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11 results for “white dwarf stars”
Faint calcium-rich transient from a double-detonation of a 0.6 M⊙ carbon-oxygen white dwarf star: Complimentary material
<p>Complimentary material to the manuscript.<br> The videos show the hydrodynamical evolution of the merger leading to the double-detonation.</p> <p>The movie "overdensity_formation.mp4" shows slices through the orbital plane color coded with the density (left) and the temperature (right), displaying frame by frame the formation of a cold, overdense fluid parcel after the disruption of the HeWD. <br> <br> The remaining movies show the overall evolution of different quantities with slices through the orbital plane on the left and perpendicular to the orbital plane on the right.</p>
Neutron Star - White Dwarf Binaries: Probing Formation Pathways and Natal Kicks with LISA
<p>We present supplementary datasets accompanying our publication<em> </em><a href="https://arxiv.org/abs/2310.06559">Neutron Star - White Dwarf Binaries: Probing Formation Pathways and Natal Kicks with LISA</a>.<em> </em>These catalogues reperesent the Galactic population of double white dwarf (DWD) and neutron star - white dwarf (NSWD) binaries emitting gravitational waves (GWs) in the <em>Laser Interferometer Space Antenna</em> (LISA) frequency band (0.1 mHz - 1 Hz). The catalogues have been constructed based on binary evolution models <a href="https://arxiv.org/abs/1208.6446">Toonen et al. 2012</a> for DWDs and <a href="https://arxiv.org/abs/1804.01538">Toonen et al. 2018</a> for NSWD binaries, obtained using SeBa binary population synthesis code.</p> <p><strong>Data contents</strong></p> <p>The dataset consists of <strong>12 catalogues </strong>representing Galactic populations of NSWD and/or DWD binaries, which are expected to be the most numerous types of binaries amongt LISA's Galactic sources. Each catalogue is distinguished by its model ID, which specifies the presence of NSWD and/or DWD binaries, the CE model used, CE efficiency values, and the NS natal kick prescription applied (see table below).</p> <p>Each catalogue is structured to describe a binary systems with the following attributes:</p> <ul> <li><strong>Name*</strong>: binary identifier; this consist of a prefix indicating the binary type (<code>'MW_DWD'</code> for a DWD binary, <code>'MW_NSWD_ecc0'</code> for a circular NSWD bianry, or <code>'MW_NSWD_ecc1'</code> for an eccentric NSWD binary) followed by a unique ID number. For example, <code>'MW_DWD 28713637'</code>.</li> <li><strong>Frequency</strong>: present-day GW frequency (Hz).</li> <li><strong>Frequency Derivative</strong>: rate of change of GW frequency over time (Hz^2).</li> <li><strong>Ecliptic Latitude</strong>: in radians (rad).</li> <li><strong>Ecliptic Longitude</strong>: in radians (rad).</li> <li><strong>Amplitude</strong>: GW amplitude (dimensionless).</li> <li><strong>Inclination</strong>: angle between the binary's orbital plane and our line of sight, in radians (rad).</li> <li><strong>Polarization</strong>: Orientation of the GW's polarization, in radians (rad).</li> <li><strong>Initial Phase</strong>: initial phase (rad).</li> <li><strong>Eccentricity</strong>: orbital eccentricity (dimensionless).</li> </ul> <p><strong>*</strong>Note that the <strong>Name </strong>field for eccentric NS+WD binaries (staring with <code>'MW_NSWD_ecc1'</code>) is not unique because these binaries are represented by multiple harmonics sharing the same name ID. The number of harmonics included varies for each binary to ensure that at least 99% of the binary's total GW power is represented. Thus, for each binary, we added harmonics incrementally until this threshold is reached.</p> <table> <tbody> <tr> <td>Model ID</td> <td>WD+WD</td> <td>NS+WD</td> <td>CE model</td> <td>CE efficiency</td> <td>NS natal kick</td> </tr> <tr> <td>1_0</td> <td>Yes</td> <td>No</td> <td>αα</td> <td>αλ=2.00</td> <td>N/A</td> </tr> <tr> <td>1_1</td> <td>Yes</td> <td>Yes</td> <td>αα</td> <td>αλ=2.00</td> <td>Verbunt</td> </tr> <tr> <td>1_2</td> <td>Yes</td> <td>Yes</td> <td>αα</td> <td>αλ=2.00</td> <td>Arzoumanian</td> </tr> <tr> <td>1_3</td> <td>Yes</td> <td>Yes</td> <td>αα</td> <td>αλ=2.00</td> <td>Hobbs</td> </tr> <tr> <td>1_4</td> <td>Yes</td> <td>Yes</td> <td>αα</td> <td>αλ=2.00</td> <td>Blaauw</td> </tr> <tr> <td>2_0</td> <td>Yes</td> <td>No</td> <td>αα2</td> <td>αλ=0.25</td> <td>N/A</td> </tr> <tr> <td>2_1</td> <td>Yes</td> <td>Yes</td> <td>αα2</td> <td>αλ=0.25</td> <td>Verbunt</td> </tr> <tr> <td>2_2</td> <td>Yes</td> <td>Yes</td> <td>αα2</td> <td>αλ=0.25</td> <td>Arzoumanian</td> </tr> <tr> <td>2_3</td> <td>Yes</td> <td>Yes</td> <td>αα2</td> <td>αλ=0.25</td> <td>Hobbs</td> </tr> <tr> <td>2_4</td> <td>Yes</td> <td>Yes</td> <td>αα2</td> <td>αλ=0.25</td> <td>Blaauw</td> </tr> <tr> <td>3_0</td> <td>Yes</td> <td>No</td> <td>αγ</td> <td>αλ=2.00, γ=1.75</td> <td>N/A</td> </tr> <tr> <td>3_1</td> <td>Yes</td> <td>Yes</td> <td>αγ</td> <td>αλ=2.00, γ=1.75</td> <td>Verbunt</td> </tr> </tbody> </table> <p> </p> <h4><strong>Citing the Dataset</strong></h4> <p>When utilising these catalogues in your research, please cite <a href="https://arxiv.org/abs/2310.06559">Korol et al. 2024.</a> We also note our companion data-analysis-focused paper <a href="https://arxiv.org/abs/2310.06568">Moore et al. 2024</a>.</p>
Evolution models of helium white dwarf-main-sequence star merger remnants: the mass distribution of single low-mass white dwarfs
<p>Inlists and data for "<a href="https://ui.adsabs.harvard.edu/#abs/2018MNRAS.474..427Z/abstract">Evolution models of helium white dwarf-main-sequence star merger remnants: the mass distribution of single low-mass white dwarfs</a>"</p>
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
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2013ApJ...772...37D/abstract">Denissenkov et al. (2013)</a>. MESA version 4631.</p> <p>Publication DOI: <a href="https://doi.org/10.1088/0004-637X/772/1/37">10.1088/0004-637X/772/1/37</a></p>
Novel modelling of ultracompact X-ray binary evolution - stable mass transfer from white dwarfs to neutron stars
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2017MNRAS.470L...6S/abstract">Novel modelling of ultracompact X-ray binary evolution - stable mass transfer from white dwarfs to neutron stars</a></p>
New full evolutionary sequences of H- and He-atmosphere massive white dwarf stars using MESA
<p>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></p>
Carbon Shell or Core Ignitions in White Dwarfs Accreting from Helium Stars
<p>MESA inlists and run_star_extras associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2016ApJ...821...28B">Brooks et al. (2016)</a>. MESA version 7624.</p> <p>Publication DOI: <a href="https://doi.org/10.3847/0004-637X/821/1/28">10.3847/0004-637X/821/1/28</a></p>
PTF1 J082340.04+081936.5: A Hot Subdwarf B Star with a Low-mass White Dwarf Companion in an 87-minute Orbit
<p>MESA inlists and run_star_extras associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2017ApJ...835..131K">Kupfer et al. (2017)</a>. MESA version 8118.</p> <p>Publication DOI: <a href="https://doi.org/10.3847/1538-4357/835/2/131">10.3847/1538-4357/835/2/131</a></p>
Accretion-induced Collapse from Helium Star + White Dwarf Binaries
<p>MESA inlists and run_star_extras associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2017ApJ...843..151B">Brooks et al. (2017)</a>. MESA version 7624.</p> <p>Publication DOI: <a href="https://doi.org/10.3847/1538-4357/aa79a6">10.3847/1538-4357/aa79a6</a></p>
Self-consistent MHD simulation of jet launching in a neutron star - white dwarf merger: Complimentary material
<p>Complementary material to the paper.</p> <p>Movies showing different magnitudes during the evolution of the neutron-star white-dwarf merger. All the movies show slices through the orbital plane (on the left) and perpendicular to the orbital plane (on the right right) centred on the neutron star. The region where the gravitational potential is softened around the neutron star is outlined by a black-dashed line.<br> The different videos show the following magnitudes: the ratio between the magnetic pressure and gas pressure (beta), the density, the entropy, the absolute value of the magnetic field, the radial velocity with respect to the neutron-star and the temperature.</p> <p>For every magnitude there are two videos (_01rsol and _003rsol) showing them in a box of 0.1 and 0.03 solar radii respectively.</p>
Heat transport and convective velocities in compositionally-driven convection in neutron star and white dwarf interiors
<p>MESA (version r22.11.1) inlists and source code used for the paper "Heat transport and convective velocities in compositionally-driven convection in neutron star and white dwarf interiors". cool_wd.zip contains the MESA files to reproduce the results discussed in section 4 of the paper. A Python-based Dedalus v3 script to reproduce the 3D numerical simulations presented in section 3 of the paper is included as Compositionally_driven_convection_3D_shell.py.</p>
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