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9 results for “stars: magnetic field”
Reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution - II. Implementation of magnetic braking in MESA and implications for the evolution of surface rotation in OB stars "
<p>This is a reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution - II. Implementation of magnetic braking in MESA and implications for the evolution of surface rotation in OB stars" by Keszthelyi et al. (2020), https://doi.org/10.1093/mnras/staa237</p>
Detecting axisymmetric magnetic fields using gravity modes in intermediate-mass stars
<p>Typical MESA and GYRE inlists associated with <a href="https://ui.adsabs.harvard.edu/abs/2020arXiv200502411V/abstract">Van Beeck et al. (2020)</a>. MESA version 10398 and GYRE version 5.2.</p> <p>Context: Angular momentum (AM) transport models of stellar interiors require improvements to explain the strong extraction of AM from stellar cores that is observed with asteroseismology. One of the often invoked mediators of AM transport are internal magnetic fields, even though their properties, observational signatures and influence on stellar evolution are largely unknown.</p> <p>Aims: We study how a fossil, axisymmetric internal magnetic field affects period spacing patterns of dipolar gravity mode oscillations in main-sequence stars with masses of 1.3, 2.0 and 3.0 <span class="math-tex">\(\mathrm{M}_{\odot}\)</span> . We assess the influence of fundamental stellar parameters on the magnitude of pulsation mode frequency shifts.</p> <p>Methods: We compute dipolar gravity mode frequency shifts due to a fossil, axisymmetric poloidal-toroidal internal magnetic field for a grid of stellar evolution models, varying stellar fundamental parameters. Rigid rotation is taken into account using the traditional approximation of rotation and the influence of the magnetic field is computed using a perturbative approach.</p> <p>Results: We find magnetic signatures for dipolar gravity mode oscillations in terminal-age main-sequence stars that are measurable for a near-core field strength larger than 10<sup>5</sup> G. The predicted signatures differ appreciably from those due to rotation.</p> <p>Conclusions: Our formalism demonstrates the potential for the future detection and characterization of strong fossil, axisymmetric internal magnetic fields in gravity-mode pulsators near the end of core-hydrogen burning from Kepler photometry, if such fields exist.</p> <blockquote> <p>The publication date is the date of acceptance.</p> </blockquote> <p>J. Van Beeck would like to thank researchers M. Michielsen, C. Johnston, and dr. M. G. Pedersen for their valuable input in the MESA and GYRE computations.</p>
Reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities"
<p>This is a reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution - IV. Grids of models at Solar, LMC, and SMC metallicities" by <a href="https://doi.org/10.1093/mnras/stac2598">Keszthelyi et al. (2022).</a></p>
Reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution: V. Models at low metallicity" by Keszthelyi et al. 2024
<p>This is a reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution: V. Models at low metallicity" by <a href="https://ui.adsabs.harvard.edu/abs/2024MNRAS.tmp.1818K/abstract">Keszthelyi et al. 2024</a></p>
Variable stellar outflows as a probe to magnetic fields and other physical characteristics of hot, massive stars
<p>It is now clear that the radiatively driven outflows from hot, massive stars are far more complex than the simple homogeneous and spherically symmetric flows originally envisioned. With the advent of high resolution, high cadence observations of various types in the past decades, a myriad of phenomena have been uncovered that can help us reach a better understanding of the parameters and characteristics of the stars from which these winds originate. This in turn has important ramifications on the various phases of evolution of the star and on the way it will ultimately end its life. In this talk, I will review the many observational signatures of variable stellar outflows of massive stars and describe how they relate to physical characteristics of the underlying star, with a particular emphasis on magnetic fields.</p>
Data for "The Origin of the Bimodal Distribution of Magnetic Fields in Early-type Stars"
<p>Accompanying data and inlists for Jermyn & Cantiello 2020 (ApJ). Models have been computed using MESA revision 11701. A Jupyter notebook is provided to reproduce the figures in the main text. </p>
Inlist files for "Detectability of axisymmetric magnetic fields from the core to the surface of oscillating post-main sequence stars"
<p>Concerned article: "Detectability of axisymmetric magnetic fields from the core to the surface of oscillating post-main sequence stars" by Bhattacharya et al. (submitted).<br>Corresponding author: Shatanik Bhattacharya</p> <p>Inlists for the proof-of-concept stellar models used in this project have been provided here for reproducibility.</p> <p>For the red-giant model, the inlist was executed with MESA version r22.05.1 and MESA-SDK version x86 64-linux-22.6.1. Model 500 (age 4.056 Gyr) was used as the RG in this project.</p> <p>For the sub-giant models, the inlist was executed with MESA version r23.05.1 and MESA-SDK version x86 64-linux-22.6.1. Models 345 (age 3.624 Gyr) and 350 (age 3.702 Gyr) were used as the MSG and LSG models respectively.</p>
Supporting data for "The Initial Magnetic Field Distribution in AB Stars"
<p>These are the inlist and run_star_extras required to reproduce the results of 'The Initial Magnetic Field Distribution in AB Stars', originally used with MESA r15140. The history output files are also included.</p>
Probing fossil magnetic field effects in the core of evolved low-mass stars using mixed-mode frequencies
<p>The recent discovery of the moderate differential rotation between the core and the envelope of intermediate-mass (IM) main-sequence and evolved stars, and the population of IM red giants presenting a surprisingly low-amplitude of their mixed modes (i.e. modes that behave as acoustic modes in their external envelope and as gravity modes in their core) could both be the signature of a strong magnetic field trapped inside the radiative regions of IM stars. Indeed, stars more massive than 1.1 solar mass are known to develop a convective core during their main sequence. The field generated by the dynamo triggered by this convection could be the progenitor of a strong fossil magnetic field trapped inside the core of the star for the rest of its evolution. In this context, the mixed modes observed thanks to space-based asteroseismology can constitute an excellent probe of the deepest layers in IM evolved stars: such magnetic fields may impact their propagation inside the core of these stars, and these perturbations should be visible in asteroseismic data. To unravel which constraints can be obtained from these observations, we theoretically investigate the effects of a plausible mixed magnetic field with various amplitudes on the mixed-mode frequencies of red giants. Applying a perturbative method, we estimate the magnetic splitting of the frequencies of simulated mixed dipolar modes that depends on the magnetic field strength and its configuration. A complete asymptotic analysis is derived, showing the potential of asteroseismology to probe the magnetism at each depth as this is done for stellar rotation. The effects of the mass and the metallicity of the stars are also explored. Finally, we infer an upper limit for the strength of the field and the associated lower limit for the timescale of its action to redistribute angular momentum in stellar interiors.</p>
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