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Representative lifetimes of stars as a function of their masses The change in size with time of a Sun-like star Artist's depiction of the life cycle of a Sun-like star, starting as a main-sequence star at lower left then expanding through the subgiant and giant phases, until its outer envelope is expelled to form a planetary nebula at upper right Chart of stellar evolution
R ∗ = 1 yr −1 (1 star formed per year, on the average over the life of the galaxy; this was regarded as conservative) f p = 0.2 to 0.5 (one fifth to one half of all stars formed will have planets) n e = 1 to 5 (stars with planets will have between 1 and 5 planets capable of developing life) f l = 1 (100% of these planets will develop life)
Kepler-452 is a G-type main-sequence star located about 1,810 light-years away from Earth [1] in the Cygnus constellation. [5] Although similar in temperature to the Sun, it is 20% brighter, 3.7% more massive and 11% larger.
The most massive stars last an average of a few million years, while stars of minimum mass (red dwarfs) burn their fuel very slowly and can last tens to hundreds of billions of years. [ 129 ] [ 130 ] Lifetimes of stages of stellar evolution in billions of years [ 131 ]
This article documents the most distant astronomical objects discovered and verified so far, and the time periods in which they were so classified. For comparisons with the light travel distance of the astronomical objects listed below, the age of the universe since the Big Bang is currently estimated as 13.787±0.020 Gyr.
In astrobiology and planetary astrophysics, the galactic habitable zone is the region of a galaxy in which life is most likely to develop. The concept of a galactic habitable zone analyzes various factors, such as metallicity (the presence of elements heavier than hydrogen and helium) and the rate and density of major catastrophes such as supernovae, and uses these to calculate which regions ...
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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 ...