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57 results for “theoretical model”
Confusion matrices for theoretical young stellar object models
<p>This is a data table supplementing the following publication: </p> <p><em><strong>A framework for modeling the evolution of young stellar objects </strong></em>(Richardson et al. 2025, accepted to ApJ).</p> <p>It contains a set of confusion matrices comparing the evolutionary stages and classes of radiative transfer YSO models selected by proximity to protostellar evolutionary tracks. Models are included in a matrix based on their correspondence to particular modeled accretion histories, zero-age stellar masses, ages, mass accretion efficiencies, and levels of detectability (defined using flux in the ALMA Band 6 wavelength range). Details on the construction and use of the table are contained in the accompanying README file, and more information about the matrices is contained in Section 4.2 of the companion paper.</p> <p>The YSO models populating these matrices are from Richardson et al. (2024); information on them is contained in the <a href="https://ui.adsabs.harvard.edu/abs/2024ApJ...961..188R/abstract" target="_blank" rel="noopener">companion work</a> and <a href="https://zenodo.org/records/10522816" target="_blank" rel="noopener">data release</a>.</p>
The SPOTS Models: A Grid of Theoretical Stellar Evolution Tracks and Isochrones For Testing The Effects of Starspots on Structure and Colors
<p><strong>The SPOTS Models: A Grid of Theoretical Stellar Evolution Tracks and Isochrones For Testing The Effects of Starspots on Structure and Colors</strong></p> <p>This repository contains the Stellar Parameters of Tracks with Starspots (SPOTS) grid of theoretical stellar evolutionary tracks and isochrones, presented in Somers, Pinsonneault, and Cao (2020, in prep). Our models were calculated with the Yale Rotating Evolution Code (e.g. van Saders & Pinsonneault, 2013, ApJ 776, 67), including updated which incorporate a treatment of surface starspots (Somers & Pinsonneault, 2015, ApJ 807, 174S). Modelling details can be found in these references. The purpose of this evolutionary suite is to provide the community with state-of-the-art predictions for the influence of starspots and magnetic activity on the structure of stars.</p> <p>The grid includes both isochrones and tracks. They can be downloaded individually from this repository, or in bulk by downloading the .zip files.</p> <p><strong>Isochrones (.isoc):</strong></p> <p>Each isochrone file contains a series of isochrones (stellar properties for a range of masses at fixed age) for ages between 1 Myrs and 4 Gyrs. Each file contains these isochrones for a different surface starspot covering fraction, given by the name of the file -- f000.isoc = 0% covering fraction, f017.isoc = 17% covering fraction, etc. Each isochrone contains several columns with different information, including,</p> <ol> <li>Fundamental properties: mass, age, luminosity, radius, logg, Teff, convective overturn timescale (TauCZ), lithium abundance relative to initial (Li/Li0).</li> <li>Starspot properties: Covering fraction (Fspot), ratio of spot temperature to ambient temperature (Xspot), the temperatures of hot and cool regions (T_hot, T_cool).</li> <li>Two-temperature colors, including Johnson BV, Cousins RI, 2MASS JHK, WISE W1, and Gaia G, BP, RP.</li> </ol> <p>Colors that fell outside of the calibrated range are listed as -99.0.</p> <p><strong>Tracks (.track):</strong></p> <p>We also include individual tracks for every combination of Fspot and Mass considered in the paper. Each .track file lists the mass and starspot covering fraction in the filename -- i.e. m055_f034.track is the model of mass 0.55Msun and with a 34% surface covering fraction. In addition to all the properties included in the isochrones, the track files also include:</p> <ol> <li>The total moment of interia of the model (total_I) and the moment of interia of the surface convection zone (CZ_I)</li> <li>The central and surface hydrogen abundances (X_cen, X_surf) and the surface metallicity (Z/X_surf)</li> <li>The deuterium abundance relative to initial (H2/H2_0)</li> </ol>
New calibrated models for the TRGB luminosity and a thorough analysis of theoretical uncertainties
<p>The files contain the grid models for TRGB stars based on <strong>Saltas & Tognelli, 2022, MNRAS, in press (arXiv: 2203.02499)</strong>. See the paper for details on the physics, and the attached readme file for a description of the structure of the attached files. If you use these data in your research please cite the above article. <br> </p>
Fig. 12 in Piggyback whorls: A new theoretical morphologic model reveals constructional linkages among morphological characters in ammonoids
Fig. 12. The same morphospaces as Fig. 11 showing the distribution of 115 species based on measurements.
Fig. 10 in Piggyback whorls: A new theoretical morphologic model reveals constructional linkages among morphological characters in ammonoids
Fig. 10. Measurements of the whorl expansion rate (Wc) and width of umbilicus (D). Note that c1 and c2 are defined as the distances from the coiling axis to the centers of the whorls. d1 and d2 are distances of umbilical seams from the coiling axis.
Fig. 8 in Piggyback whorls: A new theoretical morphologic model reveals constructional linkages among morphological characters in ammonoids
Fig. 8. Sketches of radial cross sections of ammonoids to illustrate various types of shell forms, such as planorbicone (A, B), serpenticone (C, D), oxycone (E), discocone (F), platycone (G, H), spherocone (I, J, K), and cadicone (L). A. Paraceltites elegans. B. Pseudoclymenia dillensis. C. Tropigastrites lahontanus. D. Pterolytoceras sp. E. Beloceras sp. F. Phylloceras consanguineum Gemmellaro. G. Craspedites sp. H. Tetragonites glabrus. I. Damesites sugata. J. Goniatites multiliratus Gordon. K. Latanarcestes sp. L. Cabrieroceras sp.
Fig. 9 in Piggyback whorls: A new theoretical morphologic model reveals constructional linkages among morphological characters in ammonoids
Fig. 9. Theoretical morphospace composed of ae and ar displaying several examples of computer−generated ammonoids that represent observed types illustrated in Fig. 8. A. e = 1.5 and r = 0.27. B. e = 1.75 and r = 0.34. C. e = 2.0 and r = 0.17. D. e = 2.3 and r = 0.05. E. e = 2.0 and r = 0.6. F. e = 1.7 and r = 0.27. G. e = 1.8 and r = 0.24. H. e = 2.3 and r = 0.21. I. e = 2.3 and r = 0.32. J. e = 1.95 and r = 0.28. K. e = 1.8 and r = 0.10. L. e = 1.6 and r = 0.8.
Fig. 7 in Piggyback whorls: A new theoretical morphologic model reveals constructional linkages among morphological characters in ammonoids
Fig. 7. Relationship between whorl perimeter (L) and square root of cross−sectional area of the whorl (A0.5) which varies with aand avalues. Dashed line i e r in each diagram represents the A0.5/Lcurve in the case of isometry of E and R (a= a= 1.0). A0.5/Lis generally small when ahas a large value. In each i e r i r model, e = 1.9 and r = 0.24.
Fig. 11 in Piggyback whorls: A new theoretical morphologic model reveals constructional linkages among morphological characters in ammonoids
Fig. 11. Results of computer simulations. A–D, theoretical morphospaces based on the piggyback whorls model composed of ae and ar showing values of shape parameters (S, A0.5/L, W, D) of a theoretical model corresponding to each combination of aand a. E, negative correlation between Wand S values i c e r c obtained from theoretical models. F, positive correlation between D and S. The values of S, A0.5/L, Wor D are exhibited by the size of the plots, and × indii c cates that a "forbidden" combinations of ae, ar, e, and r was employed in each simulation resulting in failure of defining form (A–D).
Fig. 6 in Piggyback whorls: A new theoretical morphologic model reveals constructional linkages among morphological characters in ammonoids
Fig. 6. Allometric growth of ammonoids. Computer models were generated with ae and ar values of 0.97, 1.0, and 1.3. Each diagram shows ontogenetic change in relationship between whorl height (H) and whorl breadth (B) that are standardized by the perimeter of the last whorl (Lmax). Dashed line in each diagram represents the B/H curve in the case of isometry of E and R (ae = ar = 1.0). Note that B/H decreases with growth in the case of ar = 0.97. In each model, e = 1.9 and r = 0.24.
Fig. 5 in Piggyback whorls: A new theoretical morphologic model reveals constructional linkages among morphological characters in ammonoids
Fig. 5. Spectrum of the computer−produced ammonoids with various values of E and R when each of them is fixed throughout growth.
Fig. 4 in Piggyback whorls: A new theoretical morphologic model reveals constructional linkages among morphological characters in ammonoids
Fig. 4. Schematic diagram of an ammonoid whorl section. The shape of the whorl (S) is represented by the closed curve illustrated here which is given by the parametric equations indicated above the diagram. Figures in the right show examples of hypothetical whorl shapes with systematically varying the S value.
Fig. 3 in Piggyback whorls: A new theoretical morphologic model reveals constructional linkages among morphological characters in ammonoids
Fig. 3. Different shapes of succeeding whorl (gray area) piling up on the hemispherical preceding whorl with same Li, l, and A values.
Fig. 2 in Piggyback whorls: A new theoretical morphologic model reveals constructional linkages among morphological characters in ammonoids
Fig. 2. Schematic figure of a cross section of the ammonoid shell showing how to define parameters of the piggyback whorls model. The enlarging rate of the whorl periphery (E) is defined as the ratio of the total perimeter of the newly added whorl section (Li) to that of preceding whorl (Li–1). The proportion of the dorsal whorl (R) is given by the ratio of the circumferential length along the dorsal wall (l) with respect to Li. The shape of the whorl section (S) is represented by the ratio of breadth (B) and height (H) of the whorl.
Fig. 1 in Piggyback whorls: A new theoretical morphologic model reveals constructional linkages among morphological characters in ammonoids
Fig. 1. Radial cross sections of ammonoids to illustrate allometric growth. A. Beloceras sp., Devonian; Erfoud, Morocco. B. Phylloceras consanguineum Gemmellaro, 1876, Jurassic; Sakaraha, Madagascar. C. Meekoceras gracilitatis White, 1879, Triassic; Crittenden Spring, Nevada. D. Girtyoceras meslerianum (Girty, 1909), Carboniferous; Jackforth Creek, Oklahoma.
Fig. 13 in Piggyback whorls: A new theoretical morphologic model reveals constructional linkages among morphological characters in ammonoids
Fig. 13. Results of same computer simulations as shown in Fig. 11 with an ornamented whorl shape. In order to produce an ornamented closed curve, the following parametric equations were used: x = 0.5Bcoso, y = 0.5H(sino + 0.3|sin4o|Q), where Q = H/B/5 if o Ṥ π, while Q = 5B/H if o> π. Note that simulated S values tend to be large as compared with Fig. 11F.
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>
Dataset for "Roles of surface forcing in the Southern Ocean temperature and salinity changes under increasing CO2: perspectives from model perturbation experiments and a theoretical framework"
<p>Reference: Kewei Lyu, Xuebin Zhang, John A. Church, Quran Wu, Russell Fiedler, and Fabio Boeira Dias (2022), Roles of surface forcing in the Southern Ocean temperature and salinity changes under increasing CO<sub>2</sub>: perspectives from model perturbation experiments and a theoretical framework, <em>Journal of Physical Oceanography</em>, <a href="https://doi.org/10.1175/JPO-D-22-0095.1">https://doi.org/10.1175/JPO-D-22-0095.1</a></p>
Hydrostatic models of theoretical planispiral ectocochleate cephalopods
<p>Zipped folder containing virtual models (in .STL format) of theoretical ectocochleate cephalopods (oxycone, serpenticone, sphaerocone, and morphospace center). There are four components of each model used in hydrostatic calculations: 1) shell, 2) chambers (camerae), 3) soft body, and 4) water displaced. Each near-endmember morphotype has two versions: 1) Body chamber lengths allowing neutral buoyancy with <em>Nautilus</em>-like chamber liquid (~12%), and 2) Body chamber lengths of the representative specimens used to build the models (<em>Sphenodiscus </em>for oxycone, <em>Dactylioceras </em>for serpenticone, and <em>Goniatites </em>for sphaerocone).</p>
Reviewed Articles from the study "Running away to sea: a theoretical model of anthropogenic factors contribution for microplastics transportation from rivers to the ocean".
<p>Table containing the papers reviewed from the study "Running away to sea: a theoretical model of anthropogenic factors contribution for microplastics transportation from rivers to the ocean". </p>
ScienceDex guides
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These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.