The evolution and masses of the neutron star and donor star in the high mass X-ray binary OAO 1657−415
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Título: | The evolution and masses of the neutron star and donor star in the high mass X-ray binary OAO 1657−415 |
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Autor/es: | Mason, Andrew B. | Clark, J. Simon | Norton, Andrew J. | Crowther, Paul A. | Tauris, Thomas M. | Langer, Norbert | Negueruela, Ignacio | Roche, Paul |
Grupo/s de investigación o GITE: | Astrofísica Estelar (AE) |
Centro, Departamento o Servicio: | Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal |
Palabras clave: | Binaries: eclipsing | Binaries: general | Stars: individual: OAO 1657−415 | Stars: massive | Stars: Wolf–Rayet | X-rays: binaries |
Área/s de conocimiento: | Astronomía y Astrofísica |
Fecha de publicación: | 1-may-2012 |
Editor: | Royal Astronomical Society |
Cita bibliográfica: | Monthly Notices of the Royal Astronomical Society. 2012, 422(1): 199-206. doi:10.1111/j.1365-2966.2012.20596.x |
Resumen: | We report near-infrared radial velocity (RV) measurements of the recently identified donor star in the high mass X-ray binary (HMXB) system OAO 1657−415 obtained in the H band using ISAAC on the Very Large Telescope. Cross-correlation methods were employed to construct a RV curve with a semi-amplitude of 22.1 ± 3.5 km s−1. Combined with other measured parameters of this system it provides a dynamically determined neutron star (NS) mass of 1.42 ± 0.26 M⊙ and a mass of 14.3 ± 0.8 M⊙ for the Ofpe/WN9 highly evolved donor star. OAO 1657−415 is an eclipsing HMXB pulsar with the largest eccentricity and orbital period of any within its class. Of the 10 known eclipsing X-ray binary pulsars OAO 1657−415 becomes the ninth with a dynamically determined NS mass solution and only the second in an eccentric system. Furthermore, the donor star in OAO 1657−415 is much more highly evolved than the majority of the supergiant donors in other HMXBs, joining a small but growing list of HMXBs donors with extensive hydrogen depleted atmospheres. Considering the evolutionary development of OAO 1657−415, we have estimated the binding energy of the envelope of the mass donor and find that there is insufficient energy for the removal of the donor’s envelope via spiral-in, ruling out a common envelope evolutionary scenario. With its non-zero eccentricity and relatively large orbital period the identification of a definitive evolutionary pathway for OAO 1657−415 remains problematic, we conclude by proposing two scenarios which may account for OAO 1657−415 current orbital configuration. |
Patrocinador/es: | ABM acknowledges support from an STFC studentship. JSC acknowledges support from an RCUK fellowship. This research is partially supported by grantsAYA2008-06166-C03-03 and Consolider-GTC CSD-2006-00070 from the Spanish Ministerio de Ciencia e Innovación (MICINN). |
URI: | http://hdl.handle.net/10045/33862 |
ISSN: | 0035-8711 (Print) | 1365-2966 (Online) |
DOI: | 10.1111/j.1365-2966.2012.20596.x |
Idioma: | eng |
Tipo: | info:eu-repo/semantics/article |
Derechos: | © 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS |
Revisión científica: | si |
Versión del editor: | http://dx.doi.org/10.1111/j.1365-2966.2012.20596.x |
Aparece en las colecciones: | INV - Astrofísica Estelar - Artículos de Revistas |
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