Journal
ASTROPHYSICAL JOURNAL
Volume 812, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/812/2/143
Keywords
gravitational waves; pulsars: general; pulsars: individual (J0453+1559)
Categories
Funding
- Chief of Naval Research
- European Research Council for the ERC Starting grant BEACON [279702]
- International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne
- Bonn-Cologne Graduate School of Physics and Astronomy
- Direct For Mathematical & Physical Scien
- Division Of Physics [1430284] Funding Source: National Science Foundation
- Office of Integrative Activities
- Office Of The Director [1458952] Funding Source: National Science Foundation
- Office Of Internatl Science &Engineering
- Office Of The Director [0968296] Funding Source: National Science Foundation
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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 M-p = 1.559 +/- 0.005 M-circle dot and that of its companion is M-c= 1.174 +/- 0.004 M-circle dot; 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)over dot = (1.8616 +/- 0.0007) x 10(-19) s s(-1); from these, we derive a characteristic age of similar to 4.1 x 10(9) years and a magnetic field of similar to 2.9 x 10(9) 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.
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