Show simple item record

dc.contributor.authorVenter, C.
dc.contributor.authorHarding, A.K.
dc.contributor.authorGuillemot, L.
dc.date.accessioned2014-05-05T14:22:40Z
dc.date.available2014-05-05T14:22:40Z
dc.date.issued2009
dc.identifier.citationVenter, C. et al. 2009. Probing millisecond pulsar emission geometry using light curves from the fermi/large area telescope. Astrophysical journal, 707(1):800-822. [http://iopscience.iop.org/0004-637X/]en_US
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357 (Online)
dc.identifier.urihttp://hdl.handle.net/10394/10483
dc.identifier.urihttp://dx.doi.org/10.1088/0004-637X/707/1/800
dc.identifier.urihttp://iopscience.iop.org/0004-637X/707/1/800/pdf/0004-637X_707_1_800.pdf
dc.description.abstractAn interesting new high-energy pulsar sub-population is emerging following early discoveries of gamma-ray millisecond pulsars (MSPs) by the Fermi Large Area Telescope (LAT). We present results from three-dimensional emission modeling, including the special relativistic effects of aberration and time-of-flight delays and also rotational sweepback of B-field lines, in the geometric context of polar cap (PC), outer gap (OG), and two-pole caustic (TPC) pulsar models. In contrast to the general belief that these very old, rapidly rotating neutron stars (NSs) should have largely pair-starved magnetospheres due to the absence of significant pair production, we find that most of the light curves are best fit by TPC and OG models, which indicates the presence of narrow accelerating gaps limited by robust pair production—even in these pulsars with very low spin-down luminosities. The gamma-ray pulse shapes and relative phase lags with respect to the radio pulses point to high-altitude emission being dominant for all geometries. We also find exclusive differentiation of the current gamma-ray MSP population into two MSP sub-classes: light curve shapes and lags across wavebands impose either pair-starved PC (PSPC) or TPC/OG-type geometries. In the first case, the radio pulse has a small lag with respect to the single gamma-ray pulse, while the (first) gamma-ray peak usually trails the radio by a large phase offset in the latter case. Finally, we find that the flux correction factor as a function of magnetic inclination and observer angles is typically of order unity for all models. Our calculation of light curves and flux correction factor for the case of MSPs is therefore complementary to the "ATLAS paper" of Watters et al. for younger pulsars.en_US
dc.language.isoenen_US
dc.publisherIOP Publishingen_US
dc.rights© 2009. The American Astronomical Society. All rights reserved.
dc.subjectAcceleration of particlesen_US
dc.subjectgamma rays: theoryen_US
dc.subjectpulsars: generalen_US
dc.subjectradiation mechanisms: non-thermal stars: neutronen_US
dc.titleProbing millisecond pulsar emission geometry using light curves from the fermi/large area telescopeen_US
dc.typeArticleen_US
dc.contributor.researchID12006653 - Venter, Christo


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record