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opencc-by-4.0Oct 2020View details →

Three-component modelling of C-rich AGB-star winds V. – dataset

The provided data include all parameter files, binary output files, and log files that are the basis for the publication in MNRAS. The file 'file_listing.txt' contains a complete list of files and directories in all gzipped tar files. Each individual gzipped tar file is formatted as follows:  Mm.m_Ll.ll_Ttttt_CtOc.cc.tar.gz where  m.m  :: the assumed mass of the model, in solar masses  l.ll :: The assumed luminosity, in log10(solar luminosities)  tttt :: The effective temperature of the star, in Kelvin.  c.cc :: The carbon-to-oxygen excess, in log10(n_C/n_H-n_O/n_H)+12 The contents vary according to the model, but here is the general directory structure:  nodr/  :: non-drift / PC models  drift/ :: drift models  nodr/init  drift/init :: Initial model files created using John Connor. File suffixes are the following:  .par :: Plain-text parameter file that contains all parameters that are          different from the respective default value in the model.      Consequently, to see all used parameters it is necessary to look in      the log file (see below).  .bin :: Binary file that contains converged models. Each model is stored in          two versions, first the previous time step and then the current time      step (both are needed to restart model calculations at that time      step).          The initial model file only contains one model; where the previous      time step data are the same as the current time step data.          The format of this file is explained below.          Note! These files can get pretty large and are therefore only        available for a smaller number of the models here. Please ask the        corresponding author for the missing files should the need appear.  .log :: Plain-text log file that shows the used model parameters and a number          of key properties for each converged model. The encoding of this file      is UTF-8.  .inf :: Plain-text secondary log file that contains the header of the          [primary] log file as well as timing information.  .tpb :: Secondary binary file that contains a number of properties specified          at the outer boundary, typically for each consecutive time step.  .lis :: Plain-text file with the iteration history. Available for some files.  .liv :: Plain-text file with values specified for a number of properties at          each gridpoint. Available for a smaller number of files.  .inp :: Plain-text file that is used to launch a model; some are still there.  .eps :: Encapsulated PostScript files created by John Connor when calculating          the initial model. Model evolution structure - file endings before the suffix:  _rlx :: Files related to relaxing the T-800 calculations on the initial model          created by John Connor.  _exp :: Files related to expanding the initially compact model to using the          full radial domain.  _fix :: Files related to the intermediate stage where calculations are changed          from expansion to outflow.            _out :: Files related to the outflow stage of the calculations; this is what          you want to look at to see the wind evolution. Results in the paper      are calculated using these data.    Note! Some outflow stage calculations continue the evolution of the previous    set of files. The underlying reason for continued calculations is typically    that the calculated time interval is too short. Such files are typically    given the extension '_cont.lin_out', '_cont2.lin_out', etc. Load files:   Two tools are provided here that can load the binary data files using the   Interactive Data Language (IDL):   sc_load_bin (for files with the suffix '.bin'):     Loads the full content of a T-800 binary file and returns a structure     with the data.   sc_load_tpb (for files with the suffix '.tpb'):     Loads the full content of a T-800 'tpb' binary file and returns a     structure with the data.     Note! Due to the way models run on clusters, this file is sometimes       incomplete; this happens when the model code T-800 is stopped as the       cluster-specific walltime is reached. If this is the case, it is       necessary to use the binary file instead, where data are saved       typically every 20:th time step.   Alternative tools for use with Python and Julia could be considered for   writing, but where not yet available when this dataset was made public.   Please contact the corresponding author for a current status on this issue.

opencc-by-4.0Dec 2023View details →

Aboveground Biomass (AGB) in the Boreal Region: Dataset for Supporting Biomass Recovery Analysis

This package supplements the following paper submitted to Nature: Biomass recovery carbon gains surpass fire losses over boreal forests during the last decades. This dataset contains the Aboveground Biomass (AGB) map (unit: Mg/ha) for the boreal region in 2020 at ~100m resolution.The global AGB dataset, upon which this regional subset is based, was initially developed by Yu et al. (2023). The preprint version of the corresponding AGB data paper has been made available online and can be accessed at <a href="https://doi.org/10.5281/zenodo.7583611">https://doi.org/10.5281/zenodo.7583611</a>. This paper is currently under peer review. The AGB map for the boreal region, as featured in our Nature submission, is provided here for reference and further research.

opencc-by-4.0Mar 2024View details →

AGB_VM: 0.25-degree gridded annual aboveground biomass estimates in Alaska and northwestern Canada 2003-2017..

Gridded 0.25-degree annual estimates of aboveground vegetation biomass (AGB) for diverse arctic and boreal ecosystems in Alaska and northwestern Canada years 2003-2017. AGB was estimated from integrated microwave vegetation optical depth (VOD) (Vegetation Optical Depth Climate Archive (VODCA) (Moesinger et al., 2020)) and optical-multispectral vegetation indices from the MODerate Resolution Imaging Spectroradiometer (MODIS) satellite remote sensing datasets. This work was conducted through NASA's Arctic and Boreal Vulnerability Experiment (ABoVE).

opencc-by-4.0Nov 2022View details →

Cool, Luminous, and Highly Variable Stars in the Magellanic Clouds. II: Spectroscopic Data of Thorne-Zytkow Object and Super-AGB Star Candidates

This dataset contains Magellan MIKE spectroscopy of a population of cool, luminous stars in the Magellanic Clouds, a sample of confirmed Magellanic Cloud red supergiants, and spectrophotometric standard stars. The spectra were analyzed in the paper "Cool, Luminous, and Highly Variable Stars in the Magellanic Clouds. II: Spectroscopic and Environmental Analysis of Thorne-\.Zytkow Object and Super-AGB Star Candidates" by O'Grady et al. (2022). More details are provided in the README.

opencc-by-4.0Dec 2021View details →

A WISE view of extreme AGB stars

The files in this distribution are related to the paper: "A WISE view of extreme AGB stars", by M.A.T. Groenewegen  published in Astronomy & Astrophysics 659, A145 (2022).

opencc-by-4.0Mar 2019View details →

The C-flame Quenching by Convective Boundary Mixing in Super-AGB Stars and the Formation of Hybrid C/O/Ne White Dwarfs and SN Progenitors

MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2013ApJ...772...37D/abstract">Denissenkov et al. (2013)</a>. MESA version 4631. Publication DOI: <a href="https://doi.org/10.1088/0004-637X/772/1/37">10.1088/0004-637X/772/1/37</a>

opencc-by-4.0Mar 2019View details →

Dust formation and mass loss around intermediate-mass AGB stars with initial metallicity Zini ≤ 10-4 in the early Universe - I. Effect of surface opacity on stellar evolution and the dust-driven wind

MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2017MNRAS.466.1709T">Dust formation and mass loss around intermediate-mass AGB stars with initial metallicity Zini ≤ 10-4 in the early Universe - I. Effect of surface opacity on stellar evolution and the dust-driven wind</a>

opencc-by-4.0Jun 2021View details →

SPH modelling of companion-perturbed AGB outflows including a new morphology classification scheme

ABSTRACT Context. Asymptotic giant branch (AGB) stars are known to lose a significant amount of mass by a stellar wind, which controls the remainder of their stellar lifetime. High angular-resolution observations show that the winds of these cool stars typically exhibit mid- to small-scale density perturbations such as spirals and arcs, believed to be caused by the gravitational interaction with a (sub-)stellar companion. Aims. We aim to explore the effects of the wind-companion interaction on the 3D density and velocity distribution of the wind, as a function of three key parameters: wind velocity, binary separation and companion mass. For the first time, we compare the impact on the outflow of a planetary companion to that of a stellar companion. We intend to devise a morphology classification scheme based on a singular parameter. Methods. We ran a small grid of high-resolution polytropic models with the smoothed particle hydrodynamics (SPH) numerical code Phantom to examine the 3D density structure of the AGB outflow in the orbital and meridional plane and around the poles. By constructing a basic toy model of the gravitational acceleration due to the companion, we analysed the terminal velocity reached by the outflow in the simulations. Results. We find that models with a stellar companion, large binary separation and high wind speed obtain a wind morphology in the orbital plane consisting of a single spiral structure, of which the two edges diverge due to a velocity dispersion caused by the gravitational slingshot mechanism. In the meridional plane the spiral manifests itself as concentric arcs, reaching all latitudes. When lowering the wind velocity and/or the binary separation, the morphology becomes more complex: in the orbital plane a double spiral arises, which is irregular for the closest systems, and the wind material gets focussed towards the orbital plane, with the formation of an equatorial density enhancement (EDE) as a consequence. Lowering the companion mass from a stellar to a planetary mass, reduces the formation of density perturbations significantly. Conclusions. With this grid of models we cover the prominent morphology changes in a companion-perturbed AGB outflow: slow winds with a close, massive binary companion show a more complex morphology. Additionally, we prove that massive planets are able to significantly impact the density structure of an AGB wind. We find that the interaction with a companion affects the terminal velocity of the wind, which can be explained by the gravitational slingshot mechanism. We distinguish between two types of wind focussing to the orbital plane resulting from distinct mechanisms: global flattening of the outflow as a result of the AGB star’s orbital motion and the formation of an EDE as a consequence of the companion’s gravitational pull. We investigate different morphology classification schemes and uncover that the ratio of the gravitational potential energy density of the companion to the kinetic energy density of the AGB outflow yields a robust classification parameter for the models presented in this paper.

opencc-by-4.0Mar 2020View details →

The VMC Survey - XXXVII. Pulsation periods of dust enshrouded AGB stars in the Magellanic Clouds

FigA1.tar and FigC2.tar contain postscript files of the 1299 light curves  and 254 spectral energy distributions, respectively, as described in the paper.

opencc-by-4.0Jun 2024View details →

AGB_China's boreal forests_10m_2018

Open the record for dataset details and reuse information.

opencc-by-4.0Jul 2024View details →

Data for "SPH modelling of AGB wind morphology in hierarchical triple systems & comparison to observation of R Aql"

<div> Additional material to Malfait et al. 2024, subm. "SPH modelling of AGB wind morphology in hierarchical triple systems & comparison to observation of R Aql" This contains input files and final output dumps of the Phantom simulations of this paper. The code used to perform the simulations is available at: <a href="https://github.com/danieljprice/phantom">https://github.com/danieljprice/phantom.</a> Splash (<a href="https://github.com/danieljprice/splash">https://github.com/danieljprice/splash</a> ) and Plons (<a href="https://github.com/Ensor-code/plons">https://github.com/Ensor-code/plons</a> ) were used to create figures and plots from this data.   </div>

opencc-by-4.0Sep 2024View details →

Appendices A-B-C for Malfait et al. 2024(a), Impact of HI cooling and study of accretion disks in AGB wind-companion smoothed particle hydrodynamic simulations

Appendices A, B, C with figures, of the paper Malfait et al. 2024(a) "Impact of HI cooling and study of accretion disks in AGB wind-companion smoothed particle hydrodynamic simulations".