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List Of Smallest Stars
This is a list of stars which are the least voluminous known (the smallest stars by volume). List Notable small stars This is a list of small stars that are notable for characteristics that are not separately listed. Smallest stars by type Timeline of smallest red dwarf star recordholders Red dwarfs are considered the smallest star known that are active fusion stars, and are the smallest stars possible that is not a brown dwarf Brown dwarfs (also called failed stars) are substellar objects that are not massive enough to sustain nuclear fusion of ordinary hydrogen ( 1H) into helium in their cores, unlike a main-sequence star. Instead, they have a mass between the most .... Notes References {{Portal bar, Astronomy, Spaceflight, Outer space, Solar System Volume, least ... [...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] |
AR Scorpii
AR Scorpii (AR Sco) is a binary pulsar that consists of a white dwarf and a red dwarf. It is located close to the ecliptic plane in the constellation Scorpius. Parallax measurements made by ''Gaia'' put the system at a distance of about 380 light-years (120 parsecs). AR Scorpii is the first, and as of 2021, the only "white dwarf-pulsar" to be discovered. Its unusual nature was first noticed by amateur astronomers. The 3.56-hour period in AR Scorpii's light curve caused it to be misclassified as a Delta Scuti variable, but in 2016, this period was found to be the binary orbital period. In addition, the system shows very strong optical, ultraviolet, and radio pulsations originating from the red dwarf with a period of just 1.97 minutes, which is a beat period from the orbital rotation and the white dwarf spin. These pulsations occur when a relativistic beam from the white dwarf sweeps across the red dwarf, which then reprocesses the beam into the observed electromagnetic ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
WD 2359−434
WD 2359-434 (Gliese 915, LHS 1005, L 362-81) is a nearby degenerate star (white dwarf) of spectral class DAP5.8, the single known component of the system, located in the constellation Phoenix, the nearest star in this constellation. Distance Currently, the most accurate distance estimate of WD 2359−434 is a trigonometric parallax from Gaia DR3: , corresponding to a distance of , or . WD 2359−434 is the 13th closest white dwarf to the Sun. Physical parameters WD 2359−434's mass is 0.85 ± 0.01 Solar masses, its surface gravity is 108.39 ± 0.01 (2.45 · 108) cm· s−2, or approximately 250,000 of Earth's, corresponding to a radius 6780 km, or 1.06 of Earth's. WD 2359−434 is relatively hot and young white dwarf, its temperature is 8570 ± 50 K; its cooling age, i. e. age as degenerate star (not including lifetime as main sequence star and as giant star) is 1.82 ± 0.06 Gyr. Gliese 518 should appear bluish-white, due temperature, comparable with th ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Procyon B
Procyon () is the brightest star in the constellation of Canis Minor and usually the list of brightest stars, eighth-brightest star in the night sky, with an apparent visual magnitude of 0.34. It has the Bayer designation α Canis Minoris, which is Latinisation of names, Latinized to Alpha Canis Minoris, and abbreviated α CMi or Alpha CMi, respectively. As determined by the European Space Agency ''Hipparcos'' astrometry satellite, this system lies at a distance of just , and is therefore one of Earth's List of nearest stars, nearest stellar neighbors. A binary star system, Procyon consists of a white-hued main-sequence star of spectral type F5 IV–V, designated component A, in orbit with a faint white dwarf companion of spectral type DQZ, named Procyon B. The pair orbit each other with a orbital period, period of 40.84 years and an orbital eccentricity, eccentricity of 0.4. Observation Procyon is usually the eighth-brightest star in the night sky, Culminati ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
40 Eridani
40 Eridani is a triple star system in the constellation of Eridanus, abbreviated 40 Eri. It has the Bayer designation Omicron2 Eridani, which is Latinized from ο2 Eridani and abbreviated Omicron2 Eri or ο2 Eri. Based on parallax measurements taken by the Gaia mission, it is about 16.3 light-years from the Sun. The primary star of the system, designated 40 Eridani A and named Keid, is easily visible to the naked eye. It is orbited by a binary pair whose two components are designated 40 Eridani B and C, and which were discovered on January 31, 1783, by William Herschel. It was again observed by Friedrich Struve in 1825 and by Otto Struve in 1851. In 1910, it was discovered that although component B was a faint star, it was white in color. This meant that it had to be a small star; in fact it was a white dwarf, the first discovered.''White Dwarfs'', E. Schatzman, Amsterdam: North-Holland, 1958. , p. 1 Although it is neither the closest white dwarf, nor the b ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
LB 1497
LB, lb or lb. may refer to: Businesses and organizations * L Brands, an American clothing retailer * Lane Bryant, a plus-size clothing retailer * Laurier Brantford, a satellite campus of Wilfrid Laurier University in Brantford, Ontario, Canada * Movement for Unification ( sq, Lëvizja për Bashkim), a nationalist Albanian political party in Kosovo * Ljubljana Bank ( sl, Ljubljanska banka), a bank named after and based in Ljubljana, Slovenia that operated in SFR Yugoslavia * airline (IATA code) * (''Left Bank'' (online edition), a Ukrainien online newspaper Places *Labrador (former postal abbreviation) *Lebanon (ISO 3166-1 alpha-2 country code) *Long Beach, California *Los Baños, Laguna (an abbreviation commonly used to address the town of Los Baños) Science and technology Mathematics and computing *.lb, the Internet country code top-level domain (ccTLD) for Lebanon *Lattice Boltzmann methods, a class of computational fluid dynamics (CFD) methods for fluid simulation *Liber ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Sirius B
Sirius is the brightest star in the night sky. Its name is derived from the Greek word , or , meaning 'glowing' or 'scorching'. The star is designated α Canis Majoris, Latinized to Alpha Canis Majoris, and abbreviated Alpha CMa or α CMa. With a visual apparent magnitude of −1.46, Sirius is almost twice as bright as Canopus, the next brightest star. Sirius is a binary star consisting of a main-sequence star of spectral type A0 or A1, termed Sirius A, and a faint white dwarf companion of spectral type DA2, termed Sirius B. The distance between the two varies between 8.2 and 31.5 astronomical units as they orbit every 50 years. Sirius appears bright because of its intrinsic luminosity and its proximity to the Solar System. At a distance of , the Sirius system is one of Earth's nearest neighbours. Sirius is gradually moving closer to the Solar System, so it is expected to increase in brightness slightly over the next 60,000 years, reaching a peak magnitude o ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
IK Pegasi
IK Pegasi (or HR 8210) is a binary star system in the constellation Pegasus. It is just luminous enough to be seen with the unaided eye, at a distance of about 154 light years from the Solar System. The primary (IK Pegasi A) is an A-type main-sequence star that displays minor pulsations in luminosity. It is categorized as a Delta Scuti variable star and it has a periodic cycle of luminosity variation that repeats itself about 22.9 times per day. Its companion (IK Pegasi B) is a massive white dwarf—a star that has evolved past the main sequence and is no longer generating energy through nuclear fusion. They orbit each other every 21.7 days with an average separation of about 31 million kilometres, or 19 million miles, or 0.21 astronomical units (AU). This is smaller than the orbit of Mercury (planet), Mercury around the Sun. IK Pegasi B is the Near-Earth supernova, nearest known supernova progenitor candidate. When the primary begins to evolve into a ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
BPM 37093
BPM 37093 (V886 Centauri) is a variable white dwarf star of the DAV, or ZZ Ceti, type, with a hydrogen atmosphere and an unusually high mass of approximately 1.1 times the Sun's. It is about from Earth in the constellation Centaurus and vibrates; these pulsations cause its luminosity to vary. Like other white dwarfs, BPM 37093 is thought to be composed primarily of carbon and oxygen, which are created by thermonuclear fusion of helium nuclei in the triple-alpha process.Late stages of evolution for low-mass stars , Michael Richmond, lecture notes, Physics 230, , accessed online May 3, 2007. [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
GRW +70 8247
GRW +70 8247 is a white dwarf star located 42 light-years from Earth in the constellation Draco. With a magnitude of about 13 it is visible only through a large telescope. Properties Although photographed in the 19th century as part of the Carte du Ciel project, the star was not determined to be a white dwarf until G. P. Kuiper observed it in 1934. This makes it the fifth or sixth white dwarf discovered. At first, its spectrum was thought to be almost featureless, but later observation showed it to have unusual broad, shallow absorption bands. In 1970, when light that it emitted was observed to be circularly polarized, it became the first white dwarf known to have a magnetic field. In the 1980s, it was realized that the unusual absorption bands could be explained as hydrogen absorption lines shifted by the Zeeman effect The Zeeman effect (; ) is the effect of splitting of a spectral line into several components in the presence of a static magnetic field. It is named ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
ZTF J1901+1458
ZTF J1901+1458 (nicknamed Z; formally ZTF J190132.9+145808.7; Gaia ID 4506869128279648512) is a white dwarf, about 135 light years away roughly in the direction of Epsilon Aquilae, discovered by the Zwicky Transient Facility circa 2021. It is the most massive white dwarf yet found, having 1.35 times the mass of the Sun, nearly the largest expected mass for this type of object. Its radius is about , about the size of Earth's Moon, and it rotates once every 7 minutes. The object's extreme rate of spin is hard to explain without supposing Z to be the result of a white dwarf merger, near the upper mass limit of a stable end product. Larger white dwarf mergers could be another mechanism of supernova production, which is not necessarily taken into account in how we have traditionally inferred dark energy In physical cosmology and astronomy, dark energy is an unknown form of energy that affects the universe on the largest scales. The first observational evidence for its existence c ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
