The expanding fireball of Nova Delphini 2013

  title={The expanding fireball of Nova Delphini 2013},
  author={Gail H. Schaefer and Theo A. ten Brummelaar and Douglas R. Gies and Christopher D. Farrington and Brian Kloppenborg and Olivier Chesneau and John D. Monnier and Stephen T. Ridgway and Nicholas J. Scott and I. Tallon-Bosc and Harold A. Mcalister and Tabetha Boyajian and Vicente Maestro and Denis Mourard and Anthony Meilland and Nicolas Nardetto and P. Stee and Judit Sturmann and Norm Vargas and F. Baron and Michael J. Ireland and Ellyn K. Baines and Xiao Che and J. M. Jones and Noel D. Richardson and Rachael M. Roettenbacher and Laszlo Sturmann and Nils H. Turner and Peter G. Tuthill and Gerard T. van Belle and Kaspar von Braun and Robert T. Zavala and Dipankar Banerjee and Nagarhalli M. Ashok and V. Joshi and Juliette C. Becker and Philip S. Muirhead},
A classical nova occurs when material accreting onto the surface of a white dwarf in a close binary system ignites in a thermonuclear runaway. Complex structures observed in the ejecta at late stages could result from interactions with the companion during the common-envelope phase. Alternatively, the explosion could be intrinsically bipolar, resulting from a localized ignition on the surface of the white dwarf or as a consequence of rotational distortion. Studying the structure of novae during… Expand
A nova outburst powered by shocks
Classical novae are runaway thermonuclear burning events on the surfaces of accreting white dwarfs in close binary star systems, sometimes appearing as new naked-eye sources in the night sky1. TheExpand
Explosive lithium production in the classical nova V339 Del (Nova Delphini 2013)
The detection of highly blue-shifted resonance lines of the singly ionized radioactive isotope of beryllium, 7Be, in the near-ultraviolet spectra of the classical nova V339 Del (Nova Delphini 2013) 38 to 48 days after the explosion supports the theoretical prediction that a significant amount of 7Li is produced in classicalNova explosions. Expand
Multiwavelength models SED of the classical nova V339 Del (Nova Del 2013) along its age
Classical nova V339 Del (Nova Del 2013) is a fast nova of the Fe II class, whose eruption was ignited on a CO white dwarf (WD). In this contribution we present the spectral energy distribution (SED)Expand
Discovery of an eclipsing dwarf nova in the ancient nova shell Te 11
We report on the discovery of an eclipsing dwarf nova (DN) inside the peculiar, bilobed nebula Te 11. Modelling of high-speed photometry of the eclipse finds the accreting white dwarf to have a massExpand
The panchromatic spectroscopic evolution of the classical CO nova V339 Delphini (Nova Del 2013) until X-ray turnoff
Context. Classical novae are the product of thermonuclear runaway-initiated explosions occurring on accreting white dwarfs. Aims. V339 Del (Nova Delphinus 2013) was one of the brightest classicalExpand
Multiwavelength Modeling of the SED of Nova V339 Del: Stopping the Wind and Long-lasting Super-Eddington Luminosity with Dust Emission
  • A. Skopal
  • Physics
  • The Astrophysical Journal
  • 2019
During the classical nova outburst, the radiation generated by the nuclear burning of hydrogen in the surface layer of a white dwarf (WD) is reprocessed by the outer material into different forms atExpand
The Distance to Nova V959 Mon from VLA Imaging
Determining reliable distances to classical novae is a challenging but crucial step in deriving their ejected masses and explosion energetics. Here we combine radio expansion measurements from theExpand
Structure and chemical composition of the envelope of Nova V339 del in the nebular phase
Based on our spectrophotometric observations, we have investigated the envelope of Nova V339 Del in the nebular phase. Our modeling of the Hα line profiles and their comparison with the observedExpand
Shock-powered radio emission from V5589 Sagittarii (Nova Sgr 2012 #1)
Since the Fermi discovery of $\gamma$-rays from novae, one of the biggest questions in the field has been how novae generate such high-energy emission. Shocks must be a fundamental ingredient. SixExpand
Radiative shocks create environments for dust formation in classical novae
Classical novae commonly show evidence of rapid dust formation within months of the outburst. However, it is unclear how molecules and grains are able to condense within the ejecta, given theExpand


Shaping of nova remnants by binary motion
We present the results of 2.5D hydrodynamic calculations of the effects of the underlying binary system on shaping the ejecta in a classical nova outburst. In the model, the outburst takes place inExpand
Local thermonuclear runaways among classical novae
A classical nova may accrete a non-homogeneousenvelope, which can result in the ignition of a local thermonuclear runaway on the surface of the white dwarf. We studied the propagation of thermalExpand
From multi-epoch adaptive optics imaging and integral field unit spectroscopy, we report the discovery of an expanding and narrowly confined bipolar shell surrounding the helium nova V445 PuppisExpand
Nova outbursts on rotating oblate white dwarfs
A novel hypothesis is proposed in which the prolate geometry and latitudinal abundance gradients observed in nova ejecta are simultaneously explained as a natural consequence of the rotation andExpand
The 2011 outburst of the recurrent nova T Pyxidis. Evidence for a face-on bipolar ejection
We report on near-IR interferometric observations of the outburst of the recurrent nova T Pyx. We obtained near-IR observations of T Pyx at dates ranging from t=2.37d to t=48.2d after the outburst,Expand
The expanding dusty bipolar nebula around the nova V1280 Scorpi
V1280 Sco is one of the slowest dust-forming nova ever historically observed. We performed multi-epoch high-spatial resolution observations of the circumstellar dusty environment of V1280 Sco toExpand
The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst - I. The optically thick phase and the origin of moving lines in novae
Aims. We aim to derive the physical properties of the recurrent nova T Pyx and the structure of the ejecta during the early stages of expansion of the 2011 outburst. Methods. The nova was observedExpand
The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst. II.The optically thin phase and the structure of the ejecta in recurrent novae
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. The nova wasExpand
On the asphericity of nova remnants caused by rotating white dwarf envelopes
The effect of rotating white dwarf envelopes in determining the structure of nova shells is examined. This is achieved by numerical hydrodynamic simulations of the flows around a binary star system.Expand
Near-infrared studies of V1280 Sco (Nova Scorpii 2007)
We present spectroscopic and photometric results of Nova V1280 Sco which was discovered in outburst in early 2007 February. The large number of spectra obtained of the object leads to one of the mostExpand