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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 ...
0.072 [21] −1.6 [21] 17.7 [21] [NB 1] Local Group: Satellite of Milky Way 25 Eridanus IV: 0.250 0.0767 [22] −4.7 [22] 14.72 [22] [NB 1] Local Group: Satellite of Milky Way [22] 489 ly [22] 26 Horologium II: 0.254 0.078 [11] −2.6 [11] 1.69 [11] [NB 1] Local Group: Satellite of Milky Way: 287 ly [23] 27 Draco Dwarf (DDO 208) dE0 pec 0.258 0 ...
1 Jan: 13.8: Big Bang, as seen through cosmic background radiation, which would have been last emitted 14 minutes after midnight 19 Jan 13.1 Oldest known Gamma Ray Burst: 26 Jan 12.85 First galaxies form [4] 16 Mar: 11: Milky Way Galaxy formed 13 May: 8.8: Milky Way Galaxy disk formed 2 Sep: 4.57: Formation of the Solar System: 6 Sep: 4.4 ...
(1 AU and 1 parsec are not to scale, 1 parsec = ~206265 AU) Stellar parallax is the apparent shift of position of any nearby star (or other object) against the background of distant stars. By extension, it is a method for determining the distance to the star through trigonometry, the stellar parallax method.
A multiple star system consists of two or more stars that appear from Earth to be close to one another in the sky. [dubious – discuss] This may result from the stars actually being physically close and gravitationally bound to each other, in which case it is a physical multiple star, or this closeness may be merely apparent, in which case it is an optical multiple star [a] Physical multiple ...
[21] [25] Despite the uncertainties in modeling the unusual supernova, it was also used to estimate a very approximate distance of 8.5 ± 1.3 Mly (2.6 ± 0.4 Mpc) to Messier 81. [20] As a local galaxy, the Central Bureau for Astronomical Telegrams (CBAT) tracks novae in M81 along with M31 and M33 .
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Type II Cepheids (also termed Population II Cepheids) are population II variable stars which pulsate with periods typically between 1 and 50 days. [17] [33] Type II Cepheids are typically metal-poor, old (~10 Gyr), low mass objects (~half the mass of the Sun). Type II Cepheids are divided into several subgroups by period.