of 2.6 days and an orbital plane that is oriented nearly face-on. It may be considered an Algol-type semidetached binary. The hotter primary component has a stellar classification of F2 IV, indicating it is an evolving subgiant star that is leaving the main sequence after consuming the hydrogen at its core. Douglas S. Hall ''et al.'' discovered that HR 5110 is a variable star, in 1978. It was given its variable star designation, BH Canum Venaticorum, in 1981. HR 5110 is classified as a RS Canum Venaticorum variable system, primarily due to chro ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
25 Canum Venaticorum
25 Canum Venaticorum is a binary star system in the northern constellation of Canes Venatici, approximately 199 light years from the Sun. It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of +4.82 The system is moving closer to the Earth with a heliocentric radial velocity of roughly −10 km/s. This is a wide binary system with an orbital period of 228 years and an eccentricity of 0.80. As of 2001, they had a projected separation of . The magnitude 4.98 primary, component A, has a stellar classification of , which matches an A-type giant star. It is 659 million years old with a projected rotational velocity of 235 km/s. This rate of spin is giving the star an oblate shape with an equatorial bulge that is an estimated 27% larger than the polar radius. The companion, component B, is a magnitude 6.95 A-type main-sequence star An A-type main-sequence star (A V) or A dwarf star is a main-sequence (hyd ... [...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, the ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
5 Canum Venaticorum
5 Canum Venaticorum is a probable binary star system in the northern constellation of Canes Venatici, located about 375 light years from the Sun. It is visible to the naked eye as a faint, yellow-hued star with an apparent visual magnitude of +4.77. The system is moving closer to the Earth with a heliocentric radial velocity of −14 km/s. The visible component is an evolved G-type giant star with a stellar classification of . The 'Ba0.3' suffix notation indicates this is a mild barium star, which means that the stellar atmosphere has been enhanced by s-process elements most likely provided by what is now an orbiting white dwarf companion. The primary is 530 million years old with 2.96 times the mass of the Sun and has expanded to about 12 times the Sun's radius. It is radiating 174 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,098 K. In Chinese astronomy, 5 Canum Venaticorum is called 相, Pinyin: Xiāng, m ... [...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 a ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
AW Canum Venaticorum
AW Canum Venaticorum is a variable star in the constellation Canes Venatici. It is visible to the naked eye with a nominal apparent visual magnitude of 4.76. The distance to this star, as measured from its annual parallax shift of , is around 620 light years. It is moving closer with a heliocentric radial velocity of −44 km/s. The variability of the brightness of HR 5219 was announced by Joel Stebbins and Charles Morse Huffer in 1928, based on observations made at Washburn Observatory. It was given its variable star designation, AW Canum Venaticorum, in 1977. At the age of 1.1 billion years, this is an evolved red giant star with a stellar classification of M3- IIIa. It is a slow irregular variable of type Lb, with a brightness that ranges between magnitudes 4.73 and 4.85. The star has 2.2 times the mass of the Sun and has expanded to 117 times the Sun's radius. It is radiating 2,387 times the Sun's luminosity from its enlarged photosphere at an e ... [...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 ampli ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
20 Canum Venaticorum
20 Canum Venaticorum is a single variable star in the northern constellation of Canes Venatici, located 238 light years from the Sun. This object has the variable star designation AO Canum Venaticorum; ''20 Canum Venaticorum ''is the Flamsteed designation. It is visible to the naked eye as a faint, white-hued star with a baseline apparent visual magnitude of +4.72. The star is moving further from the Earth with a heliocentric radial velocity of +9 km/s. Eggen (1971) listed this star as a member of the Hyades Stream. This star has a stellar classification of , which indicates the hydrogen line matches an A-type bright giant but the metal lines are closer to an F-type star. However, it does not appear to be an Am star as the Calcium K line is normal. Earlier, Morgan and Abt (1972) assigned it a giant star class of F3 III. It is classified as a Delta Scuti type variable star with a single radial pulsation mode providing the best fit to the observe ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
24 Canum Venaticorum
24 Canum Venaticorum is a single star in the northern constellation of Canes Venatici, located 277 light years away from the Sun. This object is visible to the naked eye as a faint white-hued star with an apparent visual magnitude of +4.68. It is moving closer to the Earth with a heliocentric radial velocity of −18 km/s. This is an A-type main-sequence star with a stellar classification of A4 V, and it is a shell star with rotationally-broadened lines. It is 310 million years old with a projected rotational velocity of 159 km/s. This rate of spin is giving the star an oblate shape with an equatorial bulge that is 7% larger than the polar radius. The star has 1.74 times the mass of the Sun and 1.9 times the Sun's radius. It is radiating 41 times the Sun's luminosity from its photosphere at an effective temperature of 8,285 K. 24 Canum Venaticorum displays a significant infrared excess at wavelengths of 24μm and 70μm, indicating an orbitin ... [...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, t ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
