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Title: THE FORMATION OF THE ECCENTRIC-ORBIT MILLISECOND PULSAR J1903+0327 AND THE ORIGIN OF SINGLE MILLISECOND PULSARS

Abstract

The millisecond pulsar (MSP) J1903+0327 is accompanied by an ordinary G dwarf star in an unusually wide (P{sub orb} {approx_equal} 95.2 days) and eccentric (e {approx_equal} 0.44) orbit. The standard model for producing MSPs fails to explain the orbital characteristics of this extraordinary binary, and alternative binary models are unable to explain the observables. We present a triple-star model for producing MSPs in relatively wide eccentric binaries with a normal (main-sequence) stellar companion. We start from a stable triple system consisting of a low-mass X-ray binary (LMXB) with an orbital period of at least 1 day, accompanied by a G dwarf in a wide and possibly eccentric orbit. Variations in the initial conditions naturally provide a satisfactory explanation for the unexplained triple component in the eclipsing soft X-ray transient 4U 2129+47 or the cataclysmic variable EC 19314-5915. The best explanation for J1903+0327, however, results from the expansion of the orbit of the LMXB, driven by the mass transfer from the evolving donor star to its neutron star companion, which causes the triple eventually to become dynamically unstable. Using numerical computations we show that, depending on the precise system configuration at the moment the triple becomes dynamically unstable, the ejection ofmore » each of the three components is possible. If the donor star of the LMXB is ejected, a system resembling J1903+0327 will result. If the neutron star is ejected, a single MSP results. This model therefore also provides a straightforward mechanism for forming a single MSP in the Galactic disk. We conclude that the Galaxy contains some 30-300 binaries with characteristics similar to J1903+0327 and about an order of magnitude fewer single MSPs produced with the proposed triple scenario.« less

Authors:
 [1];  [2];  [3]
  1. Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden (Netherlands)
  2. Stichting ASTRON, P.O. Box 2, 7990 AA Dwingeloo (Netherlands)
  3. Department of Astrophysics, Radboud University Nijmegen, Heyendaalseweg 135, NL-6525 AJ Nijmegen (Netherlands)
Publication Date:
OSTI Identifier:
21576636
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 734; Journal Issue: 1; Other Information: DOI: 10.1088/0004-637X/734/1/55; Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; DWARF STARS; MASS TRANSFER; NEUTRON STARS; ORBITS; PULSARS; STAR MODELS; COSMIC RADIO SOURCES; MATHEMATICAL MODELS; STARS

Citation Formats

Portegies Zwart, S, Van den Heuvel, E. P. J., Van Leeuwen, J, and Nelemans, G. THE FORMATION OF THE ECCENTRIC-ORBIT MILLISECOND PULSAR J1903+0327 AND THE ORIGIN OF SINGLE MILLISECOND PULSARS. United States: N. p., 2011. Web. doi:10.1088/0004-637X/734/1/55.
Portegies Zwart, S, Van den Heuvel, E. P. J., Van Leeuwen, J, & Nelemans, G. THE FORMATION OF THE ECCENTRIC-ORBIT MILLISECOND PULSAR J1903+0327 AND THE ORIGIN OF SINGLE MILLISECOND PULSARS. United States. https://doi.org/10.1088/0004-637X/734/1/55
Portegies Zwart, S, Van den Heuvel, E. P. J., Van Leeuwen, J, and Nelemans, G. Fri . "THE FORMATION OF THE ECCENTRIC-ORBIT MILLISECOND PULSAR J1903+0327 AND THE ORIGIN OF SINGLE MILLISECOND PULSARS". United States. https://doi.org/10.1088/0004-637X/734/1/55.
@article{osti_21576636,
title = {THE FORMATION OF THE ECCENTRIC-ORBIT MILLISECOND PULSAR J1903+0327 AND THE ORIGIN OF SINGLE MILLISECOND PULSARS},
author = {Portegies Zwart, S and Van den Heuvel, E. P. J. and Van Leeuwen, J and Nelemans, G},
abstractNote = {The millisecond pulsar (MSP) J1903+0327 is accompanied by an ordinary G dwarf star in an unusually wide (P{sub orb} {approx_equal} 95.2 days) and eccentric (e {approx_equal} 0.44) orbit. The standard model for producing MSPs fails to explain the orbital characteristics of this extraordinary binary, and alternative binary models are unable to explain the observables. We present a triple-star model for producing MSPs in relatively wide eccentric binaries with a normal (main-sequence) stellar companion. We start from a stable triple system consisting of a low-mass X-ray binary (LMXB) with an orbital period of at least 1 day, accompanied by a G dwarf in a wide and possibly eccentric orbit. Variations in the initial conditions naturally provide a satisfactory explanation for the unexplained triple component in the eclipsing soft X-ray transient 4U 2129+47 or the cataclysmic variable EC 19314-5915. The best explanation for J1903+0327, however, results from the expansion of the orbit of the LMXB, driven by the mass transfer from the evolving donor star to its neutron star companion, which causes the triple eventually to become dynamically unstable. Using numerical computations we show that, depending on the precise system configuration at the moment the triple becomes dynamically unstable, the ejection of each of the three components is possible. If the donor star of the LMXB is ejected, a system resembling J1903+0327 will result. If the neutron star is ejected, a single MSP results. This model therefore also provides a straightforward mechanism for forming a single MSP in the Galactic disk. We conclude that the Galaxy contains some 30-300 binaries with characteristics similar to J1903+0327 and about an order of magnitude fewer single MSPs produced with the proposed triple scenario.},
doi = {10.1088/0004-637X/734/1/55},
url = {https://www.osti.gov/biblio/21576636}, journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 734,
place = {United States},
year = {2011},
month = {6}
}