|
List Of Stars In Musca
This is the list of notable stars in the constellation A constellation is an area on the celestial sphere in which a group of visible stars forms Asterism (astronomy), a perceived pattern or outline, typically representing an animal, mythological subject, or inanimate object. The origins of the e ... Musca, sorted by decreasing brightness. See also * List of stars by constellation Notes References * * * * * {{Musca *List Musca ... [...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] |
Scorpius–Centaurus Association
The Scorpius–Centaurus association (sometimes called Sco–Cen or Sco OB2) is the nearest OB association to the Sun. This stellar association is composed of three subgroups (Upper Scorpius, Upper Centaurus–Lupus, and Lower Centaurus–Crux) and its distance is about 130 parsecs or 420 light-years. Using improved Hipparcos data, Rizzuto and colleagues analysed nearby stars more closely, bringing the number of known members to 436. They doubt the need to add a subclassification because they found a more continuous spread of stars. The Sco–Cen subgroups range in age from 11 million years (Upper Scorpius) to roughly 15 million years (Upper Centaurus–Lupus and Lower Centaurus–Crux). Many of the bright stars in the constellations Scorpius, Lupus, Centaurus, and Crux are members of the Sco–Cen association, including Antares (the most massive member of Upper Scorpius), and most of the stars in the Southern Cross. Hundreds of stars have been identified as members of Sco-Cen, ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 115211
HD 115211 is a single star in the southern constellation of Musca. It has an orange hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.86. Its distance from Earth is approximately 1,370 light years based on parallax, and it is drifting closer to the Sun with a radial velocity of −10 km/s. It has an absolute magnitude of −2.94. It is an aging bright giant/ supergiant star with a stellar classification of K2 Ib-II. It is a suspected variable star of unknown type, with a brightness that has been measured ranging from 4.83 down to 4.87. It is an estimated 40 million years old, with 7.1 times the mass of the Sun. With the supply of hydrogen exhausted at its core, it has expanded to 123 times the Sun's radius. It is radiating 3,849 times the luminosity of the Sun from its swollen photosphere at an effective temperature The effective temperature of a body such as a star or planet is the temperature of a black body t ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Algol Variable
Algol variables or Algol-type binaries are a class of eclipsing binary stars that are similar to the prototype member of this class, β Persei (Beta Persei, Algol). An Algol binary is a system where both stars are near-spherical such that the timing of the start and end of the eclipses is well-defined. The primary is generally a main sequence star well within its Roche lobe. The secondary may also be a main sequence star, referred to as a detached binary or it may an evolved star filling its Roche lobe, referred to as a semidetached binary. When the cooler component passes in front of the hotter one, part of the latter's light is blocked, and the total brightness of the binary, as viewed from Earth, temporarily decreases. This is the primary minimum of the binary. Total brightness may also decrease, but less so, when the hotter component passes in front of the cooler one; this is the secondary minimum. The period, or time span between two primary minima, is very regular ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Eta Muscae
Eta Muscae is a multiple star system in the southern constellation of Musca. It is visible to the naked eye as a faint, blue-white hued point of light with an apparent visual magnitude of 4.79. The system is located around 406 light years away from the Sun. It is a member of the Lower Centaurs Crux subgroup of the Sco OB2 stellar association of co-moving stars. The two main components of this system form a double-lined spectroscopic binary with a period of 2.4 days in a circular orbit. They are a detached eclipsing binary with a spectral type of B8V and a brightness that dips by 0.05 magnitude once per orbit. This pair consists of two components of similar mass and type. Further away from the primary system are stars of magnitude 7.3 and 10, designated Eta Muscae B and C. It is unclear if these stars are gravitationally–bound to the main pair. Evidence for an additional component has been found with a 30-year cycle in the orbital behavior of the main pair. T ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Slow Irregular Variable
A slow irregular variable (ascribed the GCVS types L, LB and LC) is a variable star that exhibit no or very poorly defined periodicity in their slowly changing light emissions. These stars have often been little-studied, and once more is learnt about them, they are reclassified into other categories such as semiregular variables. Nomenclature Irregular variable stars were first given acronyms based on the letter "I": ''Ia'', ''Ib''. and ''Ic''. These were later refined so that the I codes were used "nebular" or "rapidly irregular" variable stars such as T Tauri and Orion variables. The remaining irregular stars, cool slowly varying giants and supergiants of type Ib or Ic were reassigned to Lb and Lc. When the General Catalogue of Variable Stars standardised its acronyms to be all uppercase, the codes LB and LC were used. Type Lb ''Slow irregular variables of late spectral types ( K, M, C, S); as a rule, they are giants'' The GCVS also claims to give this type to slow irregular ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Mu Muscae
Mu Muscae, Latinized from μ Muscae, is a solitary star in the southern constellation of Musca. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of around 4.75. Based upon an annual parallax shift of 7.21 mas as seen from Earth, it is located about 450 light years from the Sun. The star is drifting further away with a radial velocity of +37 km/s. This is an evolved K-type giant star with a stellar classification of K4 III, having exhausted the supply of hydrogen at its core then cooled and expanded to 53 times the Sun's radius. It most likely on the red giant branch, rather than the asymptotic giant branch, and shows no signs of mass loss. Mu Muscae is a type Lb, oxygen-rich irregular variable with a small amplitude that ranges in visual magnitude between 4.71 and 4.76. It is radiating 602 times the luminosity of the Sun from its photosphere at an effective temperature The effective temperature of a ... [...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 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Epsilon Muscae
Epsilon Muscae, Latinized as ε Muscae, is a red giant star of spectral type M5III in the constellation Musca. Originally a main-sequence star of around 1.5 to 2 solar masses, it is now on the asymptotic giant branch and has now expanded to 130 times the Sun's diameter and 1800 to 2300 its luminosity. It is a semiregular variable, varying in eight distinct periods ranging from a month to over half a year in length, with the largest amplitude being of almost half a magnitude from the mean of 4.06. It is located around 300 light-years distant, the same distance as the Lower Centaurus–Crux subgroup of the Scorpius–Centaurus association The Scorpius–Centaurus association (sometimes called Sco–Cen or Sco OB2) is the nearest OB association to the Sun. This stellar association is composed of three subgroups (Upper Scorpius, Upper Centaurus–Lupus, and Lower Centaurus–Crux) ..., although it is moving much faster at around 100 km/s and does not share a common o ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
53 Persei Variable
A slowly pulsating B-type star (SPB), formerly known as a 53 Persei variable, is a type of pulsating variable star. They may also be termed a long-period pulsating B star (LPB). As the name implies, they are main-sequence stars of spectral type B2 to B9 (3 to 9 times as massive as the Sun) that pulsate with periods between approximately half a day and five days, however within this most member stars have been found to have multiple periods of oscillations. They display variability both in their light emission and in their spectral line profile. The variations in magnitude are generally smaller than 0.1 magnitudes, making it quite hard to observe variability with the naked eye in most cases. The variability increases with decreasing wavelength, thus they are more obviously variable in ultraviolet spectrum than visible light. Their pulsations are non-radial, that is, they vary in shape rather than volume; different parts of the star are expanding and contracting simultaneously. The ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Gamma Muscae
γ Muscae, Latinised as Gamma Muscae, is a blue-white hued star in the southern circumpolar constellation of Musca, the Fly. It can be seen with the naked eye, having an apparent visual magnitude of 3.87. Based upon an annual parallax shift of 10.04 mas as seen from Earth, it is located about 325 light years from the Sun. This is a B-type main-sequence star with a stellar classification of B5 V. It is a variable star that ranges between magnitudes 3.84 and 3.86 over a period of 2.7 days, and is classed as a slowly pulsating B star. It is around five times as massive as the Sun. The star is spinning rapidly with a projected rotational velocity of 205 km/s. This is giving it an oblate shape with an equatorial bulge that is 7% larger than the polar radius. Gamma Muscae is a proper motion member of the Lower Centaurus–Crux sub-group in the Scorpius–Centaurus OB association In astronomy, stellar kinematics is the observational study or measuremen ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Lambda Muscae
Lambda Muscae, Romanization of Greek, Latinized from λ Muscae, and often catalogued HD 102249 or HIP 57363, is the fourth-brightest star in the Southern Hemisphere constellation of Musca (the Fly). Lambda Muscae visibly makes up the far end of the tail of the visual Musca constellation. It is a star in a dual system according to studies, and one of the stars catalogued in astronomer Johann Bayer's 1603 publications ''Uranometria''. Lambda Muscae more recently has been recorded as having a stellar classification of A7III. Thus, Lambda Muscae has a white tint and burns significantly hotter than the Sun. Distance and visibility Based on research done by the European Space Agency for the Hipparcos catalogue, Hipparcos Star Catalogue, Lambda Muscae exhibits a parallax of 25.42 Minute and second of arc#Astronomy, milliarcseconds. With this data it can be calculated that Lambda Muscae is situated at a distance of 39.3 parsecs, or 128.0 light years, away from the sun. Lambd ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
