Evidence of Compton cooling during an X-ray flare supports a neutron star nature of the compact object in 4U1700−37

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Título: Evidence of Compton cooling during an X-ray flare supports a neutron star nature of the compact object in 4U1700−37
Autor/es: Martinez-Chicharro, Maria | Torrejon, Jose M. | Oskinova, Lidia M. | Fürst, Felix | Postnov, Konstantin | Rodes Roca, José Joaquín | Hainich, Rainer | Bodaghee, Arash
Grupo/s de investigación o GITE: Astronomía y Astrofísica
Centro, Departamento o Servicio: Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal | Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías
Palabras clave: Stars: individual: 4U1700−37, V*V884 Sco | X-rays: binaries
Área/s de conocimiento: Física Aplicada
Fecha de publicación: 1-ene-2018
Editor: Oxford University Press
Cita bibliográfica: Monthly Notices of the Royal Astronomical Society: Letters. 2018, 473(1): L74-L78. doi:10.1093/mnrasl/slx165
Resumen: Based on new Chandra X-ray telescope data, we present empirical evidence of plasma Compton cooling during a flare in the non-pulsating massive X-ray binary 4U1700−37. This behaviour might be explained by quasi-spherical accretion on to a slowly rotating magnetized neutron star (NS). In quiescence, the NS in 4U1700−37 is surrounded by a hot radiatively cooling shell. Its presence is supported by the detection of mHz quasi-periodic oscillations likely produced by its convection cells. The high plasma temperature and the relatively low X-ray luminosity observed during the quiescence, point to a small emitting area ∼1 km, compatible with a hotspot on an NS surface. The sudden transition from a radiative to a significantly more efficient Compton cooling regime triggers an episode of enhanced accretion resulting in a flare. During the flare, the plasma temperature drops quickly. The predicted luminosity for such transitions, ∼3 × 1035 erg s−1, is very close to the luminosity of 4U1700−37 during quiescence. The transition may be caused by the accretion of a clump in the stellar wind of the donor star. Thus, a magnetized NS nature of the compact object is strongly favoured.
Patrocinador/es: This research has been supported by the grant ESP2014-53672-C3-3P. AB acknowledges support from STScI award 44A-1096046. JJRR acknowledges support from MECD fellowship PRX17/00114.
URI: http://hdl.handle.net/10045/72701
ISSN: 1745-3925 (Print) | 1745-3933 (Online)
DOI: 10.1093/mnrasl/slx165
Idioma: eng
Tipo: info:eu-repo/semantics/article
Derechos: © 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
Revisión científica: si
Versión del editor: http://dx.doi.org/10.1093/mnrasl/slx165
Aparece en las colecciones:INV - Astronomía y Astrofísica - Artículos de Revistas

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