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List Of Stars In Lepus ...
This is the list of notable stars in the constellation Lepus, sorted by decreasing brightness. References * * * * * * {{Stars of Lepus *List Lepus Hares and jackrabbits are mammals belonging to the genus ''Lepus''. They are herbivores, and live solitarily or in pairs. They nest in slight depressions called forms, and their young are able to fend for themselves shortly after birth. The gen ... [...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] |
Theta Leporis
Theta Leporis, Latinized from θ Leporis, is a solitary, white-hued star in the southern constellation of Lepus. It has an apparent visual magnitude of 4.67, making it bright enough to be viewed with the naked eye. Based upon an annual parallax shift of 18.88 mas as measured from Earth, the system is located roughly 173 light years from the Sun. The star made its closest approach about 1.6 million years ago when it came within of the Sun. This is an ordinary A-type main-sequence star with a stellar classification of A0 V and an age of about 207 million years. It is rotating rapidly with a projected rotational velocity of 207 km/s. This is giving the star an oblate shape with an equatorial bulge that is an estimated 10% larger than the polar radius. It has an estimated 2.35 times the mass of the Sun and is radiating 41 times the Sun's luminosity from its photosphere at an effective temperature The effective temperature of a body such as a sta ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Iota Leporis
Iota Leporis (ι Leporis) is a triple star system in the southern constellation of Lepus. It is visible to the naked eye as a point source of blue-white light with an apparent visual magnitude of 4.45. Based upon an annual parallax shift of 14.07 mas as measured from Earth, the system is located roughly 232 light years from the Sun. The primary, designated component A, is a B-type main-sequence star with a stellar classification of B7.5 Vn, where the 'n' suffix indicates "nebulous" absorption lines caused by rotation. It is about 94 million years old and has a high rate of spin with a projected rotational velocity of 185 km/s. With an estimated 3.4 times the mass of the Sun, it is radiating 153 times the Sun's luminosity from its photosphere at an effective temperature of around 13,781 K. There is a close companion that is a source of X-ray emission. Most likely this star has at least 1.05 times the mass of the Sun. The third component, AM Le ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Kappa Leporis
Kappa Leporis, Latinized from κ Leporis, is a binary star system in the southern constellation of Lepus. The pair have apparent visual magnitudes of 4.43 and 7.00, with the former being bright enough to be seen with the naked eye. As of 2000, they had an angular separation of 2.179 arc seconds along a position angle of 357.3°. Based upon an annual parallax shift of 4.48 mas as measured from Earth, the system is located roughly 730 light years from the Sun. The system is travelling away from the Sun with a radial velocity of +20.8 km/s. The brighter, blue-white hued member of the system, component A, is a B-type main-sequence star with a stellar classification of B9 V. It has nearly five times the mass of the Sun and around 2.6 times the Sun's radius. The star is radiating 1,346 times the Sun's luminosity from its photosphere at an effective temperature of 11,588 K. It displays an infrared excess at a wavelength of 12μm, making it a candid ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Lambda Leporis
Lambda Leporis, which is the Latinized form of λ Leporis, is a solitary, blue-white hued star in the southern constellation of Lepus. It is visible to the naked eye with an apparent visual magnitude of +4.29. Based upon an annual parallax shift of 3.83 mas, it is estimated to lie roughly 850 light years from the Sun. Relative to its neighbors, this star has a peculiar velocity of . It is a member of the Orion OB1 association (Ori OB1), and it has been identified as a high-velocity runaway star. This is a massive, B-type main-sequence star with a corrected stellar classification of B0.5 V. It is an estimated eight million years old and is spinning with a projected rotational velocity of 30 km/s. This star has around 15 times the mass of the Sun and 4.5 times the Sun's radius. It is radiating 15,488 times the Sun's luminosity from its photosphere at an effective temperature of 30,400 K. References } {{DEFAULTSORT:Lambda Leporis B-type subgi ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Delta Leporis
Delta Leporis (δ Leporis) is a solitary, orange-hued star in the southern constellation of Lepus. It is visible to the naked eye with an apparent visual magnitude of 3.85. Based upon an annual parallax shift of 28.68 mas, it is 114 light years distant from Earth. This is an old, evolved K-type star with an age of about 10.7 billion years. Keenan and McNeil (1989) classified it as , indicating it is a giant star showing a deficiency of iron and an excess of cyanogen in its atmosphere. However, Gray et al. (2006) listed it as , which would suggest a less evolved subgiant star. It may be a red clump star, which indicates it is generating energy through helium fusion at its core. The measured angular diameter of this star, after correction for limb darkening, is . At the estimated distance of this star, this yields a physical size of about 10 times the radius of the Sun. It has only 94% of the Sun's mass and is radiating 46 times the Sun's luminosity from its photo ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Eta Leporis
Eta Leporis, Latinised from η Leporis, is a single, yellow-white-hued star in the southern constellation of Lepus, the hare. It is visible to the naked eye with an apparent visual magnitude of approximately 3.72. The annual parallax shift of 67.21 mas yields a distance estimate of 49 light-years. It is moving closer to the Sun with a radial velocity of −1.6 km/s. This is an ordinary F-type main-sequence star with a stellar classification of F2 V. It is about 1.8 billion years old and spinning with a projected rotational velocity of 26 km/s. The star has 1.4 times the mass of the Sun and 1.5 times the Sun's radius. It shines with six times the Sun's luminosity, which is being radiated from its photosphere at an effective temperature of around . Using the IRS instrument on the Spitzer Space Telescope, excess infrared emission has been observed from the star, which can be modeled by a dust disk extending from 1 to 16 astronomical units fro ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Gamma Leporis
Gamma Leporis, Latinized from γ Leporis, is a star in the south central part of the constellation Lepus, southeast of Beta Leporis and southwest of Delta Leporis. With an apparent visual magnitude of 3.587, it is bright enough to be seen with the naked eye. Based upon an annual parallax shift of as seen from Earth, its distance can be estimated as 29 light years from the Sun. It has a common proper motion companion, AK Leporis, which is a variable star of the BY Draconis type and has an average brightness of magnitude 6.28. The two are apart can be well seen in binoculars. Gamma Leporis is a member of the Ursa Major Moving Group. Gamma Leporis is an F-type main-sequence star with a stellar classification of F6 V. It is larger than the Sun with 1.2 times the radius of the Sun and 1.3 times the Sun's mass. The star is around 1.3 billion years old and is spinning with a rotation period of about six days. Based upon its stellar characteristics and distance fro ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Asteroid Belt
The asteroid belt is a torus-shaped region in the Solar System, located roughly between the orbits of the planets Jupiter and Mars. It contains a great many solid, irregularly shaped bodies, of many sizes, but much smaller than planets, called asteroids or minor planets. This asteroid belt is also called the main asteroid belt or main belt to distinguish it from other asteroid populations in the Solar System such as near-Earth asteroids and trojan asteroids. The asteroid belt is the smallest and innermost known circumstellar disc in the Solar System. About 60% of its mass is contained in the four largest asteroids: Ceres, Vesta, Pallas, and Hygiea. The total mass of the asteroid belt is calculated to be 3% that of the Moon. Ceres, the only object in the asteroid belt large enough to be a dwarf planet, is about 950 km in diameter, whereas Vesta, Pallas, and Hygiea have mean diameters less than 600 km. The remaining bodies range down to the size of a dust particl ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Zeta Leporis
Zeta Leporis, Latinized from ζ Leporis, is a star approximately away in the southern constellation of Lepus. It has an apparent visual magnitude of 3.5, which is bright enough to be seen with the naked eye. In 2001, an asteroid belt was confirmed to orbit the star. Stellar components Zeta Leporis has a stellar classification of A2 IV-V(n), suggesting that it is in a transitional stage between an A-type main-sequence star and a subgiant. The (n) suffix indicates that the absorption lines in the star's spectrum appear nebulous because it is spinning rapidly, causing the lines to broaden because of the Doppler effect. The projected rotational velocity is 245 km/s, giving a lower limit on the star's actual equatorial azimuthal velocity. The star has about 1.46 times the mass of the Sun, along with 1.5 times the radius, and 14 times the luminosity. The abundance of elements other than hydrogen and helium, what astronomers term the star's metallicity, is only 1 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Alpha² Canum Venaticorum Variable
An Alpha2 Canum Venaticorum variable (or α2 CVn variable) is a type of variable star. These stars are chemically peculiar main sequence stars of spectral class B8p to A7p. They have strong magnetic fields and strong silicon, strontium, or chromium spectral lines. Their brightness typically varies by 0.01 to 0.1 magnitudes over the course of 0.5 to 160 days. In addition to their intensities, the intensities and profiles of the spectral lines of α2 CVn variables also vary, as do their magnetic fields. The periods of these variations are all equal and are believed to equal the period of rotation of the star. It is thought that they are caused by an inhomogeneous distribution of metals in the atmospheres of these stars, so that the surface of the star varies in brightness from point to point. The type-star which this class is named after is α² Canum Venaticorum, a star in the binary system of Cor Caroli, which is in the northern constellation of Canes Venatici Canes Ven ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
