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Title:
X-ray eclipse time delays in 4U 2129+47
Authors:
Bozzo, E.; Falanga, M.; Papitto, A.; Stella, L.; Perna, R.; Lazzati, D.; Israel, G.; Campana, S.; Mangano, V.; di Salvo, T.; Burderi, L.
Affiliation:
AA(INAF - Osservatorio Astronomico di Roma, Via Frascati 33, 00044 Rome, Italy ; Dipartimento di Fisica - Università di Roma Tor Vergata, via della Ricerca Scientifica 1, 00133 Rome, Italy), AB(CEA Saclay, DSM/DAPNIA/Service d'Astrophysique (CNRS FRE 2591), 91191 Gif-sur-Yvette, France), AC(INAF - Osservatorio Astronomico di Roma, Via Frascati 33, 00044 Rome, Italy; Dipartimento di Fisica - Università di Roma Tor Vergata, via della Ricerca Scientifica 1, 00133 Rome, Italy), AD(INAF - Osservatorio Astronomico di Roma, Via Frascati 33, 00044 Rome, Italy), AE(JILA, University of Colorado, Boulder, CO 80309-0440, USA), AF(JILA, University of Colorado, Boulder, CO 80309-0440, USA), AG(INAF - Osservatorio Astronomico di Roma, Via Frascati 33, 00044 Rome, Italy), AH(INAF Osservatorio Astronomico di Brera, via Emilio Bianchi 46, 23807 Merate (LC), Italy), AI(INAF Istituto di Astrofisica Spaziale e Fisica Cosmica Sezione di Palermo, via Ugo La Malfa 153, 90146 Palermo, Italy), AJ(Dipartimento di Scienze Fisiche ed Astronomiche, Università di Palermo, via Archirafi 36, 90123 Palermo, Italy), AK(Università degli Studi di Cagliari, Dipartimento di Fisica, SP Monserrato-Sestu, KM 0.7, 09042 Monserrato, Italy)
Publication:
Astronomy and Astrophysics, Volume 476, Issue 1, December II 2007, pp.301-306 (A&A Homepage)
Publication Date:
12/2007
Origin:
EDP
Keywords:
accretion, accretion disks, binaries: eclipsing, stars: individual:, 4U 2129+47, stars: neutron, X-rays: stars
DOI:
10.1051/0004-6361:20078444
Bibliographic Code:
2007A&A...476..301B

Abstract

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.
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