asymptotic giant branch oor Spaans
asymptotic giant branch
en
The region of the Hertzsprung-Russell diagram populated by evolving low to medium-mass stars.
Vertalings in die woordeboek Engels - Spaans
rama asintótica gigante
en
stars powered by fusion of hydrogen and helium in shell with an inactive core of carbon and oxygen
es
periodo de la evolución estelar que experimentan todas las estrellas de masa intermedia (entre 0,5 y 9-10 masas solares) al final de sus vidas
Evolution of asymptotic giant branch stars
Evolución de las estrellas en la rama asintótica gigante
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voorbeelde
Advanced filtering
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Evolution of asymptotic giant branch stars
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The production sites of the main component are low-mass asymptotic giant branch stars.
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For stars a few times more massive than our Sun, the last phase in their evolution is the asymptotic giant branch (AGB).
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Most of the star's original mass was shed after it passed into the asymptotic giant branch stage, just prior to becoming a white dwarf.
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It was observed in 1971 to be a pre-planetary nebula (PPNe) when it seemed to be an asymptotic giant branch (AGB) B1 supergiant.
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Being greater in mass, the primary is the first of the pair to evolve onto the asymptotic giant branch, where the star's envelope expands considerably.
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Infrared excesses are often the result of circumstellar dust and are common in young stellar objects and evolved stars on the asymptotic giant branch or older.
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The star then follows an evolutionary path called the asymptotic giant branch (AGB) that parallels the other described red giant phase, but with a higher luminosity.
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Its companion, the donor star, was a carbon star on the asymptotic giant branch (AGB), and had produced carbon and s-process elements in its interior.
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The sequence M → MS → S → SC → C-N is hypothesized to be a sequence of increased carbon abundance with age for carbon stars in the asymptotic giant branch.
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When helium was exhausted in the core a helium-burning shell formed in addition to the hydrogen-burning one and the star moved to what astronomers term the asymptotic giant branch, or AGB.
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They are red giants in the very late stages of stellar evolution, on the asymptotic giant branch, that will expel their outer envelopes as planetary nebulae and become white dwarfs within a few million years.
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In the red giant stars of the asymptotic giant branch, the s-process (slow process) is ongoing to produce bismuth-209 and polonium-210 by neutron capture as the heaviest elements to be formed, and the latter quickly decays.
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During the late asymptotic giant branch (LAGB) phase, when mass loss reduces the hydrogen envelope's mass to around 10−2 M☉ for a core mass of 0.60 M☉, a star will begin to evolve towards the blue side of the Hertzsprung–Russell diagram.
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This process is predicted to happen to all Mira variables, but the relatively short duration of thermal pulses (a few thousand years at most) over the asymptotic giant branch lifetime of the star (less than a million years), means we only see it in a few of the several thousand Mira stars known, possibly in R Hydrae.
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With a spectral type of S3,4e-S5,8e, S Cassiopeiae is an S-type star similar to χ Cygni; these are asymptotic giant branch (AGB) stars similar to those of class M except that the dominant spectral bands of metal oxides are formed by metals of the fifth period of the periodic table as zirconium or yttrium.
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A carbon star is typically an asymptotic giant branch star, a luminous red giant, whose atmosphere contains more carbon than oxygen; the two elements combine in the upper layers of the star, forming carbon monoxide, which consumes all the oxygen in the atmosphere, leaving carbon atoms free to form other carbon compounds, giving the star a "sooty" atmosphere and a strikingly ruby red appearance.
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Low mass stars (including the Sun), with a mass between 0.5 M☉ and 1.8–2.5 M☉ depending on composition, do become red giants as their core hydrogen is depleted and they begin to burn helium in core in a helium flash; they develop a degenerate carbon-oxygen core later on the asymptotic giant branch; they finally blow off their outer shell as a planetary nebula and leave behind their core in the form of a white dwarf.
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Beleške [1] R Sculptoris is an example of an asymptotic giant branch (AGB) star.
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First Detection of Rubidium in Asymptotic Giant Branch Stars
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R Sculptoris is an example of an asymptotic giant branch (AGB) star.
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This Hubble Space Telescope image shows the pulsating AGB (asymptotic giant branch) star Mira. NASA image.
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Rubidium-rich Asymptotic Giant Branch stars in the Magellanic Clouds.
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[1] R Sculptoris is an example of an asymptotic giant branch (AGB) star.
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Notes [1] R Sculptoris is an example of an asymptotic giant branch (AGB) star.
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