A puzzling paucity of double peaked X-ray pulsars (Articolo in rivista)

Type
Label
  • A puzzling paucity of double peaked X-ray pulsars (Articolo in rivista) (literal)
Anno
  • 2003-01-01T00:00:00+01:00 (literal)
Alternative label
  • Bulik, T.(1); Gondek-Rosinska, D.(2); Santangelo, A.(3); Mihara, T.(4), Finger, M.(5), Cemeljic, M.(6) (2003)
    A puzzling paucity of double peaked X-ray pulsars
    (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#autori
  • Bulik, T.(1); Gondek-Rosinska, D.(2); Santangelo, A.(3); Mihara, T.(4), Finger, M.(5), Cemeljic, M.(6) (literal)
Pagina inizio
  • 1023 (literal)
Pagina fine
  • 1032 (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#numeroVolume
  • 404 (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#descrizioneSinteticaDelProdotto
  • Pubblicazione dedicata allÂ’analisi e classificazione delle curve di luce di 89 Pulsar con disco di accrescimento e presentazione di un modello teorico adatto all fenomenologia (literal)
Note
  • ISI Web of Science (WOS) (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#affiliazioni
  • 1)Nicolaus Copernicus Astronomical Center, Bartycka 18, 00716 Warsaw, Poland), 2)LUTH, Observatoire de Paris, Place Jules Janssen, 92195 Meudon Cedex, France; Nicolaus Copernicus Astronomical Center, Bartycka 18, 00716 Warsaw, Poland), 3)IFCAI-CNR, via Ugo La Malfa 153, 90146 Palermo, Italy), 4)RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan), 5)(NSSTC, 320 Sparkman Dr., Hunstville, AL 35805, USA), 6)AIP, an der Sternwarte 16, 14482 Potsdam, Germany) (literal)
Titolo
  • A puzzling paucity of double peaked X-ray pulsars (literal)
Abstract
  • Accretion powered pulsars exhibit a variety of lightcurves. In this paper we propose to classify the observed lightcurves as single or double pulsed. We analyze the lightcurves of 89 accretion powered pulsars and assign them to these classes. We present three datasets: first in which the classification can be easily done, second for which the classification is more difficult and not certain, and third for which we were unable to classify the pulsar because of a lack of published data. We analyze a simple model in which the angles between the magnetic and rotation axis beta , and between the rotation axis and the line of sight theta are random, and show that it is inconsistent with the data. We also present a model in which the angle between the magnetic axis and the rotation axis is restricted and compare it with the data. This leads to an upper limit on the angle beta < 50o. We conclude that there must be a mechanism that leads to alignment of the magnetic and spin axis in X-ray pulsars. (literal)
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