mesa_bin_6_4_002ivo://fai.kz/mesa_bin_6_4_0.02/q/mainFesenkov Astrophysical InstituteIzmailova, I.Vaidman, N. L.2026-04-16T12:18:11ZFAI NVO Team

Observatory 23, 050020 Almaty, Kazakhstan

vo@fai.kzaccretionroche-lobe-overflowbinary-starsstellar-evolutionstellar-evolutionary-modelshertzsprung-russell-diagram Grid of Close-Binary Evolution Models This dataset contains a grid of close-binary evolution models computed with the **MESA** (Modules for Experiments in Stellar Astrophysics) code, version `r24.08.1`. The primary objective is to investigate the dependence of binary interaction on the initial orbital period. **Model Configuration:** * **Donor Star (M1):** Fixed initial mass of 6.0 M_sun. The evolution is followed self-consistently. * **Companion (M2):** Represented as a point mass of 4.0 M_sun. * **Orbit:** Initially circular; the grid is constructed by varying the initial orbital period. **Physics and Assumptions:** * **Mass Transfer:** Implemented via the *Ritter prescription* for Roche-lobe overflow (RLOF). * **Efficiency:** Fully conservative mass transfer is assumed. * **Angular Momentum:** Includes losses due to gravitational radiation, magnetic braking, and systemic mass loss. * **Tides:** Tidal synchronization of the donor star is accounted for. * **Exclusions:** Wind mass transfer and irradiation effects are not included. **Termination Criteria:** Calculations are terminated if: 1. Roche-lobe overflow occurs at the very first timestep. 2. The system undergoes overflow through the outer Lagrangian point (L2). The setup is designed to isolate the role of the initial orbital period in determining the onset of mass transfer and the subsequent evolutionary regime.https://dachs.fai.kz/tableinfo/mesa_bin_6_4_002.mainSimulationResearchFesenkov Astrophysical InstituteMESAmesa_bin_6_4_002 Grid of Close-Binary Evolution Models This dataset contains a grid of close-binary evolution models computed with the **MESA** (Modules for Experiments in Stellar Astrophysics) code, version `r24.08.1`. The primary objective is to investigate the dependence of binary interaction on the initial orbital period. **Model Configuration:** * **Donor Star (M1):** Fixed initial mass of 6.0 M_sun. The evolution is followed self-consistently. * **Companion (M2):** Represented as a point mass of 4.0 M_sun. * **Orbit:** Initially circular; the grid is constructed by varying the initial orbital period. **Physics and Assumptions:** * **Mass Transfer:** Implemented via the *Ritter prescription* for Roche-lobe overflow (RLOF). * **Efficiency:** Fully conservative mass transfer is assumed. * **Angular Momentum:** Includes losses due to gravitational radiation, magnetic braking, and systemic mass loss. * **Tides:** Tidal synchronization of the donor star is accounted for. * **Exclusions:** Wind mass transfer and irradiation effects are not included. **Termination Criteria:** Calculations are terminated if: 1. Roche-lobe overflow occurs at the very first timestep. 2. The system undergoes overflow through the outer Lagrangian point (L2). The setup is designed to isolate the role of the initial orbital period in determining the onset of mass transfer and the subsequent evolutionary regime.mesa_bin_6_4_002.main Grid of Close-Binary Evolution Models This dataset contains a grid of close-binary evolution models computed with the **MESA** (Modules for Experiments in Stellar Astrophysics) code, version `r24.08.1`. The primary objective is to investigate the dependence of binary interaction on the initial orbital period. **Model Configuration:** * **Donor Star (M1):** Fixed initial mass of 6.0 M_sun. The evolution is followed self-consistently. * **Companion (M2):** Represented as a point mass of 4.0 M_sun. * **Orbit:** Initially circular; the grid is constructed by varying the initial orbital period. **Physics and Assumptions:** * **Mass Transfer:** Implemented via the *Ritter prescription* for Roche-lobe overflow (RLOF). * **Efficiency:** Fully conservative mass transfer is assumed. * **Angular Momentum:** Includes losses due to gravitational radiation, magnetic braking, and systemic mass loss. * **Tides:** Tidal synchronization of the donor star is accounted for. * **Exclusions:** Wind mass transfer and irradiation effects are not included. **Termination Criteria:** Calculations are terminated if: 1. Roche-lobe overflow occurs at the very first timestep. 2. The system undergoes overflow through the outer Lagrangian point (L2). The setup is designed to isolate the role of the initial orbital period in determining the onset of mass transfer and the subsequent evolutionary regime.14accrefDownload FITS modelmeta.ref.urlcharindexednullableownerOwner of the datacharnullableembargoDate the data will become/became publicyrcharnullablemimeMIME type of the file servedmeta.code.mimeAccess.FormatcharnullableaccsizeSize of the data in bytesbyteVOX:Image_FileSizeAccess.SizelongnullablepreviewfloatnullablenameModel identifier (e.g., p_0.90)meta.id;meta.maincharnullablem1Fixed initial mass of the donor starsolMassphys.massfloatnullablem2Fixed initial mass of the point-mass companionsolMassphys.massfloatnullablepInitial orbital perioddtime.periodfloatnullablezFixed initial metallicityphys.abund.Zfloatnullable