Find research datasets worth reusing

opencc-by-4.0Nov 2021View details →

X-ray Variability of the Massive O star zeta Pup

Analysis of very deep, high resolution X-ray spectroscopy of the early O supergiant zeta Pup, acquired by Chandra in 2018-9, is presented. The cumulative spectrum has an exposure time of 820 kiloseconds (almost 10 days) and covers the wavelength range 3-20 Å. The X-ray broad-band light curve displays significant variability with one clear period, 1.78d, which has been previously detected in optical. The correlation with optical and UV data is discussed, notably in the context of CIRs and (possibly magnetic?) spots on the stellar surface with at least one stable period. The possible correlation of periods with optical and UV data is discussed. The X-ray spectrum is divided into several wavelength bands which are explored for variability. These divisions allow construction of light curves for hard, medium, and soft bands individually (which allows calculations of time-dependent hardness ratios), along with independently investigating the temporal behavior of strong X-ray emission lines. New constraints on the structure of stellar winds for the most massive stars are discussed.

opencc-by-4.0Oct 2021View details →

The cosmic carbon footprint of massive stars stripped in binary systems

# Structure ## Overview The folder data/ contains the inlists and mod files used in this work. Intermediate data (like history or profile) files must be regenerated from the provided files. The folder plots/ contains a jupyter notebook set-up to remake all plots (assuming the data is saved in the data/ folder). There are also additional scripts and files needed to reproduce this work. The griffith.txt file is the data from https://ui.adsabs.harvard.edu/abs/2021arXiv210309837G/abstract and was accessed from https://github.com/giganano/VICE/blob/master/vice/yields/ccsne/S16/W18F/FeH0/v0/explosive/c.dat ## Data folders corehedep - Evolution from ZAMS to end of core helium burning coreodep - Evolution from end of core helium burning to end of core oxygen burning cc - Evolution from end of core oxygen burning up to core collapse ccsn - Evolution from core collapse to shock breakout engmc - Tests variations in the injection energy and mass cut of ccsn explosions spacetime - Test variations in space/time resolution of ccsn explosions ccsn_t_m - Test variations in injection time and injection mass of ccsn explosions ## Sub-folders corehedep/base - Base folder with inlists for this set of models corehedep/binary - Contains a folder for each mass for the binary-stripped stars (11-45) corehedep/single - Contains a folder for each mass for the single stars (11-45) corehedep/net/23 - A single star 23msun model ran with a larger nuclear network coreodep/base - Base folder with inlists for this set of models coreodep/binary  - Contains a folder for each mass for the binary-stripped stars (11-45) coreodep/single - Contains a folder for each mass for the single stars (11-45) coreodep/mesh - Test variations with respect to space and time during carbon burning coreodep/overshoot - Test variations with respect to overshoot during carbon burning coreodep/net - A single star 23msun model ran with a larger nuclear network cc/base - Base folder with inlists for this set of models cc/binary - Contains a folder for each mass for the binary-stripped stars (11-45) cc/single  - Contains a folder for each mass for the single stars (11-45) ccsn/base - Base folder with inlists for this set of models ccsn/binary  - Contains a folder for each mass for the binary-stripped stars (11-45) ccsn/single  - Contains a folder for each mass for the single stars (11-45) ccsn/laplace_binary - Contains core collapse explosions of the binary-stripped models from Laplace et al 2021 ccsn/laplace_single - Contains core collapse explosions of the single star models from Laplace et al 2021 spacetime/base - Base folder with inlists for this set of models spacetime/binary - Test variations in space/time resolution of ccsn explosions ccsn_t_m/base - Base folder with inlists for this set of models ccsn_t_m/binary - Test variations in injection time and injection mass of ccsn explosions engmc/base - Base folder with inlists for this set of models engmc/binary - Tests variations in the injection energy and mass cut of ccsn explosions ## Notes Folders with the name '_k' have enhanced profile output for use in Kippenhan plots. Folders with the name '_v' have enhanced profile output for use in the video of the shock explosion. Each numbered folder contains a set of inlists used (which usually only vary one or two parameters), the rest of the inlists are stored in the base/ folders (See the submit.sh files for how to get MESA to read these files). They also contain a initial.mod file (which is the starting point for this phase of evolution), this is a softlink to the final.mod file from the previous phase (thus coreodep soft links to files in corehedep, corehdep uses MESA's built in ZAMS models to start). The folders that handle the core collapse explosions have additional .mod files that handle each phase of the explosion. See the base/ folders for details on the order. ## Files cacheHist.py - Runs mesaplot code to turn history files into a python binary file for faster reading. plotKip.py - Does a quick kippenhan plot for diagnostics

opencc-by-4.0Jun 2024View details →

Merger seismology: distinguishing massive merger products from genuine single stars using asteroseismology (online data)

<h1>Input and output files for "Merger seismology: distinguishing massive merger products from genuine single stars using asteroseismology" (Henneco et al. 2024b)</h1> This repository contains the MESA and GYRE input files required to reproduce the models used in Henneco et al. (2024b), as well as some of the output files. [MESA version] MESA r12778 MESA SDK 20.3.2 [GYRE version] GYRE 7.0 MESA SDK 22.6.1   <h2>input_files</h2> This directory contains the template input files for the MESA and GYRE models. <h3>gyre</h3> - gyre_nonrot_template.in: GYRE inlist for computations without rotation - gyre_rot_template.in: GYRE inlist for computations, including rotation using the TAR - gyre_rot_pert_template: GYRE inlist for computations including rotation using the perturbative approach <h3>mesa</h3> - genuine_single: MESA work directory for genuine single stars - merger_product: MESA work directory for merger products via the fast accretion method - zams_z0142_y2703.data: ZAMS models used to start all MESA computations from <h2> </h2> <h2>output</h2> <h3>mesa</h3> In this directory, we provide the MESA history and profile (GYRE format only) output for the MESA models used in our work. The more detailed regular profile files are left out because of storage constraints, but these can be transferred upon reasonable request. - mXX_plus_mYY_at_rZZ: XX + YY Msol merger product model where the fast accretion method was invoked when the HG star had a radius of ZZ Rsol - mXX: genuine single-star model of XX Msol <h3>gyre</h3> This directory contains the GYRE summary files and input files (with the frequency ranges specific to these models). The detail files are left out because of storage constraints, but these can be transferred upon reasonable request.  [suffixes] NAD: nonadiabatic computations pmodes: computations in frequency ranges appropriate for pressure modes Om20_PERT: computations including rotation (20% of critical) using the perturbative approach Om20_TAR: computations including rotation (20% of critical) using the TAR Except for the computations in `m6.0_plus_m2.4_at_r9.0`, the GYRE computations have been made only for a specific MESA profile (the profile at the time when the models were seismically compared). These are: - m6.0_plus_m2.4_at_r9.0: profile 38 - m7.8: profile 14 - m9.0_plus_m6.3_at_r10.4: profile 62 - m13.6: profile 16 For the `m6.0_plus_m2.4_at_r9.0` model, GYRE computations have been made for profiles 27 -- 52 (see Section 4.2).

Pre-supernova outbursts via wave heating in massive stars - I. Red supergiants

MESA inlists associated with Fuller (2017). MESA version 7624. Publication DOI: <a href="https://doi.org/10.1093/mnras/stx1314">10.1093/mnras/stx1314</a>

Asymmetric core collapse of rapidly rotating massive star

MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2018MNRAS.474.2419G/abstract">Gilkis (2018)</a>. MESA version 7624. Publication DOI: 10.1093/mnras/stx2934<a href="https://doi.org/10.1093/mnras/stx2934">10.1093/mnras/stx2934</a>

Pre-explosion dynamo in the cores of massive stars

Inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2017MNRAS.464.3249S">Soker & Gilkis (2017)</a>. MESA version 7624. Publication DOI: <a href="https://doi.org/10.1093/mnras/stw2546">10.1093/mnras/stw2546</a>

The stability of massive main-sequence stars as a function of metallicity

MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2012MNRAS.423.3397S">The stability of massive main-sequence stars as a function of metallicity</a>

Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars

MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2013ApJS..208....4P">Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars</a>

Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions

MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2018ApJS..234...34P/abstract">Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions</a>

Modeling the early evolution of massive OB stars with an experimental wind routine. The first bi-stability jump and the angular momentum loss problem

MESA run_star_extras associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2017A&A...598A...4K">Keszthelyi et al. (2017)</a>. MESA version 7624. Publication DOI: <a href="https://doi.org/10.1051/0004-6361/201629468">10.1051/0004-6361/201629468</a>

New full evolutionary sequences of H- and He-atmosphere massive white dwarf stars using MESA

MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2018MNRAS.480.1547L">New full evolutionary sequences of H- and He-atmosphere massive white dwarf stars using MESA</a>

Code dependencies of pre-supernova evolution and nucleosynthesis in massive stars: evolution to the end of core helium burning

MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2015MNRAS.447.3115J">Jones et al. (2015)</a>. MESA version 3709. Publication DOI: <a href="https://doi.org/10.1093/mnras/stu2657">10.1093/mnras/stu2657</a> Files are also available in a gihub repository <a href="https://github.com/swjones/mesa-Teile/tree/master/Jones.etal.2015.MNRAS.447.4.3115">here</a>

Ultra-luminous X-ray sources and neutron-star-black-hole mergers from very massive close binaries at low metallicity

MESA inlists, run_star_extras, and data associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2017A&A...604A..55M">Marchant et al. (2017)</a>. MESA version 8118. Publication DOI: <a href="https://doi.org/10.1051/0004-6361/201630188">10.1051/0004-6361/201630188</a> Files are also available in a gihub repository <a href="https://github.com/orlox/mesa_input_data/tree/master/2016_ULX">here</a> Upload includes post-processed simulation output in the files Z-XX.tar.xz, where XX represents the metallicity (Z-25.tar.gz is for a metallicity of log10(Z)=-2.5). Each folder inside the archive corresponds to a single MESA simulation, with the name indicating the value of log10(M_1), q=M2/M1 and the orbital period in days. For example, the directory 1.600_0.500_0.900 corresponds to the simulation with log10(M1/Msun)=1.6, M2/M1=0.5 and Porb=0.9 days. Each folder is also a MESA template folder, containing all input files neccesary to reproduce that individual simulation. The file summary_tables.tar.gz contains summarized information for each simulation in ascii format.

opencc-by-4.0Aug 2024View details →

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

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>

opencc-by-4.0Sep 2024View details →

It's written in the massive stars: The role of stellar physics in the formation of black holes

This repository contains additional data for the paper "It's written in the massive stars: The role of stellar physics in the formation of black holes" by E. Laplace, F.R.N. Schneider, and Ph. Podsiadlowski (2024).

Yields from paper: ALUMINIUM-26 FROM MASSIVE BINARY STARS II. ROTATING SINGLE STARS UP TO CORE-COLLAPSE AND THEIR IMPACT ON THE EARLY SOLAR SYSTEM

Title: Aluminium-26 From Massive Binary Stars II: ROTATING SINGLE STARS UP TO CORE-COLLAPSE AND THEIR IMPACT ON THE EARLY SOLAR SYSTEM Authors: Brinkman H.E., den Hartogh J. W., Doherty C.L., Pignatari M., Lugaro M. ================================================================================ Description of contents: A .tar.gz package containing three files with the complete set of yields from the models presented in this paper. YieldsNR.txt contains the yields for the non-rotating models and Yields150.txt and Yields300.txt the yields for the models rotating at an initial velocity of 150 and 300 km/s, respectively. ================================================================================

Exploring uncertainties in the evolution of massive stars with METISSE

In the era of advanced electromagnetic and gravitational wave detectors, it has become increasingly important to effectively combine and study the impact of stellar evolution on binaries and star clusters. Systematic studies dedicated to exploring uncertain parameters in stellar evolution are required to account for the recent observations of the stellar populations. While fitting formulae to stellar tracks in the form of Single Star Evolution (SSE) code remain a popular choice for modelling stellar evolution in population synthesis codes, they are less adaptable to changes in the stellar tracks. Hence, we have developed a Method of Interpolation for Single Star Evolution (METISSE) as an alternative to SSE. It makes use of interpolation between sets of pre-computed stellar tracks to approximate evolution parameters for a population of stars. METISSE is comparable to SSE in performance and can reproduce tracks from different stellar evolution codes quite accurately. In this work, we apply METISSE with detailed stellar tracks computed by the Modules for Experiments in Stellar Astrophysics (MESA), Bonn Evolutionary Code (BEC), to study the impact of uncertainties in stellar evolution on a population of massive stars. We find that different physical ingredients used in the evolution of stars, such as the treatment of radiation dominated envelopes, can impact their evolutionary outcome, including remnant masses and maximal radial expansion. The differences in the predictions of different stellar models can help us account for the present day observations of stellar populations.

Variable stellar outflows as a probe to magnetic fields and other physical characteristics of hot, massive stars

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.

3D MHD Simulations of Magnetospheres from Obliquely Rotating Magnetic Massive Stars

We present results from the first 3D MHD simulations of the stellar-wind-fed magnetospheres from massive stars with a dipole magnetic axis that has an arbitrary obliquity angle (\(\beta\)) to the star’s rotation axis. As an initial direct application, we examine the global structure of co-rotating disks for tilt angles \(\beta =\) 0, 45 and 90 degrees using \(\zeta\) Pup stellar parameters as a prototype. We find that for models with rapid stellar rotation (~0.7 critical rotation), accumulation surfaces closely resemble the form predicted by the analytic Rigidly Rotating Magnetosphere (RRM) model, but with a mass distribution and outer disk termination set by centrifugal breakout processes. Moreover, models with low stellar rotation rates show a far more variable and complex structure than simple predictions. These models can be used to synthesize rotational modulation of photometric absorption and H-alpha emission for a direct comparison with observations.

State-of-the-art evolution models for single, binary and magnetic massive stars

The Universe is threaded by magnetic fields on all scales, from planetary systems to galaxy clusters. In massive stars, they play a pivotal and multifaceted role. They are thought to be crucial in transporting angular momentum throughout the stellar interior and maintaining the overall angular-momentum budget. They may also contribute to chemical mixing, can interact with convective fluid motions and may give rise to distinct seismic signatures. For example, the spin rates of white dwarfs, neutron stars and black holes are strongly determined by the coupling of a star’s core to its envelope. In this talk, I will discuss recent progress in our understanding of how magnetic fields affect single and binary stars, and what are possible origins of the different types of magnetic fields in massive stars. In particular, I will highlight connections to observations and how these can be used to further our understanding of how magnetic fields influence the evolution and final fates of stars.