posydon.binary_evol.SN
posydon.binary_evol.SN.profile_collapse
Collapse the profile of a star object into a BH.
This script is based on the physics explained in Appendix D of Bavera+2020.
- posydon.binary_evol.SN.profile_collapse.compute_isco_properties(a, m_BH)[source]
Compute the BH innermost stable circular orbit (ISCO) parameters.
- posydon.binary_evol.SN.profile_collapse.do_core_collapse_BH(star, mass_collapsing, mass_central_BH=2.51, neutrino_mass_loss=None, max_neutrino_mass_loss=0.5, verbose=False)[source]
Do the core collapse of a star object with MESA profile provided.
- Parameters:
star (object) – Star object of a collapsing star containing the MESA profile.
mass_collapsing (float) – Remnant barionic mass in M_sun collapsing to form the BH. This is the mass left to collapse after applying a supernova prescriptions, see e.g. rapid and delayed mechanisms of Fryer et al. (2012).
mass_central_BH (float) – Mass of the central stellar layers (in M_sun) collasping directly to form a proto BH.
neutrino_mass_loss (float) – Mass (in M_sun) lost thorugh neutrinos in the formation of the central BH.
max_neutrino_mass_loss (float) – Maximum mass (in M_sun) lost thorugh neutrinos.
verbose (bool) – If True, it prints some informations.
- Returns:
M_BH_total (float) – Mass of the final BH in M_sun.
a_BH_total (float) – Dimensionless spin of the final BH.
M_BH_array (array floats) – BH mass evelution in g.
a_BH_array (array floats) – Dimensionless spin evolution.
J_accreted_array (array floats) – Angular momentum accreted from a given shell by the BH in CGS units.
J_total_array (array floats) – Total angular momentum in accreted shells plus BH’s initial angular momentum in CGS units.
J_disk_shell_array (array floats) – Angular momentum accreted from the shell’s part collapsing to form a disk in CGS units.
radiation_eff_array (array floats) – Fraction of accretion disk radiated away, this is one minus accretion efficiency.
r_isco_array (array floats) – Radius of the innermost stable circular orbit in cm.
j_isco_array (array floats) – Specific angular momentum at the innermost stable circular orbit in CGS.
M_direct_collapse_array (array floats) – Cumulative mass accreted through direct collapse in g.
M_disk_array (array floats) – Cumulative mass accreted thorugh the disk in g.
dm_direct_array (array floats) – Shell’s mass accreted through direct collapse in g.
dm_disk_array (array floats) – Shell’s mass accreted thorugh the disk in g.
j_shell_array (array floats) – Shell’s specific angular momentum in CGS.
M_total_array (array floats) – Cumulative mass of shells and initial BH in g.
a_star_array (array floats) – Dimensionless spin parameter of the star.
- posydon.binary_evol.SN.profile_collapse.get_initial_BH_properties(star, mass_collapsing, mass_central_BH, neutrino_mass_loss, max_neutrino_mass_loss, verbose)[source]
Collapse directly the center of the star and return useful quantities.
- Parameters:
star (object) – Star object of a collapsing star containing the MESA profile.
mass_collapsing (float) – Remnant barionic mass in M_sun collapsing to form the BH. This is the mass left to collapse after applying a supernova prescriptions, see e.g., rapid and delayed mechanisms of Fryer et al. (2012).
mass_central_BH (float) – Mass of the central stellar layers (in M_sun) collasping directly to form a proto BH.
neutrino_mass_loss (float) – Mass (in M_sun) lost through neutrinos in the formation of the central BH.
max_neutrino_mass_loss (float) – Maximum mass (in M_sun) lost thorugh neutrinos.
verbose (bool) – If True, it prints some informations.
- Returns:
mass_initial_BH (float) – Mass of the initial BH in units of g.
a_initial_BH (float) – Dimensionless spin of the initial BH.
J_initial_BH (float) – Angular momentum of the initial BH in g*cm^2/s.
angular_frequency_i (array floats) – Shell’s angular frequencies in s^-1 collapsing onto the initially-formed BH.
enclosed_mass_i (array floats) – Shell’s enclosed masses in g collapsing onto the initially formed BH.
radius_i (array floats) – Shell’s radii in cm collapsing onto the initially formed BH.
density_i (array floats) – Shell’s densities in g/cm^3 collapsing onto the initially formed BH.
dm_i (array floats) – Shell’s masses in g collapsing onto the initially formed BH.
dm_i (array floats) – Shell’s width in cm collapsing onto the initially formed BH.
posydon.binary_evol.SN.step_SN
Supernova step.
This step models the end of life of stars by being applied to a binary object and verifying its state. It performs the collapse prescription used to initialize the step in the respective star. Depending on the C and He cores the final state of the star is determined, from the formation of white dwarfs to electron-capture supernova, Fe core-collapse supernova, pair pulsation supernova and pair instability supernova.
- class posydon.binary_evol.SN.step_SN.Couch20_corecollapse(turbulence_strength, path_engine_dataset, verbose)[source]
Bases:
objectCompute SN final remnant mass, fallback fraction and stellar state.
This considers the nearest neighboor of the He core mass of the star, previous to the collapse. Considering a set of data for which the He core mass of the compact object progenitors before the collapse, the final remnant mass and final stellar state of the compact object is known.
- Parameters:
- Returns:
m_rem (double) – Remnant mass of the compact object in M_sun.
f_fb (double) – Fallback mass of the compact object in M_sun.
state (string) – Finall state of the stellar remnant after the supernova.
Notes
We need [2] data for their cores.
References
[1] (1,2)Couch, S. M., Warren, M. L., & O’Connor, E. P. 2020, ApJ, 890, 127 Simulating Turbulence-aided Neutrino-driven Core-collapse Supernova Explosions in One Dimension
[2]Sukhbold, T., Ertl, T., Woosley, S. E., Brown, J. M., & Janka, H. T. (2016). Core-collapse supernovae from 9 to 120 solar masses based on neutrino-powered explosions. The Astrophysical Journal, 821(1), 38.
Initialize a Couch20_corecollapse instance.
- class posydon.binary_evol.SN.step_SN.StepSN(**kwargs)[source]
Bases:
objectThe supernova step in POSYDON.
- Keyword Arguments:
mechanism (str) –
Mechanism to perform the core-collapse on the star object and predict the supernova remnant outcome. Available options are:
’Fryer+12-rapid’ : The rapid supernova-engine described in [1]
’Fryer+12-delayed’ : The delayed supernova-engine described in [1]
’direct’ : The pre-supernova mass of the starr is collapsed into the
remnant baryonic mass.
’direct_he_core’ : The pre-supernova He core mass of the starr is
collapsed into the remnant baryonic mass.
’Sukhbold+16-engine’ : Uses the results from [2]
to describe the collapse of the star.
’Patton&Sukhbold20-engine’: Uses the results from [5]
to describe the collapse of the star.
’Couch+20-engine’: Uses the results from [6]
to describe the collapse of the star.
engine (str) –
Engine used for supernova remnanrt outcome propierties for the Sukhbold+16-engineand and Patton&Sukhbold20-engine mechanisms. Available options:
’N20’
PISN (str) –
Prescrition to take on the pair-instability supernova. Avialable options:
’Marchant+19’ : Descripes the pair-instability supernova as [3].
mass_central_BH (double) – Central mass collapsed automatically on black-holes formed by direct collapse.
max_neutrino_mass_loss (double) – Neutrino mass loss during the collapse of the proto neutron-star.
kick (bool) – If True, the kick velocities are computed corresponding to the supernova event, else no kicks are taking into account for any supernova outcome.
kick_normalisation (str) – Renormalise the kick by: ‘one_minus_fallback’ : (1-f_fb) ‘one_over_mass’ : 1.4/m_BH ‘zero’ : 0. ‘one’ : 1. ‘NS_one_minus_fallback_BH_one’: 1 for BH, (1-f_fb) for NS
ECSN (str) –
Prescription to determine the production of an electron-capture supernova. Avialable options:
’Tauris+15’: Determines the electron capture supernova in terms
of the CO core mass at pre-supernova, taking the limits from [4].
sigma_kick_CCSN_NS (double) – Standard deviation for a Maxwellian distribution to compute the kick velocities from NSs formed by Fe core-collapse supernova.
sigma_kick_CCSN_BH (double) – Standard deviation for a Maxwellian distribution to compute the kick velocities from BHs formed by Fe core-collapse supernova.
sigma_kick_ECSN (double) – Standard deviation for a Maxwellian distribution to compute the kick velocities from compact-object formed by electron-capture supernova.
max_NS_mass (double) – Maximum neutron-star mass.
use_interp_values (bool) – The outcome of core collpase was interpolated from a post processed MESA grid and stored in the star object in the mesa_step or detached_step (default). This option supports only default assumptions for all core collase mechanism.
use_profiles (bool) – Perfrome the core collpase given a MESA profile. To use this option a MESA profile must be stored in the star object which is provided by nearest neighbor interpolation in the mesa_step or (TODO) interpolated in the detached_step.
use_core_masses (bool) – This option uses the core masses at carbon depletion to determine the core collapse outcoume (classical population sythesis threatment).
approx_at_he_depletion (bool) – This option is relevant only for the mechanism Patton&Sukhbold20-engine. In case the core masses at he-depletion are not present in the star object, compute them from the history, else (approximation=True) approximate it from the core masses at C depletion.
verbose (bool) – If True, the messages will be prited in the console.
References
[1] (1,2)Fryer, C. L., Belczynski, K., Wiktorowicz, G., Dominik, M., Kalogera, V., & Holz, D. E. (2012). Compact remnant mass function: dependence on the explosion mechanism and metallicity. The Astrophysical Journal, 749(1), 91.
[2]Sukhbold, T., Ertl, T., Woosley, S. E., Brown, J. M., & Janka, H. T. (2016). Core-collapse supernovae from 9 to 120 solar masses based on neutrino-powered explosions. The Astrophysical Journal, 821(1), 38.
[3]Marchant, P., Renzo, M., Farmer, R., Pappas, K. M., Taam, R. E., De Mink, S. E., & Kalogera, V. (2019). Pulsational pair-instability supernovae in very close binaries. The Astrophysical Journal, 882(1), 36.
[4]Tauris, T. M., Langer, N., & Podsiadlowski, P. (2015). Ultra-stripped supernovae: progenitors and fate. Monthly Notices of the Royal Astronomical Society, 451(2), 2123-2144.
[5]Patton, R. A. & Sukhbold, T. 2020, MNRAS, 499, 2803. Towards a realistic explosion landscape for binary population synthesis
[6]Couch, S. M., Warren, M. L., & O’Connor, E. P. 2020, ApJ, 890, 127. Simulating Turbulence-aided Neutrino-driven Core-collapse Supernova Explosions in One Dimension
Initialize a StepSN instance.
- C_abundance_for_H_stars(CO_core_mass)[source]
Get the C abundance for a H-star given it’s CO core mass.
- C_abundance_for_He_stars(CO_core_mass)[source]
Get the C abundance for a He-star given it’s CO core mass.
- PISN_prescription(star)[source]
Compute baryonic remnant mass for the PPISN and PISN prescription.
- Parameters:
star (object) – Star object containing the star properties.
- Returns:
m_PISN – Maximum stellar mass in M_sun after the PPISN/PISN prescription.
- Return type:
double
- Patton20_corecollapse(star, engine, conserve_hydrogen_envelope=False)[source]
Compute supernova final remnant mass and fallback fraction.
It uses the results from [1]. The prediction for the core-collapse outcome is performed using the C core mass and its C abundance. The criterion by [2] is used to determine the final outcome.
- Parameters:
star (obj) – Star object of a collapsing star containing the MESA profile.
- Returns:
m_rem (double) – Remnant mass of the compact object in M_sun.
f_fb (double) – Fallback mass of the compact object in M_sun.
References
- check_SN_type(m_core, m_He_core, m_star)[source]
Get the remnant mass, fallback frac., state & SN type of the SN.
- collapse_star(star)[source]
Collapse the star object into a compact object.
This routine supports three options: 1. use_interp_values : True
The outcome of core collpase was interpolated from a post processed MESA grid and stored in the star object in the mesa_step or detached_step (default). This option supports only default assumptions for all core collase mechanism.
use_profiles : False Perfrome the core collpase given a MESA profile. To use this option a MESA profile must be stored in the star object which is provided by nearest neighbor interpolation in the mesa_step or (TODO) interpolated in the detached_step.
use_core_masses : False This option uses the core masses at carbon depletion to determine the core collapse outcoume (classical population sythesis threatment).
- Parameters:
star (object) – Star object containing the star properties.
- Returns:
m_rem (double) – Remnant mass of the compact object in M_sun. This quantity accounts for the mass loss thorugh neutrino.
state (string) – New state of the star object.
- compute_m_rembar(star, m_PISN)[source]
Compute supernova remnant barionic mass.
We follow the selected electron-capture and core-collapse mechanisms to get the remnant baryonic mass.
- Parameters:
star (object) – Star object containing the star properties.
m_PISN (double) – Maximum stellar mass in M_sun after the PPISN/PISN prescription.
- Returns:
m_rembar (double) – Barioninc mass of the remnant after the supernova in M_sun. This quantity does NOT take into account any neutrino lost, this will be taken into account in collapse_star().
f_fb (double) – Mass fraction falling back onto the compact object created in the supernova. The maximum value is 1 and means that all the barionic mass is collapsing to form the compact object.
state (string) – Finall state of the stellar remnant after the supernova.
- generate_kick(star, sigma)[source]
Draw a kick from a Maxwellian distribution.
We follow Hobbs G., Lorimer D. R., Lyne A. G., Kramer M., 2005, MNRAS, 360, 974 and choose sigma = 265 km/s
We rescale the kicks by 1 - f_fb as in Eq. 21 of Fryer, C. L., Belczynski, K., Wiktorowicz, G., Dominik, M., Kalogera, V., & Holz, D. E. (2012), ApJ, 749(1), 91.
- Parameters:
star (object) – Star object containing the star properties.
- Returns:
Vkick – Natal orbital kick in km/s.
- Return type:
double
- get_CO_core_params(star, approximation=False)[source]
Get the CO core mass and C abundance at the pre-supernova phase.
If the two parameters are available in the star’s profile, perform the Patton&Sukhbold,20 core-collapse.
If the CO core mass is available but not the C abundance then the latter is computed from the formulas at Patton&Sukhbold,20.
- Parameters:
- starobj
Star object of a collapsing star containing the MESA profile.
- approximationbool
In case the core masses at he-depletion are not present in the star object, compute them from the history default behaviour, else (approximation=True) approximate it from the core masses at C depletion.
- Returns:
- CO_core_massfloat
Mass of the CO core at He depletion == C core ignition.
- C_core_abundancefloat
C abundance of the CO core He depletion == C core ignition.
- orbital_kick(binary)[source]
Do the orbital kick.
This function computes the supernova step of the binary object [1], [2]. It checks which binary_state reached the core collapse flag, either CC1 or CC2, and runs the step accordingly updating the binary object.
Geometry: We work in a right-handed coordinate system. The collapsing helium star, here M_he_star, lies on the origin. The companion, here M_companion, lies on the negative X axis at rest. The relative velocity of the M_he_star with respect to M_companion lies in the X-Y plane, with vY>0. The orbital angular momentum vector is in Z direction, which completes the right-handed coordinate system.
- psi:
The angle in the orbital plane between the X axis and the pre-core collapse relative velocity. (psi = pi/2 points in Y direction)
- theta :
The polar angle between the kick velocity and the pre-core collapse relative velocity of the M_he_star with respect to M_companion.
- phi :
The corresponding azimuthal angle such that phi=0 is on the Z axis.
- tilt :
The angle between pre- and post- supernova orbital angular momentum vectors.
- Parameters:
binary (object) – Binary object containing the binary properties and the two star objects.
References
- class posydon.binary_evol.SN.step_SN.Sukhbold16_corecollapse(engine, path_engine_dataset, verbose)[source]
Bases:
objectCompute supernova final remnant mass, fallback fraction and CO type.
This consider the nearest neighboor of the He core mass of the star, previous to the collapse. Considering a set of data for which the He core mass of the compact object projenitos previous the collapse, the final remnant mass and final stellar state of the compact object is known.
- Parameters:
- Returns:
m_rem (double) – Remnant mass of the compact object in M_sun.
f_fb (double) – Fallback mass of the compact object in M_sun.
state (string) – Finall state of the stellar remnant after the supernova.
References
Initialize a Sukhbold16_corecollapse instance.