MESA_Bin_Gridivo://fai.kz/mesa_bin_6_4_0.02/q/qFesenkov Astrophysical InstituteVaidman, N. L.Izmailova, I.2026-04-21T09:23:43ZFAI 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/mesa_bin_6_4_0.02/q/q/infoSimulationResearchIsServedByFAI archives TAP servicehttps://dachs.fai.kz/mesa_bin_6_4_0.02/q/q/formhttps://dachs.fai.kz/mesa_bin_6_4_0.02/q/q/capabilitieshttps://dachs.fai.kz/mesa_bin_6_4_0.02/q/q/availabilityhttps://dachs.fai.kz/mesa_bin_6_4_0.02/q/q/tableMetadatahttps://dachs.fai.kz/tapFesenkov 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.1414componentEvolutionary component (STAR1 or STAR2)meta.id.partcharnullablem1Initial mass of primarysolMassphys.massintm2Initial mass of secondarysolMassphys.massintperiodInitial orbital perioddtime.perioddoublenullablezInitial metallicityphys.abund.Zdoublenullablemodel_numberEvolutionary step numberintstar_ageCurrent age of the staryrtime.agedoublenullablestar_massCurrent stellar masssolMassphys.massdoublenullablelog_abs_mdotlog10(abs(star_mdot))solMass/yrdoublenullablelog_dtlog10 time_step in yearsyrdoublenullablenum_zonesNumber of zones in the modelintmass_conv_coreMass coordinate of top of convective coresolMassdoublenullableconv_mx1_topTop of largest convective region (m/Mstar)doublenullableconv_mx1_botBottom of largest convective region (m/Mstar)doublenullableconv_mx2_topTop of 2nd largest convective region (m/Mstar)doublenullableconv_mx2_botBottom of 2nd largest convective region (m/Mstar)doublenullablemx1_topTop of largest mixed region (m/Mstar)doublenullablemx1_botBottom of largest mixed region (m/Mstar)doublenullablemx2_topTop of 2nd largest mixed region (m/Mstar)doublenullablemx2_botBottom of 2nd largest mixed region (m/Mstar)doublenullableepsnuc_m_1Start of 1st burning zonesolMassdoublenullableepsnuc_m_2Inner edge of 1st burning zone reaches limitsolMassdoublenullableepsnuc_m_3Outer edge of 1st burning zone drops below limitsolMassdoublenullableepsnuc_m_4End of 1st burning zonesolMassdoublenullableepsnuc_m_5Start of 2nd burning zonesolMassdoublenullableepsnuc_m_6Inner edge of 2nd burning zone reaches limitsolMassdoublenullableepsnuc_m_7Outer edge of 2nd burning zone drops below limitsolMassdoublenullableepsnuc_m_8End of 2nd burning zonesolMassdoublenullablehe_core_massHelium core masssolMassdoublenullableco_core_massCO core masssolMassdoublenullablefe_core_massIron core masssolMassdoublenullablelog_lhlog10 power_h_burndoublenullablelog_lhelog10 power_he_burndoublenullablelog_lzlog10 total burning power excluding LH and LHedoublenullablelog_lnuclog(LH + LHe + LZ)doublenullablelog_teffLog10 effective temperaturephys.temperature.effectivedoublenullableluminosityLuminosity in Lsun unitssolLumphys.luminositydoublenullablelog_lLog10 luminosity in Lsun unitsphys.luminositydoublenullablelog_rLog10 radius in Rsun unitsphys.size.radiusdoublenullablelog_gLog10 surface gravityphys.gravitydoublenullablegravitySurface gravitydoublenullablesurf_avg_omegaSurface average angular velocitydoublenullablesurf_avg_omega_div_omega_critSurface average omega divided by critical omegadoublenullablelog_center_tLog10 central temperaturedoublenullablelog_center_rhoLog10 central densitydoublenullablelog_center_pLog10 central pressuredoublenullablecenter_muCentral mean molecular weightdoublenullablecenter_yeCentral electron fractiondoublenullablecenter_h1Central H1 mass fractiondoublenullablecenter_he4Central He4 mass fractiondoublenullablecenter_c12Central C12 mass fractiondoublenullablecenter_o16Central O16 mass fractiondoublenullablesurface_c12Surface C12 mass fractiondoublenullablesurface_o16Surface O16 mass fractiondoublenullabletotal_mass_h1Total H1 masssolMassdoublenullabletotal_mass_he4Total He4 masssolMassdoublenullableppLog10 total luminosity for pp reaction categorydoublenullablecnoLog10 total luminosity for cno reaction categorydoublenullabletri_alphaLog10 total luminosity for tri-alpha reaction categorydoublenullablev_div_csound_surfVelocity divided by sound speed at surfacedoublenullablenum_retriesNumber of solver retriesintmodel_number_1Secondary model number trackerdoublenullableageBinary system ageyrdoublenullableperiod_daysCurrent binary perioddtime.perioddoublenullablebinary_separationOrbital separationsolRadphys.size;src.orbitaldoublenullablev_orb_1Orbital velocity of star 1km/sdoublenullablev_orb_2Orbital velocity of star 2km/sdoublenullablerl_1Roche lobe radius of star 1solRaddoublenullablerl_2Roche lobe radius of star 2solRaddoublenullablerl_relative_overflow_1Roche lobe relative overflow for star 1doublenullablerl_relative_overflow_2Roche lobe relative overflow for star 2doublenullablestar_1_massMass of star 1solMassdoublenullablestar_2_massMass of star 2solMassdoublenullablelg_mtransfer_rateLog10 mass transfer ratesolMass/yrdoublenullablelg_mstar_dot_1Log10 mass change rate star 1solMass/yrdoublenullablelg_mstar_dot_2Log10 mass change rate star 2solMass/yrdoublenullablelg_system_mdot_1Log10 system mass change rate 1solMass/yrdoublenullablelg_system_mdot_2Log10 system mass change rate 2solMass/yrdoublenullablelg_wind_mdot_1Log10 wind mass loss rate star 1solMass/yrdoublenullablelg_wind_mdot_2Log10 wind mass loss rate star 2solMass/yrdoublenullablefixed_xfer_fractionFixed transfer fractiondoublenullableeff_xfer_fractionEffective transfer fractiondoublenullablej_orbOrbital angular momentumdoublenullablejdotRate of change of orbital angular momentumdoublenullablejdot_mbJdot due to magnetic brakingdoublenullablejdot_grJdot due to gravitational radiationdoublenullablejdot_mlJdot due to mass lossdoublenullablejdot_lsJdot due to L-S couplingdoublenullablejdot_missing_windJdot due to missing winddoublenullableextra_jdotExtra Jdot termdoublenullabledonor_indexIndex of the donor stardoublenullablepoint_mass_indexIndex of the point mass companiondoublenullable