PULSAR J0453+1559: A DOUBLE NEUTRON STAR SYSTEM WITH A LARGE MASS ASYMMETRY

By J. Martinez, K. Stovall, P. Freire, Julia Deneva, Fredrick A. Jenet, Maura Mclaughlin, M. Bagchi, S. Bates, A. Ridolfi. 2015

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To understand the nature of supernovae and neutron star (NS) formation, as well as binary stellar evolution and their interactions, it is important to probe the distribution of NS masses. Until now, all double NS (DNS) systems have been measured as having a mass ratio close to unity (q ≥ 0.91). Here, we report the measurement of the individual masses of the 4.07-day binary pulsar J0453+1559 from measurements of the rate of advance of periastron and Shapiro delay: the mass of the pulsar is Mp = 1.559 ± 0.005 M⊙ and that of its companion is M c = 1.174 ± 0.004 ?> M⊙; q = 0.75. If this companion is also an NS, as indicated by the orbital eccentricity of the system (e = 0.11), then its mass is the smallest precisely measured for any such object. The pulsar has a spin period of 45.7 ms and a spin period derivative of P ˙ ?> = (1.8616±0.0007)×10−19 s s−1; from these, we derive a characteristic age of ∼ 4.1×109 years and a magnetic field of ∼ 2.9×109 G, i.e., this pulsar was mildly recycled by the accretion of matter from the progenitor of the companion star. This suggests that it was formed with (very approximately) its current mass. Thus, NSs form with a wide range of masses, which is important for understanding their formation in supernovae. It is also important for the search for gravitational waves released during an NS–NS merger: it is now evident that we should not assume that all DNS systems are symmetric.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/e9e93f21bae1a1ca42fa25953a4849a7aa385023

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Citations in the corpus

The overarching framework of core-collapse supernova explosions as revealed by 3D fornax simulations (2019, background): “…calculations of Radice et al. (2017) concerning the sources from ∼8−8.8 M progenitors of the lowest-mass pulsars (down to ∼1.17 M gravitational; (Martinez et al. 2015)), we have now been able to reproduce in a qualitative sense the general range of residual neutronstar masses inferred for…”
Constraints on the neutron star equation of state from AT2017gfo using radiative transfer simulations (2018, background): “…recombination energy (e.g. Fryer, Woosley & Hartmann 1999; Di Matteo et al. 2002; Metzger, Piro & Quataert 2008; Dessart et al. 2009; Fernández & Metzger 2013; Perego et al. 2014; Siegel, Ciolfi & Rezzolla 2014; Ciolfi & Siegel 2015; Just et al. 2015; Martinez et al. 2015; Rezzolla & Kumar 2015).”
Formation of Double Neutron Star Systems (2017, background): “For some DNS systems, like PSR J0737−3039, the results obtained from the different DM distance models are quite similar, whereas in other cases (PSRs J0453+1559 and B1913+16) the 4 In the case of PSR B1913+16, we adopted a default distance based on HI absorption measurements (Weisberg et al. 2008). ”
Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors (2018, background): “…binary evolution like mass transfer and binary breakup, it is noteworthy that these gravitational masses fall nicely within the range of measured masses (∼ 1.17-1.6M ) in double neutron star systems (Martinez et al. 2015; Özel & Freire 2016; Tauris et al. 2017; Ferdman & PALFA Collaboration 2018).”