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Radio and γ-ray constraints on the emission geometry and birthplace of PSR j2043+2740
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2011 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 728, no 2, 77- p.Article in journal (Refereed) Published
Abstract [en]

We report on the first year of Fermi γ-ray observations of pulsed high-energy emission from the old PSR J2043 + 2740. The study of the γ-ray efficiency of such old pulsars gives us an insight into the evolution of pulsars' ability to emit in γ rays as they age. The y-ray light curve of this pulsar above 0.1 GeV is clearly defined by two sharp peaks, 0.353 ± 0.035 periods apart. We have combined the γ-ray profile characteristics of PSR J2043 + 2740 with the geometrical properties of the pulsar's radio emission, derived from radio-polarization data, and constrained the pulsar-beam geometry in the framework of a two-pole caustic (TPC) and an outer gap (OG) model. The ranges of magnetic inclination and viewing angle were determined to be {α, ζ} ∼ {52°-57°, 61°-68°} for the TPC model, and {α, ζ} ∼ {62°-73°, 74°-81°} and {α, ζ,} ∼ {72°-83°, 60°-75°} for the OG model. Based on this geometry, we assess possible birth locations for this pulsar and derive a likely proper motion, sufficiently high to be measurable with VLBI. At a characteristic age of 1.2 Myr, PSR J2043 + 2740 is the third oldest of all discovered, non-recycled, γ-ray pulsars: it is twice as old as the next oldest, PSR J0357 + 32, and younger only than the recently discovered PSR J1836 + 5925 and PSR J2055 + 25, both of which are at least five and ten times less energetic, respectively.

Place, publisher, year, edition, pages
2011. Vol. 728, no 2, 77- p.
Keyword [en]
Gamma rays: stars, Pulsars: individual (PSR J2043 + 2740)
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:kth:diva-141870DOI: 10.1088/0004-637X/728/2/77ISI: 000286973600004Scopus ID: 2-s2.0-84891222024OAI: oai:DiVA.org:kth-141870DiVA: diva2:698846
Note

QC 20140225

Available from: 2014-02-25 Created: 2014-02-25 Last updated: 2017-12-05Bibliographically approved

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