Abstract:Aims. T Pyx is the first recurrent nova ever historically studied. It was seen in outburst six times between 1890 and 1966 and then not for 45 years. We report on near-IR interferometric observations of the recent outburst of 2011. Methods. We obtained near-IR observations of T Pyx at dates ranging from t = 2.37 d to t = 48.2 d after the outburst, with the CLASSIC recombiner located at the CHARA array and with the PIONIER and AMBER recombiners located at the VLTI array. These data are supplemented with near-IR… Show more
“…Dust discs are observed in very different classes of stars known to be binaries (Chesneau et al 2011). Stable discs are observed around most known post-AGB binaries (van Winckel 2003;de Ruyter et al 2006;Van Winckel et al 2006).…”
Circumbinary discs are commonly observed around post-asymptotic giant branch (post-AGB) systems and are known to play an important role in their evolution. Several studies have pointed out that a circumbinary disc interacts through resonances with the central binary and leads to angular momentum transfer from the central binary orbit to the disc. This interaction may be responsible for a substantial increase in the binary eccentricity. We investigate whether this disc eccentricity-pumping mechanism can be responsible for the high eccentricities commonly found in post-AGB binary systems.
“…Dust discs are observed in very different classes of stars known to be binaries (Chesneau et al 2011). Stable discs are observed around most known post-AGB binaries (van Winckel 2003;de Ruyter et al 2006;Van Winckel et al 2006).…”
Circumbinary discs are commonly observed around post-asymptotic giant branch (post-AGB) systems and are known to play an important role in their evolution. Several studies have pointed out that a circumbinary disc interacts through resonances with the central binary and leads to angular momentum transfer from the central binary orbit to the disc. This interaction may be responsible for a substantial increase in the binary eccentricity. We investigate whether this disc eccentricity-pumping mechanism can be responsible for the high eccentricities commonly found in post-AGB binary systems.
“…Shara et al 1997). This confusion has been dramatically removed by the infrared continuum and line spectrointerferometric observations during the current outburst by Chesneau et al (2011) using infrared CHARA and VLTI. They find that after day 28 the AMBER K-band and PIONIER-H band visibilities are consistent with a two-component bipolar plus central point source model with very low inclination.…”
Section: Modeling the Structure Of The Ejectamentioning
Aims. We continue our study of the physical properties of the recurrent nova T Pyx, focussing on the structure of the ejecta in the nebular stage of expansion during the 2011 outburst.
“…As pragmatic as he could be, he decided to perform a simple analysis with simple geometric models (Chesneau & Banerjee 2012). Middle: T Pyx bipolar fireball, as seen by AMBER and PIONIER as a face-on bipolar nebula (Chesneau et al 2011). Right: NACO/VLT 2010 K band image of V1280 Sco, revealing a bipolar dusty nebula developed by N. Nardetto.…”
Section: Live Formation Of Bipolar Novae: Rs Oph and T Pyxmentioning
Abstract. Olivier Chesneau founded a brand new field of observational astrophysics with his attempts to resolve the novae expanding fireball from the very first days of the explosion. With the images he could get, he showed that novae do indeed explode in an aspherical way, leading to a change of paradigm for the physics of these yet-poorly understood catastrophic systems. He also set the stage for a new way of estimating novae distances, by directly measuring the sky-size of the fireball and comparing it with spectroscopic scales, taking into account the tremendous effects of the fireball geometry.
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