Impact of rotation on stellar models

Meynet, Georges; Maeder, A.; Eggenberger, P.; Ekström, Sylvia; Georgy, Cyril; Chiappini, Cristina; Privitera, Giovanni; Choplin, Arthur

doi:10.1002/asna.201612380

Cited by 7 publications

(3 citation statements)

References 51 publications

(57 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Large studies of the connection between stellar evolution and rotation have already been carried out by Brott et al (2011) and Ekström et al (2012). Similar studies were performed taking into account the dependence of the magnetic field of the star and its rotation velocity by Shultz et al (2019a); Meynet et al (2016) andde Mink et al (2013) for binaries. The result for our sample is shown in the Figure 22.…”

Section: Rotation Velocitymentioning

confidence: 92%

Testing the fossil field hypothesis: could strongly magnetized OB stars produce all known magnetars?

Макаренко

Igoshev

Kholtygin

2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Stars of spectral types O and B produce neutron stars (NSs) after supernova explosions. Most of NSs are strongly magnetized including normal radio pulsars with B ∝ 1012 G and magnetars with B ∝ 1014 G. A fraction of 7–12 per cent of massive stars are also magnetized with B ∝ 103 G and some are weakly magnetized with B ∝ 1 G. It was suggested that magnetic fields of NSs could be the fossil remnants of magnetic fields of their progenitors. This work is dedicated to study this hypothesis. First, we gather all modern precise measurements of surface magnetic fields in O, B, and A stars. Secondly, we estimate parameters for lognormal distribution of magnetic fields in B stars and found μB = 2.83 ± 0.1 log10 (G), σB = 0.65 ± 0.09 for strongly magnetized and μB = 0.14 ± 0.5 log10 (G), $\sigma =0.7_{-0.27}^{+0.57}$ for weakly magnetized. Third, we assume that the magnetic field of pulsars and magnetars have 2.7-dex difference in magnetic fields and magnetars represent 10 per cent of all young NSs and run population synthesis. We found that it is impossible to simultaneously reproduce pulsars and magnetars populations if the difference in their magnetic fields is 2.7 dex. Therefore, we conclude that the simple fossil origin of the magnetic field is not viable for NSs.

show abstract

Section: Rotation Velocitymentioning

confidence: 92%

Testing the fossil field hypothesis: could strongly magnetized OB stars produce all known magnetars?

Макаренко

Igoshev

Kholtygin

2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

Section: Rotation Velocitymentioning

confidence: 99%

Testing the fossil field hypothesis: could strongly magnetised OB stars produce all known magnetars?

Makarenko,

Igoshev,

Kholtygin

2021

Preprint

View full text Add to dashboard Cite

Stars of spectral types O and B produce neutron stars (NSs) after supernova explosions. Most of NSs are strongly magnetised including normal radio pulsars with 𝐵 ∝ 10 12 G and magnetars with 𝐵 ∝ 10 14 G. A fraction of 7-12 per cent of massive stars are also magnetised with 𝐵 ∝ 10 3 G and some are weakly magnetised with 𝐵 ∝ 1 G. It was suggested that magnetic fields of NSs could be the fossil remnants of magnetic fields of their progenitors. This work is dedicated to study this hypothesis. First, we gather all modern precise measurements of surface magnetic fields in O, B and A stars. Second, we estimate parameters for log-normal distribution of magnetic fields in B stars and found 𝜇 𝐵 = 2.83±0.1 log 10 (G), 𝜎 𝐵 = 0.65±0.09 for strongly magnetised and 𝜇 𝐵 = 0.14 ± 0.5 log 10 (G), 𝜎 = 0.7 0.57 −0.27 for weakly magnetised. Third, we assume that the magnetic field of pulsars and magnetars have 2.7 DEX difference in magnetic fields and magnetars represent 10 per cent of all young NSs and run population synthesis. We found that it is impossible to simultaneously reproduce pulsars and magnetars populations if the difference in their magnetic fields is 2.7 DEX. Therefore, we conclude that the simple fossil origin of the magnetic field is not viable for NSs.

show abstract

“…The so-called rotational mixing hides in reality a complex interplay between angular momentum transport, chemical mixing, magnetism, tidal effects, mass loss, ... A state of the art of the problems associated to the modeling of these processes can be found in e.g Buldgen et al (these proceedings) and their impact is discussed in e.g. Meynet et al (2016). The transport of angular momentum by waves and modes is still very difficult to quantify.…”

Section: Model Dependencementioning

confidence: 99%

Current problems in stellar pulsation theory

Dupret¹

2019

Preprint

View full text Add to dashboard Cite

The last decade lead to major progress in asteroseismology and stellar physics with the advent of space missions. Thanks to the richness and precision of current oscillation spectra, sophisticated seismic probing techniques allow us now to pinpoint the limits of our current models of stellar structure and evolution. However, the accuracy of the seismic diagnosis depends on the accuracy of the pulsation models. In solar-like oscillations, the main source of inaccuracy comes from the near-surface layers where the oscillations are non-adiabatic and strongly coupled with turbulent convection. Some pulsating stars rotate fast and this must be accurately taken into account in the modeling of their pulsations. In others, the magnetic field or the dynamic tides could play some role. I propose here an overview of the great achievements and current limitation of asteroseismology.

show abstract

Impact of rotation on stellar models

Cited by 7 publications

References 51 publications

Testing the fossil field hypothesis: could strongly magnetized OB stars produce all known magnetars?

Testing the fossil field hypothesis: could strongly magnetized OB stars produce all known magnetars?

Testing the fossil field hypothesis: could strongly magnetised OB stars produce all known magnetars?

Current problems in stellar pulsation theory

Contact Info

Product

Resources

About