Search results
Results From The WOW.Com Content Network
An eclipsing binary star is a binary star system in which the orbital plane of the two stars lies so nearly in the line of sight of the observer that the components undergo mutual eclipses. [20] In the case where the binary is also a spectroscopic binary and the parallax of the system is known, the binary is quite valuable for stellar analysis.
The closest encounter to the Sun so far predicted is the low-mass orange dwarf star Gliese 710 / HIP 89825 with roughly 60% the mass of the Sun. [4] It is currently predicted to pass 0.1696 ± 0.0065 ly (10 635 ± 500 au) from the Sun in 1.290 ± 0.04 million years from the present, close enough to significantly disturb the Solar System's Oort ...
This image indicates the location of the newly discovered binary star D9, which is orbiting Sagittarius A*, the supermassive black hole at the centre of our galaxy. It is the first star pair ever ...
A binary consisting of a yellow supergiant or yellow hypergiant and a Blue supergiant. MACS J1149 Lensed Star 1: 1.49 [7] 4,410 2018 The most distant known star prior to the discovery of Earendel. Warhol 0.94 [8] 3,000 2014 Transient, extremely luminous O-type star or a Large Wolf-Rayet star [9] AT 2022zmn: 0.019 [10] 84 2022 Luminous blue ...
Below there are lists the nearest stars separated by spectral type.The scope of the list is still restricted to the main sequence spectral types: M, K, F, G, A, B and O.It may be later expanded to other types, such as S, D or C.
The primary component is a B-type star with a stellar classification of B2 III. [3] The stellar spectrum of π 4 Ori A shows a strong depletion of the element boron. [12] It has nearly 11 [6] times the mass of the Sun and nine times the Sun's radius. [7] The star is 15.4 [10] million years old and has a projected rotational velocity of 38 km/s. [9]
Gamma Cephei (γ Cephei, abbreviated Gamma Cep, γ Cep) is a binary star system approximately 45 light-years away in the northern constellation of Cepheus.The primary (designated Gamma Cephei A, officially named Errai / ɛ ˈ r eɪ. iː /, the traditional name of the system) [11] [12] is a stellar class K1 orange giant or subgiant star; it has a red dwarf companion (Gamma Cephei B).
Gamma Virginis is a binary star, consisting of two stars of nearly equal apparent magnitudes 3.65 and 3.56, and of spectral type F0V. [2] With an orbital period of 168.93 years, [5] [6] it was an easy object for amateur astronomers until the beginning of the 1990s, but in 2011 the smaller apparent distance between the stars requires a larger telescope or special techniques such as speckle ...