منابع مشابه
CI Cam: A Shell-shocked X-ray Nova
We present radio imaging observations of the 1998 outburst of the peculiar emission line star CICam, taken ∼1, 4, 75, 82, 93, 163, and 306 days after the beginning of the 31.64 March 1998 X-ray flare. The first two epochs show a resolved but compact (no larger than 12 milliarcseconds) radio source which becomes optically thin at frequencies higher than 5GHz. The spectrum and brightness temperat...
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We describe observational evidence for a new kind of interacting-binary-star outburst that involves both an accretion instability and an increase in thermonuclear shell burning on the surface of an accreting white dwarf. We refer to this new type of eruption as a combination nova. In late 2000, the prototypical symbiotic star Z Andromedae brightened by roughly two magnitudes in the optical. We ...
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We report the results of two Chandra observations of the recurrent nova CI Aql at 14 and 16 months after its outburst in April 2000, respectively. The X-ray emission is faint in both cases, without any noticeable change in spectrum or intensity. Although the emission is very soft, it is not luminous enough to be due to late-time H-burning. This implies that the luminous supersoft phase ended ev...
متن کاملVLTI / AMBER interferometric observations of the recurrent Nova RS Oph 5 . 5 days after outburst ⋆
Aims. We report on spectrally dispersed interferometric AMBER/VLTI observations of the recurrent nova RSOph five days after the discovery of its outburst on 2006 Feb 12. Methods. Using three baselines ranging from 44 to 86m, and a spectral resolution of λ/δλ=1500, we measured the extension of the milliarcsecond-scale emission in the K band continuum and in the Brγ and He I 2.06μm lines, allowin...
متن کاملV5116 Sgr, an Eclipsing Supersoft Post-outburst Nova?
months after the optical outburst. The X-ray spectrum shows that the nova had evolved to a pure supersoft X-ray source, with no significant emission at energies above 1 keV. The X-ray light-curve shows abrupt decreases and increases of the flux by a factor ∼ 8. It is consistent with a periodicity of 2.97 h, the orbital period suggested by Dobrotka et al. (2007), although the observation lasted ...
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ژورنال
عنوان ژورنال: Science
سال: 2014
ISSN: 0036-8075,1095-9203
DOI: 10.1126/science.345.6192.43-h