|
Omicron Velorum Cluster
IC 2391 (also known as the Omicron Velorum Cluster or Caldwell 85) is an open cluster in the constellation Vela. The Persian astronomer Al Sufi may have first described it about 964. It was found by Abbe Lacaille and cataloged as Lac II 5. The cluster is about 500 light-years away from Earth and can be seen with the naked eye. It contains about 30 stars with a total visual magnitude of 2.5, spread out along 50 arcminutes. It includes the following naked-eye members: * ο Velorum * HD 74560 (HY Velorum) * HD 74146 (NZ Velorum) * HD 74071 (HW Velorum) * HD 74196 * HD 74535 (KT Velorum) * HD 75466 * HD 73952 IC 2391 appears to be about the same age as the open cluster IC 2602, and has a lithium depletion boundary age of about 50 million years. IC 2391 has been closely linked to the Argus Association of co-moving stars. Proposed members of this moving group include Denebola, Epsilon Pavonis, 49 Ceti, HD 61005, and HD 88955. IC 2391 also includes HD 74438, the youn ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Vela (constellation)
Vela is a constellation in the southern sky, which contains the Vela Supercluster. Its name is Latin for the sails of a ship, and it was originally part of a larger constellation, the ship ''Argo Navis'', which was later divided into three parts, the others being Carina and Puppis. With an apparent magnitude of 1.8, its brightest star is the hot blue multiple star Gamma Velorum, one component of which is the brightest Wolf-Rayet star in the sky. Delta and Kappa Velorum, together with Epsilon and Iota Carinae, form the asterism known as the False Cross. 1.95-magnitude Delta is actually a triple or quintuple star system. History Argo Navis was one of the 48 classical constellations listed by the 2nd-century astronomer Ptolemy, and represented the ship '' Argo'', used by Jason and the Argonauts on their quest for the Golden Fleece in Greek mythology. German cartographer Johann Bayer depicted the constellation on his ''Uranometria'' of 1603, and gave the stars Bayer desig ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 61005
HD 61005, also known as HIP 36948, is a young star located in the southern constellation Puppis, the poop deck. It has an apparent magnitude of 8.22, making it readily visible in binoculars, but not to the naked eye. The object is located relatively close at a distance of 119 light years based on Gaia DR3 parallax measurements but is receding with a heliocentric radial velocity of . Characteristics HD 61005 has a stellar classification of G8 Vk, indicating that it is a yellow dwarf with interstellar absorption features in its spectrum. However, it is younger than the Sun at an age of 30 million years. Other studies place it an older age, ranging from 135 million years to 2 billion years. Nevertheless, the star retains a protoplanetary disk - the accumulation of the gas-dust matter, forming a planetary system. HD 61005 is located in the Local Bubble, a region with a low concentration of dust clouds. It is suspected to be a member of the Argus association. It has ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
49 Ceti
49 Ceti is a single star in the equatorial constellation of Cetus. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 5.607. The star is located away from the Solar System, based on its parallax, and is drifting further away with a radial velocity of +10 km/s. 49 Ceti has been identified as a member of the 40-million-year-old Argus Association. This is a young A-type main-sequence star with a stellar classification of A1V. It is about 40 million years old with a high rate of spin, showing a projected rotational velocity of 196 km/s. The star has double the mass of the Sun. It is radiating 19 times the Sun's luminosity from its photosphere at an effective temperature of 8,790 K. 49 Ceti displays a significant infrared excess, which is a characteristic of a debris disk orbiting the star. Unusually, the disk seems to be gas-rich, with evidence of carbon monoxide (CO) gas. This carbon monoxide gas may possibly b ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Epsilon Pavonis
Epsilon Pavonis, Latinized from ε Pavonis, is a single, white-hued star in the constellation Pavo. It can be viewed with the naked eye, having an apparent visual magnitude of 3.97. The annual parallax shift of 31.04 mas provides a distance estimate of 105 light years from the Sun. This star is a member of the proposed Argus Association, a young moving group of more than 60 stars associated with the IC 2391 cluster. Epsilon Pavonis is moving closer to the Sun with a radial velocity of −6.7 km/s. With a stellar classification of A0 Va, Epsilon Pavonis is an ordinary A-type main-sequence star that is generating energy through hydrogen fusion at its core. It is just 27 million years old with a projected rotational velocity of 85 km/s. The star has 2.2 times the mass of the Sun and 1.74 the Sun's radius. It is radiating 32 times the Sun's luminosity from its photosphere at an effective temperature The effective temperature of a body such as a ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Denebola
Denebola is the second-brightest star in the zodiac constellation of Leo.The two components of the γ Leonis double star, which are unresolved to the naked eye, have a combined magnitude brighter than it. It has the Bayer designation Beta Leonis or β Leonis, which are abbreviated Beta Leo or β Leo. Denebola is an A-type main sequence star with 75% more mass than the Sun and 15 times the Sun's luminosity. Based on parallax measurements from the Hipparcos astrometry satellite, the star is at a distance of from the Sun. Its apparent visual magnitude is 2.14, making it readily visible to the naked eye. Denebola is a Delta Scuti type variable star, meaning its luminosity varies very slightly over a period of a few hours. Nomenclature ''β Leonis'' ( Latinised to ''Beta Leonis'') is the star's Bayer designation. In Johann Bayer's ''Uranometria'' (1603), it was designated β (Beta) as the second-brightest star in the constellation. It also bears the Flamsteed desig ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Moving Group
In astronomy, stellar kinematics is the observational study or measurement of the kinematics or motions of stars through space. Stellar kinematics encompasses the measurement of stellar velocities in the Milky Way and its satellites as well as the internal kinematics of more distant galaxies. Measurement of the kinematics of stars in different subcomponents of the Milky Way including the thin disk, the thick disk, the bulge, and the stellar halo provides important information about the formation and evolutionary history of our Galaxy. Kinematic measurements can also identify exotic phenomena such as hypervelocity stars escaping from the Milky Way, which are interpreted as the result of gravitational encounters of binary stars with the supermassive black hole at the Galactic Center. Stellar kinematics is related to but distinct from the subject of stellar dynamics, which involves the theoretical study or modeling of the motions of stars under the influence of gravity. Stel ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Argus Association
IC 2391 (also known as the Omicron Velorum Cluster or Caldwell 85) is an open cluster in the constellation Vela. The Persian astronomer Al Sufi may have first described it about 964. It was found by Abbe Lacaille and cataloged as Lac II 5. The cluster is about 500 light-years away from Earth and can be seen with the naked eye. It contains about 30 stars with a total visual magnitude of 2.5, spread out along 50 arcminutes. It includes the following naked-eye members: * ο Velorum * HD 74560 (HY Velorum) * HD 74146 (NZ Velorum) * HD 74071 (HW Velorum) * HD 74196 * HD 74535 (KT Velorum) * HD 75466 * HD 73952 IC 2391 appears to be about the same age as the open cluster IC 2602, and has a lithium depletion boundary age of about 50 million years. IC 2391 has been closely linked to the Argus Association of co-moving stars. Proposed members of this moving group include Denebola, Epsilon Pavonis, 49 Ceti, HD 61005, and HD 88955. IC 2391 also includes HD 74438, the younge ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Lithium Depletion Boundary
The lithium depletion boundary (LDB) technique is a method proposed for dating open clusters based on a determination of the lithium Lithium (from el, λίθος, lithos, lit=stone) is a chemical element with the symbol Li and atomic number 3. It is a soft, silvery-white alkali metal. Under standard conditions, it is the least dense metal and the least dense solid ... abundances of a cluster's stars whose masses are at about the hydrogen burning mass limit.Darling, David. 2004. ''The Universal Book of Astronomy''. References Open clusters {{astronomy-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
IC 2602
IC 2602 (also known as the Southern Pleiades, Theta Carinae Cluster, or Caldwell 102) is an open cluster in the constellation Carina. Discovered by Abbe Lacaille in 1751 from South Africa, the cluster is easily visible to the unaided eye, and is one of the nearest star clusters, centred about 149 parsecs (486 light-years) away from Earth. Description IC 2602 has a total apparent magnitude of 1.9, and contains about 75 stars. It is the third-brightest open cluster in the sky, following the Hyades and the Pleiades. Its apparent diameter is about 50 arcminutes. IC 2602 is likely about the same age as the open cluster IC 2391,, which has a lithium depletion boundary age of 50 million years old, though the age estimated from its Hertzsprung-Russell diagram is about 13.7 million years. IC 2602 is thought to form part of the Lower Scorpius–Centaurus association. Components Theta Carinae is the brightest star within the open cluster, with the apparent visual magnitude of +2.74. Th ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
.jpg "Click for more on -> IC 2602")