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5 results for “Cool Dwarfs”
Theoretical Models of Ultra-Cool Objects (Brown Dwarfs and Free-Floating Planets) Including Water Latent Heat Effect: Thermal Structure, Spectra, and Photometry
<p><strong>OVERVIEW</strong><br> Data presented here are from the work of Tang et al. (2021), which present a one-dimensional (vertical) atmospheric structure model for ultra-cool objects<br> that includes moist adiabatic convection (water latent heat release effect).<br> Model grids across a range of effective temperatures (350, 300, 250, 200 K), metallicities ([M/H] of 0.0, 0.5, 0.7, 1.5),<br> and gravities (logg of 4.0, 4.5, 4.7, 5.0) that mimic the atmosphere condition of Y-class brown dwarf and Free-Floating Planets.</p> <p><strong>ATMOSPHERIC THERMAL STRUCTURE</strong><br> The pressure-temperature profile are saved under the ./pT_profiles/, which have two folders:</p> <ol> <li>pT_profile_dry_adiabat: for dry adiabatic treatment.</li> <li>pT_profile_moist_adiabat: for moist adiabatic treatment.</li> </ol> <p>File name of each compressed files gives the effective temperature (Teff, in Kelvin), gravity (in MKS), and metallicity (in [M/H]) information as for example:<br> t200g100nc_m0.0.cmp.gz --> Teff of 200K, gravity as 100 m/s2, and [M/H]=0.0.</p> <p>The table formate of the pressure-temperature profile, i.e., the .cmp files, is made to work with the [<a href="https://natashabatalha.github.io/picaso/">PICASO software</a>](https://natashabatalha.github.io/picaso/).<br> Each .cmp file contains</p> <ul> <li>Column 01 (x) : atmosphere pressure level</li> <li>Column 02 (pressure) : atmosphere pressure in bar</li> <li>Column 03 (DEN) : atmosphere density in cm^{-3}</li> <li>Column 04 (temperature) : atmosphere temperature in kelvin</li> <li>Column 05-14 : molecule mixing ratios for H2, He, CH4, H2O, NH3, CO, PH3, H2S, N2, CO2</li> <li>Column 15 (MU) : mean molecular weight in grams/mole</li> </ul> <p><strong>SPECTRA</strong><br> Model spectra are saved under the ./spectra/ with wavelength ranging from 1 to 30 micron.<br> File name of each compressed file gives the effective temperature (Teff, in Kelvin), gravity (in MKS), metallicity (in [M/H]), adiabatic treatment, and<br> the resolving power information as for example:<br> sp_t200_g100_m0.0_dry_R3000.csv.gz --> Teff of 200K, gravity as 100 m/s2, [M/H]=0.0, with dry adiabatic treatment, and R=3000.<br> Each spetrum .cv file contains two columns:</p> <ul> <li>Column 01 wavelength [micron]</li> <li>Column 02 Flux [W/m2/micron], the spectral fluxes are given at the top of the atmosphere, taken to be 1 Jupiter radius.</li> </ul> <p><strong>PHOTOMETRY</strong><br> Photometry data derived from the spectra at the top of the atmosphere (assuming one Jupiter radius) are given in the syn_photometry.csv.<br> Photometry filters are from the Mauna Kea Observatory (MKO) photometry system, the Wide-field Infrared Survey Explorer (WISE), and the<br> Spitzer Space Telescope. Filter profiles and Vega magnitude zero points are from the [<a href="http://svo2.cab.inta-csic.es/theory/fps/">SVO Filter Profile Service</a>](http://svo2.cab.inta-csic.es/theory/fps/)</p> <ul> <li>Column 01 (gravity) , gravity in MKS</li> <li>Column 02 (teff) , effective temperature in Kelvin</li> <li>Column 03 ([M/H]) , metallicity</li> <li>Column 04-12 , photometry magnitude for IRAC36, IRAC45, W1, W2, GiminiM, MKO_J, MKO_H, MKO_K, MKO_Lp all in Vega system.</li> <li>Column 13 (adiabatic), adiabatic treatment; D: dry adiabatic, M: moist adiabatic</li> </ul> <p><strong>CREDITS</strong><br> Please cite Tang et al. (2021, Astrophysical Journal, in press.)<br> [<a href="https://ui.adsabs.harvard.edu/abs/2021arXiv210507000T/abstract">ADS link</a>](https://ui.adsabs.harvard.edu/abs/2021arXiv210507000T/abstract) if you used data here in your research.</p>
Data from: Macrobenthic assemblage structure in a cool-temperate intertidal dwarf-eelgrass bed in comparison to those in lower latitudes.
The evolution and ecology of latitudinal patterns in marine macrofaunal biodiversity and assemblage structure are contentious. With the aim of investigating the occurrence of such patterns in intertidal dwarf-eelgrass beds (Nanozostera spp.), those at cool-temperate Scolt Head Island, UK (latitude 52°N), were examined and compared to equivalent systems in warm-temperate Knysna, South Africa (34°S), and subtropical Moreton Bay, Australia (27°S); systems that had earlier been examined using identical methodology. The Scolt Head bed supported the highest faunal density (mean 6,568 0.1m-2), lowest observed and estimated species richness (32 and 33 spp respectively), lowest species diversity (Simpson's Index 0.34), highest mean Constancy Index (23.0), lowest proportion of total numbers contributed by singletons or doubletons (0.06%), largest Berger-Parker Dominance (0.81), and least degree of variability between component samples. The beds at Knysna were intermediate between those at Scolt Head and Moreton Bay in all those respects, as well as in nature and composition of the fauna. Similar dwarf-eelgrass beds at Arcachon, France, likewise appear intermediate between those of Scolt Head and Knysna. Community variance in all three regions was greatest at the smallest spatial scale of ≤1 m, at which scale two of the three also displayed randomly organized faunal assemblages, although this changed to non-random at larger spatial scales. Assemblages were deterministically structured at all spatial scales at Knysna. A consistent series of changes in structural characteristics of macrofaunal dwarf-eelgrass assemblages therefore occurred along the latitudinal sequence of Scolt Head (530): Arcachon (450): Knysna (340): Moreton Bay (270). Community assembly patterns did not change with latitude, however, but did so with spatial scale in two of the three regions.
A Uniform Retrieval Analysis of Ultra-cool Dwarfs. IV. A Statistical Census from 50 Late-T Dwarfs
<p>Posterior distributions for all model runs of A Uniform Retrieval Analysis of Ultra-cool Dwarfs. IV. A Statistical Census from 50 Late-T Dwarfs</p> <p>To view, simply download the file and extract the zipfile.</p> <p>Directory structure is as follows:</p> <p><strong>BEST_FIT_SPECTRA</strong>: Figures for best-fit model spectra for all 50 objects.</p> <p><strong>CLOUD_OPTICAL_DEPTH: </strong>Derived tau_cloud optical depth posteriors from the cloud model.</p> <p><strong>CORNER_PLOTS</strong>: Corner plots for all 50 objects.</p> <p><strong>TEMPERATURE_PROFILES</strong>: Retrieved temperature profiles for all 50 objects. Overlaid are relevant condensation curves (legend found in the text of the publication).</p>
Data from: Macrobenthic assemblage structure in a cool-temperate intertidal dwarf-eelgrass bed in comparison to those in lower latitudes.
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The importance of Urca-process cooling in accreting ONe white dwarfs
<p>MESA inlists associated with <a href="http://adsabs.harvard.edu/abs/2017MNRAS.472.3390S">Schwab et al. (2017)</a>. MESA version r9793.</p>
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