PSR J1903+0327: A Unique Millisecond Pulsar With a Main-Sequence Companion Star

Khargharia, Juthika; Stocke, John T.; Froning, Cynthia S.; Gopakumar, A.; Joshi, B. C.

doi:10.1088/0004-637x/744/2/183

Cited by 16 publications

(9 citation statements)

References 36 publications

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“…Freire et al also measured an ẋ = 0.020(3) × 10 −12 that they attributed to proper-motion bias. A recent optical analysis of radial-velocity measurements estimated the mass ratio of this system to be q = m p /m c = 1.56(15) (68.3% confidence; Khargharia et al 2012), consistent with the radio-timing estimate of q = 1.62(3) made by Freire et al…”

Section: Resultssupporting

confidence: 87%

The Nanograv Nine-Year Data Set: Mass and Geometric Measurements of Binary Millisecond Pulsars

Fonseca

Pennucci

Ellis

et al. 2016

ApJ

607

441

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We analyze 24 binary radio pulsars in the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) nine-year data set. We make fourteen significant measurements of Shapiro delay, including new detections in four pulsar-binary systems (PSRs J0613−0200, J2017+0603, J2302+4442, and J2317+1439), and derive estimates of the binary-component masses and orbital inclination for these MSP-binary systems. We find a wide range of binary pulsar masses, with values as low as m p = 1.18 +0.10 −0.09 M for PSR J1918−0642 and as high as m p = 1.928 +0.017 −0.017 M for PSR J1614−2230 (both 68.3% credibility). We make an improved measurement of the Shapiro timing delay in the PSR J1918−0642 and J2043+1711 systems, measuring the pulsar mass in the latter system to be m p = 1.41 +0.21 −0.18 M (68.3% credibility) for the first time. We measure secular variations of one or more orbital elements in many systems, and use these measurements to further constrain our estimates of the pulsar and companion masses whenever possible. In particular, we used the observed Shapiro delay and periastron advance due to relativistic gravity in the PSR J1903+0327 system to derive a pulsar mass of m p = 1.65 +0.02 −0.02 M (68.3% credibility). We discuss the implications that our mass measurements have on the overall neutron-star mass distribution, and on the "mass/orbital-period" correlation due to extended mass transfer.

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Section: Resultssupporting

confidence: 87%

The Nanograv Nine-Year Data Set: Mass and Geometric Measurements of Binary Millisecond Pulsars

Fonseca

Pennucci

Ellis

et al. 2016

ApJ

607

441

View full text Add to dashboard Cite

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“…Similar conclusions have been derived by various other authors (e.g. : Portegies Zwart et al2011, Bejger et al2011, Pijloo et al2012, Khargharia 2012. After many years for which it was mostly a theoretical exercise, first the discovery of J1903+0327 and now (see Lazarus's contribution) that of a truly triple system in the Galactic field, promise to open the doors of a new gym for evolutionary and dynamical studies.…”

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confidence: 83%

Binary pulsar evolution: unveiled links and new species

Possenti¹

2012

Proc. IAU

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In the last years a series of blind and/or targeted pulsar searches led to almost triple the number of known binary pulsars in the galactic field with respect to a decade ago. The focus will be on few outliers, which are emerging from the average properties of the enlarged binary pulsar population. Some of them may represent the long sought missing links between two kinds of neutron star binaries, while others could represent the stereotype of new groups of binaries, resulting from an evolutionary path which is more exotic than those considered until recently. In particular, a new class of binaries, which can be dubbed Ultra Low Mass Binary Pulsars (ULMBPs), is emerging from recent data.

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“…In the case of PSR J1024−0719, the current binary companion is a main-sequence star and thus can not have recycled the pulsar. Currently we know of only one other MSP with a main-sequence companion; PSR J1903+0327, which is a 2.15 ms period MSP in a 95 day eccentric (e = 0.44) orbit (Champion et al 2008) around a 1.0 M G-dwarf companion (Freire et al 2011;Khargharia et al 2012). This system is believed to have evolved from a hierarchical triple consisting of a compact low-mass X-ray binary, accompanied by the G dwarf in a wide orbit.…”

Section: A Triple Star Formation Scenariomentioning

confidence: 99%

A millisecond pulsar in an extremely wide binary system

Bassa

Janssen

Stappers

et al. 2016

Mon. Not. R. Astron. Soc.

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We report on 22 yrs of radio timing observations of the millisecond pulsar J1024−0719 by the telescopes participating in the European Pulsar Timing Array (EPTA). These observations reveal a significant second derivative of the pulsar spin frequency and confirm the discrepancy between the parallax and Shklovskii distances that has been reported earlier. We also present optical astrometry, photometry and spectroscopy of 2MASS J10243869−0719190. We find that it is a low-metallicity main-sequence star (K7V spectral type, [M/H] = −1.0, T eff = 4050 ± 50 K) and that its position, proper motion and distance are consistent with those of PSR J1024−0719. We conclude that PSR J1024−0719 and 2MASS J10243869−0719190 form a common proper motion pair and are gravitationally bound. The gravitational interaction between the main-sequence star and the pulsar accounts for the spin frequency derivatives, which in turn resolves the distance discrepancy. Our observations suggest that the pulsar and main-sequence star are in an extremely wide (P b > 200 yr) orbit. Combining the radial velocity of the companion and proper motion of the pulsar, we find that the binary system has a high spatial velocity of 384 ± 45 km s −1 with respect to the local standard of rest and has a Galactic orbit consistent with halo objects. Since the observed main-sequence companion star cannot have recycled the pulsar to millisecond spin periods, an exotic formation scenario is required. We demonstrate that this extremely wide-orbit binary could have evolved from a triple system that underwent an asymmetric supernova explosion, though find that significant fine-tuning during the explosion is required. Finally, we discuss the implications of the long period orbit on the timing stability of PSR J1024−0719 in light of its inclusion in pulsar timing arrays.

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PSR J1903+0327: A Unique Millisecond Pulsar With a Main-Sequence Companion Star

Cited by 16 publications

References 36 publications

The Nanograv Nine-Year Data Set: Mass and Geometric Measurements of Binary Millisecond Pulsars

The Nanograv Nine-Year Data Set: Mass and Geometric Measurements of Binary Millisecond Pulsars

Binary pulsar evolution: unveiled links and new species

A millisecond pulsar in an extremely wide binary system

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