psi orionis
found out that it is a double star, but I did not split it tonight. Seeing: 7, darkness:
During the eclipse of the primary component, the visual magnitude is reduced by 0.06, whereas the secondary eclipse reduces the magnitude by 0.03. [6] The close orbit is causing their mutual gravitational interaction to distort the shapes of the stars, turning this system into an ellipsoidal variable. Location of site:
It lies among a dense cluster of low-mass pre-main-sequence stars in the Orion OB1a. It also rotates rapidly (141 km/sec
Psi1 Orionis (25 Orionis) é uma estrela na direção da constelação de Orion. mag 4
magnitude>
Seeing Scale (10 best)>
Star: Psi Orionis Date & Time: 12/02/99, 9:30UT to 14:00 UT Seeing: 9 Location: Staveley, ~80km SW of Christchurch, New Zealand. Magnification: 48x,
[11], Like the star Pleione in the Pleiades open cluster, 25 Ori is a Be star with a gaseous circumstellar disk. 27 Ori was the brighter
The pair may be 1,420 light
Orion OB1 Association. Psi Orionis är en Bayer-beteckning som delas av två stjärnor i stjärnbilden Orion : 25 Orionis, en Be-stjärna av magnitud 4,87. Sua magnitude aparente é igual a 4.89. December 5, 1999, 10:00 to 10:30 pm CST
It has an apparent visual magnitude of 4.60,[2] indicating that it is visible to the naked eye. Sky darkness: 4
Seeing: 8 <1-10
Killeen, TX, USA (suburban)
The SIMBAD astronomical database lists its spectral class as B1Vn. Telescope: Orion
72x, 120x, 240x, Star: Psi 2 Orionis
Easily split at high
When looking for eta Ori
PSI ORI (Psi Orionis = Psi-2 Orionis). It is a Beta CMa variable. Possui uma ascensão reta de 05h 24m 44.83s e uma declinação de +01° 50′ 47.2″.
Magnification: 48x,
Telescope: Orion
[10], The combined spectrum of Psi2 Orionis matches that of a B-type subgiant star with a stellar classification of B2 IV. 10:37 pm CST using a micrometer reticle:
Star: Psi Orion
Seeing Scale (10 best)>
Esta é uma página de desambiguação que lista os artigos que podem ser associados a um ou vários títulos. [3], 25 Orionis is a fast rotator, clocking a rotational velocity of 316 km/s, significantly faster than Achernar's speed of 251 km/s in the constellation Eridanus. magnitude>
Psi Orionis Origem: Wikipédia, a enciclopédia livre. these were unrelated. Site classification:
[10] It is one of several sub-associations within Orion OB1a, all thought to lie at around the same distance of 338 parsecs. The Bayer designation Psi Orionis (ψ Ori / ψ Orionis) is shared by two stars in the constellation Orion : 25 Orionis (ψ 1), a Be star 30 Orionis (ψ 2, often just called ψ Orionis), an ellipsoidal and eclipsing variable This article includes a list of related items that share the …
Seeing: 7 <1-10
120x, Update from : 12/25/98
Se uma ligação interna o conduziu até aqui, sugerimos que a corrija para apontá-la diretamente ao artigo adequado. PA measured at 357 degrees,
I later determined that
25 Orionis, less commonly known by its Bayer designation Psi1 Orionis (ψ1 Orionis, ψ1 Ori) is a fifth-magnitude star in the constellation Orion.
at the equator). Psi2 Orionis a binary star system in the equatorial constellation of Orion. 6" Dob
of the two, yellow in color. 25 Orionis, less commonly known by its Bayer designation Psi1 Orionis is a fifth-magnitude star in the constellation Orion. Based upon an annual parallax shift of 2.87 mass, it is roughly 1,100 light years distant from the Sun. The AaxB period is on the
Considerando sua distância de 1109 anos-luz em relação à Terra, sua … Location of site:
November, 23th, 1998 - 10:30 pm CST
PA measured at 357 degrees, separation at 103.14". [8][12] Having a radius of 6 R☉, the star rotates on its axis roughly once every 23 hours. This is a double-lined spectroscopic binary,[4] which means that the individual absorption lines of both components can be discerned.
Based upon an annual parallax shift of 2.87 mass, it is roughly 1,100 light years distant from the Sun. [3] The primary component is an evolved giant star with a class of B1 III, while the secondary is a B-type main sequence star with a classification of B2 V.[4], Monthly Notices of the Royal Astronomical Society, Centre de données astronomiques de Strasbourg, https://en.wikipedia.org/w/index.php?title=Psi2_Orionis&oldid=968453652, Creative Commons Attribution-ShareAlike License, This page was last edited on 19 July 2020, at 14:04. 6" Dob. The pair orbit each other with a period of 2.526 days and a low eccentricity of 0.04. Great Orion is filled with hot blue stars, many of which are vaguely related through birth within various subgroups of the vast Orion OB1 association. Star A is a spectroscopic
Killeen, TX (Lat 31 N, Elev 600 ft)
[9] The inclination of orbital plane is sufficiently low that the two stars form a grazing eclipsing binary. Telescope: Orion
I saw what appeared to be a pair in the finder. It has an apparent visual magnitude of 4.60, indicating that it is visible to the naked eye. 25 Orionis is the dominant member of a rich low-mass star region,[9] first identified in 2005 in a statistical analysis of 2.5 million star. Killeen, TX (Lat 31 N, Elev 600 ft)
separation at 103.14". power. Its Flamsteed designation provides it with the name 28 Orionis, Sissy Haas’s Double Stars for Small Telescopes refers to it as Psi-2, the Sky and Telescope Pocket Atlas designates it as just plain Psi, and the Cambridge Double Star Atlas calls it by two names, Psi and Knott 3 (G. Knott recorded some double star discoveries and observations in the 1860’s, but that’s about all the information I can find on … SAO 132060 was the fainter member; I later
With a mass in excess of 10 M☉, the star is expected to explode as a supernova. binary with a 2.5260 day period. Hopped here from 23 Ori. Over 200 members of the 25 Orionis stellar group have been found, mostly T Tauri stars with spectral types of K and M and masses less than half the sun's. Site classification:
There are also around 60 hotter stars in the region, including the eruptive variable V346 Tauri. Suburban
Instrument: 102mm f/9.8 refractor Sky darkness: 6 - 6.5
The primary was white and the secondary was faint. It is part of the
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