The UvA-LINKER will give you a range of other options to find the full text of a publication (including a direct link to the full-text if it is located on another database on the internet).
De UvA-LINKER biedt mogelijkheden om een publicatie elders te vinden (inclusief een directe link naar de publicatie online als deze beschikbaar is in een database op het internet).


Zoekopdracht: journal id: "astrophysicalxjournal"

AuteursD.L. Kaplan, K. Stovall, S.M. Ransom, M.S.E. Roberts, R. Kotulla, A.M. Archibald, C.M. Biwer, J. Boyles, L. Dartez, D.F. Day, A.J. Ford, A. Garcia, J.W.T. Hessels, F.A. Jenet, C. Karako, V.M. Kaspi, V.I. Kondratiev, D.R. Lorimer, R.S. Lynch, M.A. McLaughlin, M.D.W. Rohr, X. Siemens, I.H. Stairs, J. van Leeuwen
TitelDiscovery of the Optical/Ultraviolet/Gamma-Ray Counterpart to the Eclipsing Millisecond Pulsar J1816+4510
TijdschriftAstrophysical Journal
FaculteitFaculteit der Natuurwetenschappen, Wiskunde en Informatica
Instituut/afd.FNWI: Astronomical Institute Anton Pannekoek (IAP)
SamenvattingThe energetic, eclipsing millisecond pulsar J1816+4510 was recently discovered in a low-frequency radio survey with the Green Bank Telescope. With an orbital period of 8.7 hr and a minimum companion mass of 0.16 M ☉, it appears to belong to an increasingly important class of pulsars that are ablating their low-mass companions. We report the discovery of the γ-ray counterpart to this pulsar and present a likely optical/ultraviolet counterpart as well. Using the radio ephemeris, we detect pulsations in the unclassified γ-ray source 2FGL J1816.5+4511, implying an efficiency of ~25% in converting the pulsar's spin-down luminosity into γ-rays and adding PSR J1816+4510 to the large number of millisecond pulsars detected by Fermi. The likely optical/UV counterpart was identified through position coincidence (<0farcs1) and unusual colors. Assuming that it is the companion, with R = 18.27 ± 0.03 mag and effective temperature gsim 15,000 K, it would be among the brightest and hottest of low-mass pulsar companions and appears qualitatively different from other eclipsing pulsar systems. In particular, current data suggest that it is a factor of two larger than most white dwarfs of its mass but a factor of four smaller than its Roche lobe. We discuss possible reasons for its high temperature and odd size, and suggest that it recently underwent a violent episode of mass loss. Regardless of origin, its brightness and the relative unimportance of irradiation make it an ideal target for a mass, and hence a neutron star mass, determination.
Soort documentArtikel
Document finderUvA-Linker