X-Ray Eclipse Time Delays in 4U2129+47

Tiziana Di Salvo, Mangano, Falanga, Gianluca Israel, Bozzo, Campana, Lazzati, Burderi, Perna, Stella, Papitto

Risultato della ricerca: Articlepeer review

9 Citazioni (Scopus)


Aims.4U 2129+47 was discovered in the early 80's and classified as an accretion disk corona source due to its broad and partial X-ray eclipses. The 5.24 h binary orbital period was inferred from the X-ray and optical light curve modulation, implying a late K or M spectral type companion star. The source entered a low state in 1983, during which the optical modulation disappeared and an F8 IV star was revealed, suggesting that 4U 2129+47 might be part of a triple system. The nature of 4U 2129+47 has since been investigated, but no definitive conclusion has been reached.Methods.Here, we present timing and spectral analyses of two XMM-Newton  observations of this source, carried out in May and June, 2005.Results.We find evidence for a delay between two mid-eclipse epochs measured ~22 days apart, and we show that this delay can be naturally explained as being due to the orbital motion of the binary 4U 2129+47 around the center of mass of a triple system. This result thus provides further support in favor of the triple nature of 4U 2129+47
Lingua originaleEnglish
pagine (da-a)301-306
Numero di pagine6
Stato di pubblicazionePublished - 2007

All Science Journal Classification (ASJC) codes

  • ???subjectarea.asjc.3100.3103???
  • ???subjectarea.asjc.1900.1912???


Entra nei temi di ricerca di 'X-Ray Eclipse Time Delays in 4U2129+47'. Insieme formano una fingerprint unica.

Cita questo