13 Canis Majoris
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13 Canis Majoris
Kappa Canis Majoris, Latinized from κ Canis Majoris, is a solitary, blue-white hued star in the constellation Canis Major. It is visible to the naked eye with an apparent visual magnitude of +3.87. Based upon an annual parallax shift of 7.70  mas as seen from Earth, this star is located about 660 light years from the Sun. This is a B-type main-sequence star with a stellar classification of B1.5 Ve, although Hiltner et al. (1969) classified it as B1.5 IVe suggesting it is a subgiant star. The 'e' suffix indicates it is a rapidly rotating Be star with a circumstellar decretion disk of heated gas. The radius of the emitting disk is about , or about 3.7 times the radius of the star. It is classified as a Gamma Cassiopeiae type variable star and its brightness varies from magnitude +3.4 to +3.97. The star became 50% brighter between 1963 and 1978, increasing from magnitude 3.96 or so to 3.52. Naming In Chinese, (), meaning ''Bow and Arrow The bow ...
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J2000
In astronomy, an epoch or reference epoch is a moment in time used as a reference point for some time-varying astronomical quantity. It is useful for the celestial coordinates or orbital elements of a celestial body, as they are subject to perturbations and vary with time. These time-varying astronomical quantities might include, for example, the mean longitude or mean anomaly of a body, the node of its orbit relative to a reference plane, the direction of the apogee or aphelion of its orbit, or the size of the major axis of its orbit. The main use of astronomical quantities specified in this way is to calculate other relevant parameters of motion, in order to predict future positions and velocities. The applied tools of the disciplines of celestial mechanics or its subfield orbital mechanics (for predicting orbital paths and positions for bodies in motion under the gravitational effects of other bodies) can be used to generate an ephemeris, a table of values giving ...
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Variable Star
A variable star is a star whose brightness as seen from Earth (its apparent magnitude) changes systematically 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 periodically; for example, because the star 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 exhibit at least some oscillation 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. A ...
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Eta Carinae
η Carinae (Eta Carinae, abbreviated to η Car), formerly known as η Argus, is a stellar system containing at least two stars with a combined luminosity greater than five million times that of the Sun, located around distant in the constellation Carina. Previously a 4th-magnitude star, it brightened in 1837 to become brighter than Rigel, marking the start of its so-called "Great Eruption". It became the second-brightest star in the sky between 11–14 March 1843 before fading well below naked-eye visibility after 1856. In a smaller eruption, it reached 6th magnitude in 1892 before fading again. It has brightened consistently since about 1940, becoming brighter than magnitude 4.5 by 2014. At declination −59° 41′ 04.26″, η Carinae is circumpolar from locations on Earth south of latitude 30°S (for reference, the latitude of Johannesburg is 26°12′S), and is not visible north of about latitude 30°N, just south of Cairo (w ...
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Omega Velorum
Omega (, ; uppercase Ω, lowercase ω; Ancient Greek ὦ, later ὦ μέγα, Modern Greek ωμέγα) is the twenty-fourth and last letter in the Greek alphabet. In the Greek numeric system/isopsephy (gematria), it has a value of 800. The word literally means "great O" (''o mega'', mega meaning "great"), as opposed to omicron, which means "little O" (''o mikron'', mikron meaning "little"). In phonetic terms, the Ancient Greek Ω represented a long open-mid back rounded vowel , comparable to the "aw" of the English word ''raw'' in dialects without the cot–caught merger, in contrast to omicron, which represented the close-mid back rounded vowel , and the digraph ''ου'', which represented the long close-mid back rounded vowel . In Modern Greek, both omega and omicron represent the mid back rounded vowel or . The letter omega is transliterated into a Latin-script alphabet as ''ō'' or simply ''o''. As the final letter in the Greek alphabet, omega is often used to ...
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Delta Velorum
Delta Velorum (δ Velorum, abbreviated Delta Vel, δ Vel) is a triple star system in the southern constellation of Vela, near the border with Carina, and is part of the False Cross. Based on parallax measurements, it is approximately from the Sun. It is one of the stars that at times lies near the south celestial pole due to precession. δ Velorum consists of an eclipsing binary, designated Delta Velorum A, and a more distant third companion, Delta Velorum B. δ Velorum A's two components are themselves designated Aa (officially named Alsephina , the traditional name for the entire system) and Ab. Nomenclature ''δ Velorum'' ( Latinised to ''Delta Velorum'') is the system's Bayer designation. The designations of the two constituents as ''Delta Velorum A'' and ''B'', and those of ''A'' components—''Delta Velorum Aa'' and ''Ab''—derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the Internati ...
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Pi Puppis
Pi Puppis, Latinisation of names, Latinized from π Puppis, also named Ahadi, is the List of stars in Puppis, second-brightest star in the southern constellation of Puppis. It has an apparent visual magnitude of about 2.7, so it can be viewed with the naked eye at night. Parallax measurements yield an estimated distance of roughly from the Earth. This is a double star with a magnitude 6.86 companion at an angular separation of 0.72 Minute and second of arc#Symbols and abbreviations, arcsecond and a position angle of 148° from the brighter primary. The stellar spectrum, spectrum of Pi Puppis matches a stellar classification of K3 Ib. The Ib luminosity class indicates this a lower luminosity supergiant star that has consumed the hydrogen fuel at its core, stellar evolution, evolved away from the main sequence, and expanded to about 235 times the solar radius, Sun's radius. The effective temperature of the star's outer envelope is approximately , which ...
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Epsilon Canis Majoris
Epsilon Canis Majoris is a binary star system and the second-brightest star in the constellation of Canis Major. Its name is a Bayer designation that is Latinised from ε Canis Majoris, and abbreviated Epsilon CMa or ε CMa. This is the 22nd- brightest star in the night sky with an apparent magnitude of 1.50. About 4.7 million years ago, it was the brightest star in the night sky, with an apparent magnitude of −3.99. Based upon parallax measurements obtained during the Hipparcos and the Gaia mission, it is about light-years distant. The two components are designated ε Canis Majoris A, officially named Adhara – the traditional name of the system, and B. Nomenclature ''ε Canis Majoris'' (Latinised to ''Epsilon Canis Majoris'') is the binary system's Bayer designation. The designations of the two components as ''ε Canis Majoris A'' and ''B'' derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by th ...
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K Puppis
k Puppis (k Pup, k Puppis) is a Bayer designation given to an optical double star in the constellation Puppis, the two components being k1 Puppis and k2 Puppis. Bayer designation Note that the Bayer designation for this star is "k" not "kappa" (κ). In Bayer's original Uranometria, k Puppis was listed as ρ (rho) Navis. When Lacaille broke apart the large constellation Argo Navis into Carina, Puppis, and Vela, he re-designated the stars with Greek letters in a single sequence across all three constellations. Additionally, Lacaille used Latin letters for many additional stars. κ (kappa) is in the constellation of Vela and so there is no kappa in Puppis. The confusion also extends to the proper name Markab which properly applies to κ Velorum (and other stars) but which has also been used for k Puppis when it is called κ Puppis. Description Both k1 Puppis and k2 Puppis are bright blue B-type stars of nearly equal brightness, +4.50 and +4.62, respectively. To th ...
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Omicron Puppis
Omicron Puppis (ο Puppis) is candidate binary star system in the southern constellation of Puppis. It is visible to the naked eye, having a combined apparent visual magnitude of +4.48. Based upon an annual parallax shift of 2.30  mas as seen from Earth, it is located roughly 1,400 light years from the Sun. This is a suspected close spectroscopic binary system. The spectrum varies with a periodicity of 28.9 days, and a helium emission component shows a radial velocity variation that matches the period. The properties indicate it may be a φ Per-like system with a Be star primary and a hot subdwarf companion of type sdO. If this is the case, then the pair have a circular orbit with a period that matches the variability. The close-orbiting pair may have undergone interaction in the past, leaving the subdwarf stripped down and the primary star spinning rapidly. ο Puppis is slightly variable. The General Catalogue of Variable Stars lists it as a possible B ...
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HD 65456
χ Puppis, Latinised as Chi Puppis, is a single star in the southern constellation of Puppis. It has a white hue and is faintly visible to the eye at night with an apparent visual magnitude of 4.79. The star is located at a distance of approximately 1,800 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +30 km/s. O. J. Eggen listed this star as a member of the Hyades Stream based on its space motion. There has been some disagreement as to the stellar classification of Chi Puppis. In 1962, W. Buscombe classified it as A2Vvar, matching a variable A-type main-sequence star. However, P. S. Conti in 1965 considered that to be a misclassification on the basis of its B-V color index. He considers it of later type A5. In their study of the nearby open cluster NGC 2483, M. P. Fitzgerald and A. F. J. Moffat used the same class, A2Vv. In 1979, Nancy Houk assigned it to class A7 III, indicating it may be an A-type g ...
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HD 63032
c Puppis, also known as HD 63032 and HR 3017, is a spectroscopic binary star in the constellation Puppis. Its apparent magnitude is of 3.61, making it the eight-brightest star in Puppis. The system is the brightest member of the open cluster NGC 2451, over two magnitudes brighter than every other star in the cluster. As the turnoff point of the cluster is currently around B7, the parameters of the system fit with cluster membership. The primary component of the system is a red supergiant or bright giant of spectral classification K2.5Ib-IIa. It is twelve times more massive than the Sun, and is estimated 16 million years old. At this evolutionary stage, it has expanded to 280 times the size of the Sun and is 15,000 more luminous. Its surface has cooled to an effective temperature of 3,781  K, giving it a red-orange hue. The secondary component is a late B-type star In astronomy, stellar classification is the classification of stars based on their spectral chara ...
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Eta Canis Majoris
Eta Canis Majoris (η Canis Majoris, abbreviated Eta CMa, η CMa), also named Aludra , is a blue supergiant star in the constellation of Canis Major. It has an apparent magnitude varying between 2.38 and 2.48, which makes it the fifth-brightest in the constellation and brightest stars. Parallax measurements from the Hipparcos mission give a large distance of 2,000 light-years. Nomenclature ''η Canis Majoris'' ( Latinised to ''Eta Canis Majoris'') is the star's Bayer designation. The traditional name ''Aludra'' originates from the Arabic: ''العذراء'' ''al-adhraa'', 'the virgin'. This star, along with Epsilon Canis Majoris (Adhara), Delta Canis Majoris (Wezen) and Omicron2 Canis Majoris (Thanih al Adzari), were ''Al 'Adhārā'' (''العذاري''), 'the Virgins'. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016 included a table ...
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