Neutron star-black hole mergers with a nuclear equation of state and neutrino cooling: Dependence in the binary parameters
Bibliographic record
Abstract
We present a first exploration of the results of neutron star-black hole mergers using black hole masses in the most likely range of $7{M}_{\ensuremath{\bigodot}}--10{M}_{\ensuremath{\bigodot}}$, a neutrino leakage scheme, and a modeling of the neutron star material through a finite-temperature nuclear-theory based equation of state. In the range of black hole spins in which the neutron star is tidally disrupted (${\ensuremath{\chi}}_{\mathrm{BH}}\ensuremath{\gtrsim}0.7$), we show that the merger consistently produces large amounts of cool ($T\ensuremath{\lesssim}1\text{ }\text{ }\mathrm{MeV}$), unbound, neutron-rich material (${M}_{\mathrm{ej}}\ensuremath{\sim}0.05{M}_{\ensuremath{\bigodot}}--0.20{M}_{\ensuremath{\bigodot}}$). A comparable amount of bound matter is initially divided between a hot disk (${T}_{\mathrm{max}}\ensuremath{\sim}15\text{ }\text{ }\mathrm{MeV}$) with typical neutrino luminosity of ${L}_{\ensuremath{\nu}}\ensuremath{\sim}{10}^{53}\text{ }\text{ }\mathrm{erg}/\mathrm{s}$, and a cooler tidal tail. After a short period of rapid protonization of the disk lasting $\ensuremath{\sim}10\text{ }\text{ }\mathrm{ms}$, the accretion disk cools down under the combined effects of the fall-back of cool material from the tail, continued accretion of the hottest material onto the black hole, and neutrino emission. As the temperature decreases, the disk progressively becomes more neutron rich, with dimmer neutrino emission. This cooling process should stop once the viscous heating in the disk (not included in our simulations) balances the cooling. These mergers of neutron star-black hole binaries with black hole masses of ${M}_{\mathrm{BH}}\ensuremath{\sim}7{M}_{\ensuremath{\bigodot}}--10{M}_{\ensuremath{\bigodot}}$, and black hole spins high enough for the neutron star to disrupt provide promising candidates for the production of short gamma-ray bursts, of bright infrared postmerger signals due to the radioactive decay of unbound material, and of large amounts of r-process nuclei.
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How this classification was reachedexpand
Full frame machine prediction
Teacher imitationNot calibrated prevalence, not ground truth. Human validation pending. The Gemma side is a direct model label for every work in the frame, read from the title-only record. The Codex side is a classifier learned from the 10,348 direct Codex labels and calibrated to design-weighted sample rates; fields without enough sample support carry no Codex call. Candidate is the union of the two sides; consensus is their intersection. These outputs are machine_predicted_unvalidated and are not human labels.
Distilled classifier scores by category (both heads)
| Category | Codex | Gemma |
|---|---|---|
| Metaresearch | 0.001 | 0.004 |
| Meta-epidemiology (narrow) | 0.001 | 0.000 |
| Meta-epidemiology (broad) | 0.001 | 0.001 |
| Bibliometrics | 0.000 | 0.001 |
| Science and technology studies | 0.001 | 0.001 |
| Scholarly communication | 0.001 | 0.001 |
| Open science | 0.001 | 0.001 |
| Research integrity | 0.001 | 0.001 |
| Insufficient payload (model declined to judge) | 0.002 | 0.000 |
Machine scores (provisional)
The two teacher heads of the student model, read on this work. A score orders the frame for review; it never asserts a category, and the validation status ships verbatim with every row.
Baseline scores from an immature model (maturity gate not passed, 7 training rounds). Scores rank; they never assert a category.
score_only:v0-immature-baseline · verbatim from the scoring run: score_only means the number may rank works, and no category label ships from itClassification
machine, unvalidatedMachine predicted; a candidate call from one source (direct Gemma or distilled Codex), not a consensus.
How this classification was reached, model by model and score by score, is at the end of the page under "How this classification was reached".