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AuthorsL. Lin, C. Kouveliotou, M.G. Baring, A.J. van der Horst, S. Guiriec, P.M. Woods, E. Gogus, Y. Kaneko, J. Scargle, J. Granot, R. Preece, A. von Kienlin, V. Chaplin, A.L. Watts, R.A.M.J. Wijers, S.N. Zhang, N. Bhat, M.H. Finger, N. Gehrels, A. Harding, L. Kaper, V. Kaspi, J. Mcenery, C.A. Meegan, W.S. Paciesas, A. Pe'er, E. Ramirez-Ruiz, M. van der Klis, S. Wachter, C. Wilson-Hodge
TitleFermi/Gamma-ray burst monitor observations of SGR J0501+4516 bursts
JournalAstrophysical Journal
Volume739
Year2011
Pages16
ISSN0004637X
FacultyFaculty of Science
Institute/dept.FNWI: Astronomical Institute Anton Pannekoek (IAP)
AbstractWe present our temporal and spectral analyses of 29 bursts from SGR J0501+4516, detected with the gamma-ray burst monitor on board the Fermi Gamma-ray Space Telescope during 13 days of the source's activation in 2008 (August 22- September 3). We find that the T 90 durations of the bursts can be fit with a log-normal distribution with a mean value of ~123 ms. We also estimate for the first time event durations of soft gamma repeater (SGR) bursts in photon space (i.e., using their deconvolved spectra) and find that these are very similar to the T 90 values estimated in count space (following a log-normal distribution with a mean value of ~124 ms). We fit the time-integrated spectra for each burst and the time-resolved spectra of the five brightest bursts with several models. We find that a single power law with an exponential cutoff model fits all 29 bursts well, while 18 of the events can also be fit with two blackbody functions. We expand on the physical interpretation of these two models and we compare their parameters and discuss their evolution. We show that the time-integrated and time-resolved spectra reveal that E peak decreases with energy flux (and fluence) to a minimum of ~30 keV at F = 8.7 × 10–6 erg cm–2 s–1, increasing steadily afterward. Two more sources exhibit a similar trend: SGRs J1550-5418 and 1806-20. The isotropic luminosity, L iso, corresponding to these flux values is roughly similar for all sources (0.4-1.5 × 1040 erg s–1).
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