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J/A+A/603/A118      Systematic survey of wind mass loss           (Renzo+, 2017)

Systematic survey of the effects of wind mass loss algorithms on the evolution of single massive stars. Renzo M., Ott C.D., Shore S.N., de Mink S.E. <Astron. Astrophys. 603, A118 (2017)> =2017A&A...603A.118R (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Models ; Mass loss Keywords: stars: evolution - stars: massive - stars: mass-loss - stars: winds, outflows - supernovae: general Abstract: Mass loss processes are a key uncertainty in the evolution of massive stars. They determine the amount of mass and angular momentum retained by the star, thus influencing its evolution and presupernova structure. Because of the high complexity of the physical processes driving mass loss, stellar evolution calculations must employ parametric algorithms, and usually only include wind mass loss. We carried out an extensive parameter study of wind mass loss and its effects on massive star evolution using the open-source stellar evolution code MESA. We provide a systematic comparison of wind mass loss algorithms for solar-metallicity, nonrotating, single stars in the initial mass range of 15M to 35M. We consider combinations drawn from two hot phase (i.e., roughly the main sequence) algorithms, three cool phase (i.e., post-main-sequence) algorithms, and two Wolf-Rayet mass loss algorithms. We discuss separately the effects of mass loss in each of these phases. In addition, we consider linear wind efficiency scale factors of 1, 0.33, and 0.1 to account for suggested reductions in mass loss rates due to wind inhomogeneities. We find that the initial to final mass mapping for each zero-age main-sequence (ZAMS) mass has a ∼50% uncertainty if all algorithm combinations and wind efficiencies are considered. The ad-hoc efficiency scale factor dominates this uncertainty. While the final total mass and internal structure of our models vary tremendously with mass loss treatment, final luminosity and effective temperature are much less sensitive for stars with ZAMS mass ≤30M. This indicates that uncertainty in wind mass loss does not negatively affect estimates of the ZAMS mass of most single-star supernova progenitors from pre-explosion observations. Our results furthermore show that the internal structure of presupernova stars is sensitive to variations in both main sequence and post main-sequence mass loss. The compactness parameter ξ∝M/R(M) has been identified as a proxy for the "explodability" of a given presupernova model. We find that ξ varies by as much as 30% for models of the same ZAMS mass evolved with different wind efficiencies and mass loss algorithm combinations. This suggests that the details of the mass loss treatment might bias the outcome of detailed core-collapse supernova calculations and the predictions for neutron star and black hole formation. Description: Output of stellar structure and evolution models computed with MESA, revision 7624. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table34.dat 48 94 Data from tables 3 and 4: end of mass loss phase table5.dat 22 5 Maximum spreads at the end of mass loss phase table6.dat 43 30 Models at the end of the hot phase of evolution table7.dat 40 43 Models at oxygen depletion table8.dat 44 6 Models at the onset of core collapse
Byte-by-byte Description of file: table34.dat
Bytes Format Units Label Explanations
1- 2 I2 Msun Mzams Zero age main sequence mass 4- 7 F4.2 ---- eta Wind efficiency parameter 9- 16 A8 ---- ID Wind combination identifier 18- 22 F5.2 Msun M Final mass 24- 28 F5.2 Msun MHe Helium core mass 30- 34 F5.2 Msun MCO Carbon Oxygen core mass 36- 38 I3 Rsun R Final radius 40- 43 F4.2 [Lsun] log10L log10 luminosity 45- 48 F4.2 [K] log10Teff log10 effective temperature
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 2 I2 Msun Mzams Zero age main sequence mass 4- 6 I3 Rsun DeltaR Maximum spread in radii 8- 12 F5.2 Msun DeltaM Maximum spread in final masses 14- 17 F4.2 Msun DeltaMHe Maximum spread He core mass 19- 22 F4.2 Byte-by-byte Description of file: table6*dat<-A.
Bytes Format Units Label Explanations
1 A1 --- hotwind [VK] Model for hotwind
(1) 3- 4 I2 Msun Mzams Zero age main sequence mass 6- 9 F4.2 --- eta Wind efficiency parameter 12- 17 F6.2 Rsun R Radius at end hot phase 19- 23 F5.2 10+4Lsun L Luminosity at end hot phase 25- 29 F5.2 Msun Mendhot Mass at the end of hot phase 31- 35 F5.2 Msun MHe Helium core mass (at end hot phase) 37- 43 F7.4 10+6yr age Duration of the hot phase
Note (1): Model as follows: V = Vink et al. (2000A&A...362..295V, 2001A&A...369..574V) K = Kudritzki et al. (1989A&A...219..205K)
Byte-by-byte Description of file: table7.dat
Bytes Format Units Label Explanations
1- 2 I2 Msun Mzams Zero age main sequence mass 4- 7 F4.2 ---- eta Wind efficiency parameter 9- 12 A4 ---- ID Wind combination identifier 14- 17 I4 Rsun R Radius at oxygen depletion 19- 23 F5.2 Msun M Final masses at oxygen depletion 25- 29 F5.2 Msun MHe He core mass at oxygen depletion 31- 34 F4.2 Msun MCO CO core mass at oxygen depletion 36- 40 F5.3 ---- xi compactness parameter at O depl.
Byte-by-byte Description of file: table8.dat
Bytes Format Units Label Explanations
1- 2 I2 Msun Mzams Zero age main sequence mass 4- 7 F4.2 ---- eta Wind efficiency parameter 9- 12 A4 ---- ID Wind combination identifier 14- 18 F5.3 ---- xi Compactness parameter at pre-SN 20- 23 F4.2 Msun M4 Mass coordinate of entropy s=4 25- 29 F5.3 ---- mu4 Ertl et al. (2016ApJ...818..124E) parameter (dm/dr at s=4) 31- 34 F4.2 Msun Mrho6 Mass coordinate of density=1e6 36- 39 F4.2 Msun MCO pre-SN CO core mass 41- 44 F4.2 Msun MFe pre-SN iron core mass
Acknowledgements: Mathieu Renzo, m.renzo(at)uva.nl
(End) Mathieu Renzo [Univ. of Amsterdam], Patricia Vannier [CDS] 04-Apr-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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