Modelling Double Neutron Stars: Radio and Gravitational Waves. (arXiv:1912.02415v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Chattopadhyay_D/0/1/0/all/0/1">Debatri Chattopadhyay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stevenson_S/0/1/0/all/0/1">Simon Stevenson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hurley_J/0/1/0/all/0/1">Jarrod R. Hurley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rossi_L/0/1/0/all/0/1">Luca J. Rossi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Flynn_C/0/1/0/all/0/1">Chris Flynn</a>
We have implemented prescriptions for modelling pulsars in the rapid binary
population synthesis code COMPAS. We perform a detailed analysis of the double
neutron star (DNS) population, accounting for radio survey selection effects.
The surface magnetic field decay timescale (${approx}1000$,Myr) and mass
scale (${approx}0.02$,M$_odot$) are the dominant uncertainties in our model.
Mass accretion during common envelope evolution plays a non-trivial role in
recycling pulsars. We find a best-fit model that is in broad agreement with the
observed Galactic DNS population. Though the pulsar parameters (period and
period derivative) are strongly biased by radio selection effects, the observed
orbital parameters (orbital period and eccentricity) closely represent the
intrinsic distributions. The number of radio observable DNSs in the Milky Way
at present is $approx$,2500 in our model, only $approx$,10% of the
predicted total number of DNSs in the galaxy. Using our model calibrated to the
Galactic DNS population, we make predictions for DNS mergers observed in
gravitational waves. The median DNS chirp mass is 1.14,M$_mathrm{odot}$ and
$approx$40% of DNSs have a chirp mass $geq$ 1.2,M$_mathrm{odot}$. The
expected effective spin $chi_mathrm{eff}$ for isolated DNSs is $lesssim$0.03
from our model. We predict that $approx$34% of the current Galactic isolated
DNSs will merge within a Hubble time, and have a median total mass of
2.7,M$_mathrm{odot}$. Finally, we discuss implications for fast radio bursts
and post-merger remnant gravitational-waves.
We have implemented prescriptions for modelling pulsars in the rapid binary
population synthesis code COMPAS. We perform a detailed analysis of the double
neutron star (DNS) population, accounting for radio survey selection effects.
The surface magnetic field decay timescale (${approx}1000$,Myr) and mass
scale (${approx}0.02$,M$_odot$) are the dominant uncertainties in our model.
Mass accretion during common envelope evolution plays a non-trivial role in
recycling pulsars. We find a best-fit model that is in broad agreement with the
observed Galactic DNS population. Though the pulsar parameters (period and
period derivative) are strongly biased by radio selection effects, the observed
orbital parameters (orbital period and eccentricity) closely represent the
intrinsic distributions. The number of radio observable DNSs in the Milky Way
at present is $approx$,2500 in our model, only $approx$,10% of the
predicted total number of DNSs in the galaxy. Using our model calibrated to the
Galactic DNS population, we make predictions for DNS mergers observed in
gravitational waves. The median DNS chirp mass is 1.14,M$_mathrm{odot}$ and
$approx$40% of DNSs have a chirp mass $geq$ 1.2,M$_mathrm{odot}$. The
expected effective spin $chi_mathrm{eff}$ for isolated DNSs is $lesssim$0.03
from our model. We predict that $approx$34% of the current Galactic isolated
DNSs will merge within a Hubble time, and have a median total mass of
2.7,M$_mathrm{odot}$. Finally, we discuss implications for fast radio bursts
and post-merger remnant gravitational-waves.
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