|
Pi Arietis
Pi Arietis, Latinized from π Arietis, is the Bayer designation for a multiple star system in the northern constellation of Aries. Based upon parallax measurements made during the Hipparcos mission, this system is approximately distant from Earth and has an apparent visual magnitude of 5.21. This is bright enough to be faintly seen with the naked eye. The primary member of this system is a massive, B-type main sequence star with a stellar classification of B6 V. It is a close spectroscopic binary with an orbital period of 3.854 days, an eccentricity of 0.04, and a combined visual magnitude of 5.30. At an angular separation of 3.28 arcseconds is a magnitude 8.46 A-type main sequence star with a classification of A0 Vp. Finally, a fourth member of the system is a magnitude 11.0 F-type main sequence star with a classification of F8V at an angular separation of 25.2 arcseconds from the primary. Name This star, along with δ Ari, ε Ari, ζ Ar ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Aries (constellation)
Aries is one of the constellations of the zodiac. It is located in the Northern celestial hemisphere between Pisces to the west and Taurus to the east. The name Aries is Latin for ram. Its old astronomical symbol is (♈︎). It is one of the 48 constellations described by the 2nd century astronomer Ptolemy, and remains one of the 88 modern constellations. It is a mid-sized constellation ranking 39th in overall size, with an area of 441 square degrees (1.1% of the celestial sphere). Aries has represented a ram since late Babylonian times. Before that, the stars of Aries formed a farmhand. Different cultures have incorporated the stars of Aries into different constellations including twin inspectors in China and a porpoise in the Marshall Islands. Aries is a relatively dim constellation, possessing only four bright stars: Hamal (Alpha Arietis, second magnitude), Sheratan (Beta Arietis, third magnitude), Mesarthim (Gamma Arietis, fourth magnitude), and 41 Arietis (als ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Orbital Period
The orbital period (also revolution period) is the amount of time a given astronomical object takes to complete one orbit around another object. In astronomy, it usually applies to planets or asteroids orbiting the Sun, moons orbiting planets, exoplanets orbiting other stars, or binary stars. For celestial objects in general, the sidereal period ( sidereal year) is referred to by the orbital period, determined by a 360° revolution of one body around its primary, e.g. Earth around the Sun, relative to the fixed stars projected in the sky. Orbital periods can be defined in several ways. The tropical period is more particularly about the position of the parent star. It is the basis for the solar year, and respectively the calendar year. The synodic period incorporates not only the orbital relation to the parent star, but also to other celestial objects, making it not a mere different approach to the orbit of an object around its parent, but a period of orbital relations wit ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Mu Arietis
Mu Arietis, Latinized from μ Arietis, is the Bayer designation for a star system in the northern constellation of Aries. It is approximately distant from Earth, give or take a 30 light-year margin of error, and has a combined apparent visual magnitude of 5.74. According to the Bortle Dark-Sky Scale, this means it is faintly visible to the naked eye from dark suburban skies. At the heart of this system is a close orbiting pair consisting of a magnitude 6.38 A-type main sequence star with a stellar classification of A0 Vp and a magnitude 8.38 F-type main sequence companion with a classification of F2 V. These two components have an angular separation of 0.04 arcsecond A minute of arc, arcminute (arcmin), arc minute, or minute arc, denoted by the symbol , is a unit of angular measurement equal to of one degree. Since one degree is of a turn (or complete rotation), one minute of arc is of a turn. The na ...s. A third component, consisting ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Nu Arietis
Nu Arietis, Latinized from ν Arietis, is the Bayer designation for a white-hued star in the northern constellation of Aries. It is faintly visible to the naked eye with an apparent visual magnitude of +5.43. Based upon an annual parallax shift of 9.68 mas as seen from Earth, it is located roughly 340 light years from the Sun. It is moving away from the Sun with a radial velocity of 8 km/s. This is an A-type main sequence star with a stellar classification of A7 V. Nu Arietis has an estimated 2.4 times the mass of the Sun and about 1.8 times the Sun's radius. The star is radiating 63.5 times the Sun's luminosity from its photosphere at an effective temperature of around 8,000 K. It is roughly 621 million years old and is spinning with a projected rotational velocity Stellar rotation is the angular motion of a star about its axis. The rate of rotation can be measured from the spectrum of the star, or by timing the movements of active feat ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Bond (Chinese Constellation)
''Leu'' (or ''Low'') ''sieu'' () meaning "the Train of a garment", was one of the Twenty-eight mansions, twenty-eight lunar mansions of the traditional Chinese astronomy. It was one of the White Tiger (Chinese constellation), White Tiger of the West (西方白虎). The asterisms in the Region of ''Leu'' （婁宿天區） Notes See also * Traditional Chinese star names References * * 大崎正次 (1987). 『中国の星座の歴史』 雄山閣出版. External links * 陳冠中, 陳輝�「中國古代的星象系統 (71)： 婁宿天區」 - 天文教育資訊網 (AEEA) {{Chinese constellation Chinese constellations ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Chinese Astronomy
Astronomy in China has a long history stretching from the Shang dynasty, being refined over a period of more than 3,000 years. The ancient Chinese people have identified stars from 1300 BCE, as Chinese star names later categorized in the twenty-eight mansions have been found on oracle bones unearthed at Anyang, dating back to the mid-Shang dynasty. The core of the "mansion" (宿 ''xiù'') system also took shape around this period, by the time of King Wu Ding (1250–1192 BCE). Detailed records of astronomical observations began during the Warring States period (fourth century BCE) and flourished from the Han period onward. Chinese astronomy was equatorial, centered on close observation of circumpolar stars, and was based on different principles from those in traditional Western astronomy, where heliacal risings and settings of zodiac constellations formed the basic ecliptic framework. Joseph Needham has described the ancient Chinese as the most persistent and accurat ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Rho3 Arietis
Rho3 Arietis (Rho3 Ari, ρ3 Arietis, ρ3 Ari) is the Bayer designation for a star in the northern constellation of Aries. It is faintly visible to the naked eye with an apparent visual magnitude of 5.63. Based upon an annual parallax shift of 28.29 mas, this star is located at a distance of approximately from Earth. This is an astrometric binary system. The visible component is an F-type main sequence star with a stellar classification of F6 V. It is around 2.4 billion years old and has a high abundance of elements other than hydrogen and helium when compared to the Sun. Name This star, along with δ Ari, ε Ari, ζ Ari, and π Ari, were Al Bīrūnī's ''Al Buṭain'' (ألبطين), the dual of ''Al Baṭn'', the Belly. According to the catalogue of stars in the ''Technical Memorandum 33-507 - A Reduced Star Catalog Containing 537 Named Stars'', ''Al Buṭain'' were the title for five stars : δ Ari as ''Botein'', π Ari as ''Al ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Zeta Arietis
Zeta Arietis, Latinized from ζ Arietis, is the Bayer designation for a star in the northern constellation of Aries. It is dimly visible to the naked eye with an apparent visual magnitude of +4.89. Based upon an annual parallax shift of 12.77 mas, the distance to this star is . This is an A-type main sequence star with a stellar classification of A1 V. It has a high rate of rotation with a projected rotational velocity of 133 km/s. The star is shining at an effective temperature of 9,500 K, giving it the characteristic white-hued glow of an A-type star. Name This star, along with δ Ari, ε Ari, π Ari, and ρ3 Ari, were Al Bīrūnī's ''Al Buṭain'' (ألبطين), the dual of ''Al Baṭn'', the Belly. According to the catalogue of stars in the ''Technical Memorandum 33-507 - A Reduced Star Catalog Containing 537 Named Stars'', ''Al Buṭain'' were the title for five stars : δ Ari as ''Botein'', π Ari as ''Al Buṭain I'', ρ3 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Epsilon Arietis
Epsilon Arietis (ε Ari, ε Arietis) is the Bayer designation for a visual binary star system in the northern constellation of Aries. It has a combined apparent visual magnitude of 4.63 and can be seen with the naked eye, although the two components are too close together to be resolved without a telescope. With an annual parallax shift of 9.81 mas, the distance to this system can be estimated as , give or take a 30 light-year margin of error. It is located behind the dark cloud MBM12. The brighter member of this pair has an apparent magnitude of 5.2. At an angular separation of from the brighter component, along a position angle of , is the magnitude 5.5 companion. Both are A-type main sequence stars with a stellar classification of A2 Vs. (The 's' suffix indicates that the absorption lines in the spectrum are distinctly narrow.) In the 2009 ''Catalogue of Ap, HgMn and Am stars'', the two stars have a classification of A3 Ti, indicating they are Ap star ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Delta Arietis
Delta Arietis (δ Arietis, abbreviated Delta Ari, δ Ari), officially named Botein , is a star in the northern constellation of Aries, 1.8 degrees north of the ecliptic. The apparent visual magnitude is 4.35, so it is visible to the naked eye. It has an annual parallax shift of 19.22 mas; corresponding to a distance of about from the Sun. Nomenclature ''δ Arietis'' ( Latinised to ''Delta Arietis'') is the star's Bayer designation. It bore the traditional name ''Botein'' which is derived from Al Bīrūnī's ''Al Buṭayn'' (Arabic: البُطَين), the diminutive of ''Al Baṭn'', "the Belly". This is the name of a star association consisting of this star, Epsilon Arietis, Zeta Arietis, Pi Arietis, and Rho3 Arietis According to a 1971 NASA catalogue of stars, ''Al Buṭain'' was the title for five stars: Delta Arietis (listed as ''Botein''), Pi Arietis (as ''Al Buṭain I''), Rho3 Arietis (''Al Buṭain II''), Epsilon Arietis (''Al Buṭain III'') and Zeta ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
F-type Main Sequence Star
An F-type main-sequence star (F V) is a main-sequence, hydrogen-fusing star of spectral type F and luminosity class V. These stars have from 1.0 to 1.4 times the mass of the Sun and surface temperatures between 6,000 and 7,600 K.Tables VII and VIII. This temperature range gives the F-type stars a whitish hue when observed by the atmosphere. Because a main-sequence star is referred to as a dwarf star, this class of star may also be termed a yellow-white dwarf (not to be confused with white dwarfs, remnant stars that are a possible final stage of stellar evolution). Notable examples include Procyon A, Gamma Virginis A and B, and KIC 8462852. Spectral standard stars The revised Yerkes Atlas system (Johnson & Morgan 1953) listed a dense grid of F-type dwarf spectral standard stars; however, not all of these have survived to this day as stable standards. The ''anchor points'' of the MK spectral classification system among the F-type main-sequence dwarf stars, i.e. those st ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
A-type Main Sequence Star
An A-type main-sequence star (A V) or A dwarf star is a main-sequence (hydrogen-burning) star of spectral type A and luminosity class V (five). These stars have spectra defined by strong hydrogen Balmer absorption lines. They measure between 1.4 and 2.1 solar masses () and have surface temperatures between 7,600 and 10,000 K. Bright and nearby examples are Altair (A7 V), Sirius A (A1 V), and Vega (A0 V). A-type stars do not have convective zones and thus are not expected to harbor magnetic dynamos. As a consequence, because they do not have strong stellar winds, they lack a means to generate X-ray emissions. In July 2019, astronomers reported finding an A-type star, S5-HVS1, traveling , faster than any other star detected so far. The star is in the Grus (or Crane) constellation in the southern sky, about 29,000 light-years from Earth, and may have been ejected out of the Milky Way after interacting with Sagittarius A*, the supermassive black hole at the center ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
