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  Timing of a Young Mildly Recycled Pulsar with a Massive White Dwarf Companion

Lazarus, P., Tauris, T. M., Knispel, B., Freire, P. C. C., Deneva, J. S., Kaspi, V. M., et al. (2014). Timing of a Young Mildly Recycled Pulsar with a Massive White Dwarf Companion. Monthly Notices of the Royal Astronomical Society, 437 (2), 1485-1494. doi:10.1093/mnras/stt1996.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-0014-77A4-F Version Permalink: http://hdl.handle.net/11858/00-001M-0000-002B-5F86-E
Genre: Journal Article

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 Creators:
Lazarus, P., Author
Tauris, T. M., Author
Knispel, B.1, Author              
Freire, P. C. C., Author
Deneva, J. S., Author
Kaspi, V. M., Author
Allen, B.1, Author              
Bogdanov, S., Author
Chatterjee, S., Author
Stairs, I. H., Author
Zhu, W. W., Author
Affiliations:
1Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_24011              

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Free keywords: Astrophysics, Solar and Stellar Astrophysics, astro-ph.SR, Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE
 Abstract: We report on timing observations of the recently discovered binary pulsar PSR J1952+2630 using the Arecibo Observatory. The mildly recycled 20.7-ms pulsar is in a 9.4-hr orbit with a massive, M_WD > 0.93 M_sun, white dwarf (WD) companion. We present, for the first time, a phase-coherent timing solution, with precise spin, astrometric, and Keplerian orbital parameters. This shows that the characteristic age of PSR J1952+2630 is 77 Myr, younger by one order of magnitude than any other recycled pulsar-massive WD system. We derive an upper limit on the true age of the system of 50 Myr. We investigate the formation of PSR J1952+2630 using detailed modelling of the mass-transfer process from a naked helium star on to the neutron star following a common-envelope phase (Case BB Roche-lobe overflow). From our modelling of the progenitor system, we constrain the accretion efficiency of the neutron star, which suggests a value between 100 and 300% of the Eddington accretion limit. We present numerical models of the chemical structure of a possible oxygen-neon-magnesium WD companion. Furthermore, we calculate the past and the future spin evolution of PSR J1952+2630, until the system merges in about 3.4 Gyr due to gravitational wave emission. Although we detect no relativistic effects in our timing analysis we show that several such effects will become measurable with continued observations over the next 10 years; thus PSR J1952+2630 has potential as a testbed for gravitational theories.

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 Dates: 2013-10-222014
 Publication Status: Published in print
 Pages: 12 pages, 10 figures, to be published in MNRAS
 Publishing info: -
 Table of Contents: -
 Rev. Method: -
 Identifiers: arXiv: 1310.5857
URI: http://arxiv.org/abs/1310.5857
DOI: 10.1093/mnras/stt1996
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Title: Monthly Notices of the Royal Astronomical Society
Source Genre: Journal
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Publ. Info: Oxford : Blackwell Science
Pages: - Volume / Issue: 437 (2) Sequence Number: - Start / End Page: 1485 - 1494 Identifier: ISSN: 1365-8711
CoNE: /journals/resource/1000000000024150