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The IACOB project XI. No increase of mass-loss rates over the bistability region
Solar and Stellar Astrophysics · Submitted 16 May 2024
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Our results show no increase in the mass-loss rates over the bistability jump.
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The abstract, sentence by sentence
The properties of blue supergiants are key for constraining the end of the main sequence (MS) of massive stars. Whether the observed drop in the relative number of fast-rotating stars below $\sim$21$\,$kK is due to enhanced mass-loss rates at the location of the bistability jump, or the result of the end of the MS is still debated. Here, we combine newly derived estimates of photospheric and wind parameters with Gaia distances and wind terminal velocities from the literature to obtain upper limits on the mass-loss rates for a sample of 116 Galactic luminous blue supergiants. The parameter space covered by the sample ranges between 35-15$\,$kK in $T_{\rm eff}$ and 4.8-5.8$\,$dex in log(L/L$_{\odot}$). Our results show no increase in the mass-loss rates over the bistability jump. Therefore, we argue that the drop in rotational velocities cannot be explained by enhanced mass loss. Since a large jump in the mass-loss rates is commonly included in evolutionary models, we suggest an urgent revision of the currently used default prescriptions.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The properties of blue supergiants are key for constraining the end of the main sequence (MS) of massive stars. | background 1.00 | 0.05 | 0.02 | asserted 1.00 |
| s1 | Whether the observed drop in the relative number of fast-rotating stars below $\sim$21$\,$kK is due to enhanced mass-loss rates at the location of the bistability jump, or the result of the end of the MS is still debated. | gap 0.81 | 0.04 | 0.03 | hedged possibility 0.58 |
| s2 | Here, we combine newly derived estimates of photospheric and wind parameters with Gaia distances and wind terminal velocities from the literature to obtain upper limits on the mass-loss rates for a sample of 116 Galactic luminous blue supergiants. | method 0.92 | 0.90 | 0.03 | asserted 0.91 |
| s3 | The parameter space covered by the sample ranges between 35-15$\,$kK in $T_{\rm eff}$ and 4.8-5.8$\,$dex in log(L/L$_{\odot}$). | method 0.70 | 0.66 | 0.02 | asserted 0.99 |
| s4 | Our results show no increase in the mass-loss rates over the bistability jump. | result 1.00 | 0.96 | 0.96 | asserted 1.00 |
| s5 | Therefore, we argue that the drop in rotational velocities cannot be explained by enhanced mass loss. | interpretation 1.00 | 0.39 | 0.30 | hedged possibility 0.53 |
| s6 | Since a large jump in the mass-loss rates is commonly included in evolutionary models, we suggest an urgent revision of the currently used default prescriptions. | future work 0.81 | 0.13 | 0.12 | hedged possibility 0.96 |
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Original abstract
The properties of blue supergiants are key for constraining the end of the main sequence (MS) of massive stars. Whether the observed drop in the relative number of fast-rotating stars below $\sim$21$\,$kK is due to enhanced mass-loss rates at the location of the bistability jump, or the result of the end of the MS is still debated. Here, we combine newly derived estimates of photospheric and wind parameters with Gaia distances and wind terminal velocities from the literature to obtain upper limits on the mass-loss rates for a sample of 116 Galactic luminous blue supergiants. The parameter space covered by the sample ranges between 35-15$\,$kK in $T_{\rm eff}$ and 4.8-5.8$\,$dex in log(L/L$_{\odot}$). Our results show no increase in the mass-loss rates over the bistability jump. Therefore, we argue that the drop in rotational velocities cannot be explained by enhanced mass loss. Since a large jump in the mass-loss rates is commonly included in evolutionary models, we suggest an urgent revision of the currently used default prescriptions.
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Estimates of the effective temperature (), surface gravity (), and the wind-strength parameter ($Q$) were obtained by means of quantitative spectroscopic analysis, employing models calculated with the FASTWIND code [ref] , as described in [ref] .
The IACOB project X. Large-scale quantitative spectroscopic analysis of Galactic luminous blue stars · Sample, data, and models · 1.00
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