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List Of Stars In Leo Minor ...
This is the list of notable stars in the constellation Leo Minor, sorted by decreasing brightness. See also *List of stars by constellation References * * * * * {{Stars of Leo Minor *List Leo Minor Leo Minor is a small and faint constellation in the northern celestial hemisphere. Its name is Latin for "the smaller lion", in contrast to Leo, the larger lion. It lies between the larger and more recognizable Ursa Major to the north and Le ... [...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] |
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] |
11 Leonis Minoris
11 Leonis Minoris is a binary star located 36.5 light years away from Earth, in the northern constellation of Leo Minor. It is visible to the naked eye as a dim, yellow-hued star with an apparent visual magnitude of 5.54. The system is moving away from the Earth with a heliocentric radial velocity of +14.4 km/s. It has a relatively high proper motion, traversing the celestial sphere at the rate of 0.764 arc seconds per annum. The primary component is a G-type main-sequence star with a stellar classification of G8V, which is slightly less massive and slightly dimmer than the Sun. This is an RS Canum Venaticorum variable star with its luminosity varying by 0.033 magnitudes over a period of 18 days. Compared to the Sun, it has more than double the abundance of elements more massive than helium—what astronomers term the star's metallicity. There is a secondary component, a 14th magnitude red dwarf star much dimmer than the primary. The pair have an orbital ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
20 Leonis Minoris
20 Leonis Minoris is a binary star system in the northern constellation of Leo Minor. It is faintly visible to the naked eye, having an apparent visual magnitude of +5.4. Based upon an annual parallax shift of 66.46 mas, it is located 49 light years from the Sun. The star has a relatively high proper motion and is moving away from the Sun with a radial velocity of +56 km/s. The system made its closest approach about 150,000 years ago when it came within . The primary member of this system is a G-type main-sequence star with a stellar classification of . It has 12% more mass and a 25% larger radius than the Sun. The star is about seven billion years old and is spinning with a rotation period of 10.6 days. The small companion is an active red dwarf star that has a relatively high metallicity. The two stars are currently separated by 14.5 arc seconds, corresponding to a projected separation of 2016 AU. In 2020, a candidate exoplanet was det ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
42 Leonis Minoris
42 Leonis Minoris (42 LMi) is a solitary, bluish-white hued star located in the northern constellation Leo Minor. It has a visual apparent magnitude of 5.35, allowing it to be faintly seen with the naked eye. Parallax measurements place it at a distance of 412 light years. The object has a heliocentric radial velocity of , indicating that it is drifting away from the Solar System. 42 LMi has a general stellar classification of B9 V, indicating that it is an ordinary B-type main-sequence star. However, Cowley et al. (1969) gave a slightly cooler class of A1 Vn, indicating that it is instead an A-type main-sequence star with 'nebulous' (broad) absorption lines due to rapid rotation. Nevertheless, it has 2.77 times the mass of the Sun and a radius of . It radiates at 107 times the luminosity of the Sun from its photosphere at an effective temperature of . Its high luminosity and slightly enlarged diameter suggests that the object might be evolved. Like most hot stars, 42 LMi ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
19 Leonis Minoris
19 Leonis Minoris (19 LMi) is a spectroscopic binary located in the northern constellation Leo Minor. It has an apparent magnitude of 5.1, making it one of the brighter members of the constellation. The system is relatively close at a distance of 94 light years but is drifting closer with a heliocentric radial velocity of . This spectroscopic binary can be classified as single lined because only the primary's spectrum can be observed clearly, with it having a stellar classification of F6 V. This makes it an ordinary F-type main-sequence star. The companion is probably a G-type main-sequence star of G0, having a mass 101% that of the Sun. The pair have a relatively circular orbit of about 9 days. 19 LMi has 129% the mass of the Sun and an effective temperature of , giving a yellow white hue. The object is somewhat evolved at an age of 2.5 billion years, having a slightly enlarged radius of and a luminosity of , high for its class. 19 LMi has an iron abundance 123% tha ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
41 Leonis Minoris
41 Leonis Minoris is a single star in the northern constellation Leo Minor, located near the southern border with the neighboring constellation of Leo. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 5.08. This object is located approximately 229 light years away from the Sun, based on parallax, and is drifting further away with a radial velocity of +18.5 km/s. This is an ordinary A-type main-sequence star with a stellar classification of A3Vn, where the 'n' suffix indicates "nebulous" (broadened) lines due to rapid rotation. It is about 182 million years old with a high projected rotational velocity of 201 km/s. The star has 2.5 times the mass of the Sun and 2.1 times the Sun's radius. It is radiating 55 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 t ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
30 Leonis Minoris
30 Leonis Minoris is a single star in the northern constellation of Leo Minor. It is visible to the naked eye as a faint, white-hued point of light with an apparent visual magnitude of 4.72. The distance to this star, as estimated from parallax measurements, is 233 light years. It is drifting away from the Earth with a heliocentric radial velocity of +13.7 km/s. This object has been catalogued as an Am star and was given a stellar classification of kF0hF2mF2 by Abt and Morrell (1995). This notation indicates the calcium K line matches an F0 star, while the hydrogen and metal lines fit an F2 star. However, Gray et al. (2001) assigned it a class of A9IIIa, matching an A-type giant star. 30 Leonis Minoris has 2.3 times the mass of the Sun and 4.2 times the Sun's radius. It has a moderate rate of spin, showing a projected rotational velocity of 34 km/s. The star is radiating 58 times the Sun's luminosity from its photosphere at an effective temperature T ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
37 Leonis Minoris
37 Leonis Minoris is a single, yellow-hued star in the northern constellation of Leo Minor. It is faintly visible to the naked eye with an apparent visual magnitude of 4.68. The star is moving closer to the Sun with a heliocentric radial velocity of −8 km/s. The annual parallax shift of provides a distance estimate of roughly 580 light years. The Bright Star Catalogue lists this star with a stellar classification of G2.5 IIa, indicating it is an evolved G-type bright giant. Gray et al. (2001) gave it a class of G1 II, while Keenan and McNeil (1989) assigned this star to the giant class G2.5 IIIa. It has an estimated 3.72 times the mass of the Sun and about 31 times the Sun's radius. The star is around 200 million years old with a projected rotational velocity of 6.4 km/s. It is radiating about 438 times the Sun's luminosity from its enlarged photosphere at an effective temperature The effective temperature of a body such as a star o ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
RS Canum Venaticorum Variable
An RS Canum Venaticorum variable is a type of variable star. The variable type consists of close binary stars having active chromospheres which can cause large stellar spots. These spots are believed to cause variations in their observed luminosity. Systems can exhibit variations on timescales of years due to variation in the spot surface coverage fraction, as well as periodic variations which are, in general, close to the orbital period of the binary system. Some systems exhibit variations in luminosity due to their being eclipsing binaries. Typical brightness fluctuation is around 0.2 magnitudes. They take their name from the star RS Canum Venaticorum (abbreviated RS CVn). Otto Struve (1946) first called attention to the group, but it was Oliver (1974) who was the first to formally propose a set of observational characteristics to define the RS CVn criteria. The working definition, as it is used today, was that set down by Hall (1976). Berdyuginabr>2.4 RS CVn stars/ref> The ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
10 Leonis Minoris
10 Leonis Minoris is a single variable star in the northern constellation Leo Minor, located approximately 191 light years away based on parallax. It has the variable star designation SU Leonis Minoris; ''10 Leonis Minoris'' is the Flamsteed designation. This body is visible to the naked eye as a faint, orange-hued star with a baseline apparent visual magnitude of 4.54. It is moving closer to the Earth with a heliocentric radial velocity of −12 km/s. This is an evolved giant star with a stellar classification of G8.5 III. It is reported as a RS CVn variable with magnitude varying by 0.02 mag. and showing a high level of chromospheric activity. The star has 2.54 times the mass of the Sun and has expanded to 8.7 times the Sun's radius. It is radiating 46 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 5,099 K. References {{DEFAULTSORT:10 Leonis Minoris G-type giants RS Canum Venaticorum variables ... [...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] |
