The neutron-star merger delay-time distribution, r-process "knees", and the metal budget of the Galaxy
Fuente:
arXiv
Saved in:
| Main Authors: | , |
|---|---|
| Format: | Preprint |
| Published: |
2024
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866913389878444032 |
|---|---|
| author | Maoz, Dan Nakar, Ehud |
| author_facet | Maoz, Dan Nakar, Ehud |
| contents | For a sample of 18 recycled millisecond pulsars (rMSPs) that are in double neutron star (DNS) systems, and 42 rMSPs that are not in DNS pairs, we analyze the distributions of the characteristic age, $τ_c$, and the time until merger of the double systems, $τ_{\rm gw}$. Based on the $τ_c$ distribution of non-DNS rMSPs, we argue that $τ_c$ is a reasonable estimator of true pulsar age and that rMSPs are active as pulsars for a long (~Hubble) time. Among the DNSs there is an excess of young systems (small $τ_c$) with short life expectancy (small $τ_{\rm gw}$) compared to model expectations for the distributions of $τ_c$ and $τ_{\rm gw}$ if, at birth, DNSs have a delay-time distribution (DTD) of the form $t^{-1}$ (expected generically for close binaries), or for that matter, from expectations from any single power-law DTD. A two-population DNS model solves the problem: the data are best fit by the combination of a "fast" population with DTD going as $t^{-1.9\pm0.4}$, and a "slow" population of DNSs, with DTD proportional to $t^{-1.1\pm0.15}$. The fast population can be equivalently represented by a DTD with an exponential cutoff beyond t~300 Myr. The fast population completely dominates, by a factor A~10-100, the numbers of DNSs that merge within a Hubble time, and that presumably lead to short gamma-ray bursts and kilonova explosions. With a simple, empirically based, chemical-evolution calculation, we show that the fast/steep kilonova DTD, convolved with the measured star-formation history of the Milky Way's thick-disk population, naturally reproduces the "knee" structure seen in abundance-ratio diagrams of thick-disk stars, for europium and two other r-process elements. As a corollary we show, based again solely on empirical input, that the Milky Way is nearly a "closed box" that has retained at least ~70-90% of the metals produced over the Galaxy's lifetime. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2406_08630 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The neutron-star merger delay-time distribution, r-process "knees", and the metal budget of the Galaxy Maoz, Dan Nakar, Ehud High Energy Astrophysical Phenomena For a sample of 18 recycled millisecond pulsars (rMSPs) that are in double neutron star (DNS) systems, and 42 rMSPs that are not in DNS pairs, we analyze the distributions of the characteristic age, $τ_c$, and the time until merger of the double systems, $τ_{\rm gw}$. Based on the $τ_c$ distribution of non-DNS rMSPs, we argue that $τ_c$ is a reasonable estimator of true pulsar age and that rMSPs are active as pulsars for a long (~Hubble) time. Among the DNSs there is an excess of young systems (small $τ_c$) with short life expectancy (small $τ_{\rm gw}$) compared to model expectations for the distributions of $τ_c$ and $τ_{\rm gw}$ if, at birth, DNSs have a delay-time distribution (DTD) of the form $t^{-1}$ (expected generically for close binaries), or for that matter, from expectations from any single power-law DTD. A two-population DNS model solves the problem: the data are best fit by the combination of a "fast" population with DTD going as $t^{-1.9\pm0.4}$, and a "slow" population of DNSs, with DTD proportional to $t^{-1.1\pm0.15}$. The fast population can be equivalently represented by a DTD with an exponential cutoff beyond t~300 Myr. The fast population completely dominates, by a factor A~10-100, the numbers of DNSs that merge within a Hubble time, and that presumably lead to short gamma-ray bursts and kilonova explosions. With a simple, empirically based, chemical-evolution calculation, we show that the fast/steep kilonova DTD, convolved with the measured star-formation history of the Milky Way's thick-disk population, naturally reproduces the "knee" structure seen in abundance-ratio diagrams of thick-disk stars, for europium and two other r-process elements. As a corollary we show, based again solely on empirical input, that the Milky Way is nearly a "closed box" that has retained at least ~70-90% of the metals produced over the Galaxy's lifetime. |
| title | The neutron-star merger delay-time distribution, r-process "knees", and the metal budget of the Galaxy |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2406.08630 |