12/3/2023 0 Comments Biggest main sequence starOur models show that the Eddington limit is expected to be reached in all stars above ~40 M ⊙ in the LMC, even in lower mass stars in the Galaxy, or in close binaries or rapid rotators. ![]() Furthermore, our coolest models show highly inflated envelopes with masses of up to several solar masses, and appear to be candidates for producing major luminous blue variable eruptions.Ĭonclusions. We find that the hot edge of the S Dor variability region coincides with a line beyond which our models are inflated by more than a factor of two, indicating a possible connection between S Dor variability and inflation. stars above ~40 M ⊙ show inflation, with a radius increase of up to a factor of about 40. We find that all models with luminosities higher than 4 × 10 5 L ⊙, i.e. We find that the local violation of the Eddington limit has severe consequences for the envelope structure, as it leads to envelope inflation, convection, density inversions, and, possibly to, pulsations. While most models adjust their structure such that the local Eddington limit is exceeded at most by a few per cent, our most extreme models do so by a factor of more than seven. When we define an appropriate Eddington limit locally in the stellar envelope, we can show that most stars more massive than ~40 M ⊙ actually exceed this limit, in particular, in the partial ionisation zones of iron, helium, or hydrogen. We find that the Eddington limit is almost never reached at the stellar surface, even for stars up to 500 M ⊙. We use published grids of detailed stellar models, computed with a state-of-the-art, one-dimensional hydrodynamic stellar evolution code using LMC composition, to investigate the envelope properties of core hydrogen burning massive stars. We analyse stellar evolutionary models in which the Eddington limit is reached and exceeded, explore the rich diversity of physical phenomena that take place in their envelopes, and investigate their observational consequences. This brings their envelopes very close to the Eddington limit. Because of the steep mass-luminosity relation, massive main-sequence stars become extremely luminous. Massive stars play a vital role in the Universe, however, their evolution even on the main-sequence is not yet well understood.Īims. Bestenlehner †Īrgelander-Insitut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, GermanyĬontext. Astronomical objects: linking to databasesĭ.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes
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