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993 results for “T Dwarfs”
Self-consistent Models of Y Dwarf Atmospheres with Water Clouds and Disequilibrium Chemistry
<p>This data set consists of 1d radiative-convective equilibrium models intended for Y Dwarfs or cool giant planets with negligible levels of external irradiation, computed using coolTLUSTY and a recently updated set of molecular absorption cross sections. Models span effective temperatures of 200 - 600 K, metallicities of [-0.5], [0], and [+0.5] dex, and surface gravities of log10(g / [cm/s^2]) = 3.5 - 5.0, and are computed for both cloudy and clear cases, in thermochemical equilibrium and with nonequilibrium carbon and nitrogen chemistry due to vertical mixing. Models extend from 0.5 microns to 300 microns with 30,000 frequency points evenly spaced in ln(frequency), which corresponds to an average resolving power of R ~ 4340.</p> <p>See README.txt for a description of file formats, naming conventions, and decompressed sizes.</p> <p>A more thorough summary of the assumptions made in computing these models and a walk-through of their properties can be found in Lacy & Burrows 2023 "Self-consistent Models of Y Dwarf Atmospheres with Water Clouds and Disequilibrium Chemistry" accepted for publication in the Astrophysical Journal and available on arXiv.</p> <p>If you make use of these models please cite that publication, along with this zenodo data set.</p>
Inlist Files for Effects of Full Sphere Convection On M-Dwarf Dynamo Action, Flux Emergence, and Spin-Down
<p>Inlist files for a model of a ZAMS 0.3 M_sun star used as background for global convection simulations in <em>Effects of Full Sphere Convection On M-Dwarf Dynamo Action, Flux Emergence, and Spin-Down</em>. Run using MESA version r12115.</p>
Data release for "Identifying LISA verification binaries among the Galactic population of double white dwarfs"
<p>Posterior samples and SNR calculations associated with <em>Identifying LISA verification binaries among the Galactic population of double white dwarfs</em> (<a href="https://arxiv.org/abs/2210.10812">arxiv:2210.10812</a>, <a href="https://doi.org/10.1093/mnras/stad1288">MNRAS, 522, 5358 (2023)</a>).</p> <p>The <code>data</code> folder contains the following:</p> <ul> <li><code>vb_table</code>: Verification binary (VB) candidate properties obtained from electromagnetic (EM) observations. This data was compiled by Kupfer et al. and is available at <a href="https://gitlab.in2p3.fr/LISA/lisa-verification-binaries">https://gitlab.in2p3.fr/LISA/lisa-verification-binaries</a> (accessed on 2022 September 2). Used in Table 1.</li> <li><code>snr</code>: SNR calculations for each VB candidate as a function of mission duration. Used in Figure 2.</li> <li><code>basic</code>: Gravitational-wave (GW) parameter estimation study of each VB candidate. Used in Table 2 and Figure 3.</li> <li><code>detection_time</code>: VB SNR calculations with source property (and LISA launch time) uncertainty taken into account. Used in Figure 1 and Figure 4.</li> <li><code>em_priors</code>: GW parameter estimation study with EM information included in the priors. Used in Figure 5.</li> <li><code>unknown_noise</code>: GW parameter estimation study with the inclusion of noise parameters to vary the PSD. Used in Figure 6.</li> <li><code>filtered_populations</code>: Source properties of DWDs nearby in frequency to each VB candidate. See the <code>confused_sources.ipynb</code> notebook. Used in Figure 7.</li> <li><code>confusion_snr</code>: SNR calculations of the above confusion sources. Used in Figure 7.</li> <li><code>confusion</code>: A analysis of V803Cen with a realistic Galactic population of DWDs included in the data. Used in Figure 8.</li> </ul> <p>Code to reproduce every figure from the paper is available in <code>plots</code>.</p> <p>Supplementary notebooks associated with the generation of a realistic data instance (i.e. including a simulated Galactic population of DWDs nearby in frequency to V803Cen) can be found in <code>notebooks</code>.</p>
White Dwarfs Revealed in Gaia's Candidate Compact Object Binaries
<p>Discovery and characterisation of black holes (BHs), neutron stars (NSs), and white dwarfs (WDs) with detached luminous companions (LCs) in wide orbits are exciting because they are important test beds for dark remnant (DR) formation physics as well as binary stellar evolution models. Recently, 187 candidates have been identified from <em>Gaia</em>'s non-single star catalog as wide orbit (P<sub>orb</sub>/day>45), detached binaries hosting DRs. We identify UV counterparts for 49 of these sources in the archival GALEX data. Modeling the observed spectral energy distribution (SED) spanning FUV-NUV to IR for these sources and stellar evolution models, we constrain the LC properties including mass, bolometric luminosity, and effective temperature for these 49 sources. Using the LC masses, and the astrometric mass function constrained by <em>Gaia,</em> we constrain the DR masses for these sources. We find that 9 have masses clearly in the NS or BH mass range. Fifteen sources exhibit significant NUV excess and 4 show excess both in FUV and NUV. The simplest explanation for these excess UV fluxes is that the DRs in these sources are WDs. Using SED modeling we constrain the effective temperature and bolometric luminosity for these 15 sources. Our estimated DR masses for all of these 15 sources are lower than the Chandrasekhar mass limit for WDs. Interestingly, five of these sources had been wrongly identified as neutron stars in literature.</p> <p>MIST_OUTPUT.zip : MIST output file for mass estimations</p> <p>Readme : Description of MIST_output files.</p>
Seismic Signatures of the 12C(α, γ)16O Reaction Rate in White Dwarf Models with Overshooting
<p>This data set has all necessary files and scripts to reproduce figures 1-8 in our accepted manuscript.</p>
Data and Images for the paper "Evidence for a radiation belt around a brown dwarf" by Climent et al.
<p>Data used for the figures that appear in the main text and also in the supplementary materials in the paper titled "Evidence for a radiation belt around a brown dwarf" by Climent et al. published in Science.</p>
Figure 11 in Description of three new species of dwarf Glossogobius from New Guinea and northern Australia
Figure 11. – Live individual from Timika area of Glossogobius pumilus. Photo G. Allen.
Figure 9 in Description of three new species of dwarf Glossogobius from New Guinea and northern Australia
Figure 9. – Preserved holotype of Glossogobius pumilus, WAM P.27823-011, 32 mm SL male.
Figure 8 in Description of three new species of dwarf Glossogobius from New Guinea and northern Australia
Figure 8. – Live individual from type locality of Glossogobius nanus. Photo M. Hammer.
Ericaceous dwarf shrubs contribute a significant but drought-sensitive fraction of soil respiration in a boreal pine forest
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Data from: Diversity and composition of viral communities: coinfection of barley and cereal yellow dwarf viruses in California grasslands
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Data for: Molecular footprints of Quaternary climate fluctuations in the circumpolar tundra shrub dwarf birch
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Data from: Does warming by open-top chambers induce change in the root-associated fungal community of the arctic dwarf shrub Cassiope tetragona (Ericaceae)?
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Data from: Feeding strategies of the Pleistocene insular dwarf elephants <em>Palaeoloxodon falconeri</em> and <em>Palaeoloxodon mnaidriensis</em> from Sicily (Italy)
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Data from: Varietal and intrafamilial species diversity influence aphid and yellow dwarf virus pressure within mixtures of wheat and barley
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Numerical code and data for the stellar structure and dynamical instability analysis of generalised uncertainty white dwarfs
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Data from: Declining temperature and increasing moisture sensitivity of shrub growth in the Low-Arctic erect dwarf-shrub tundra of western Greenland
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Bimodal nesting season in Karoo dwarf tortoises (Chersobius boulengeri)
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Gut microbiota sequences of the long-tailed dwarf hamster (Cricetulus longicaudatus) using 16S rDNA
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The conservation genetics of Iris lacustris (Dwarf Lake Iris), a Great Lakes endemic
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Allen Brain Atlas
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International Brain Laboratory public data
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OpenNeuro
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