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 S. 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 P. K. Banerjee and Nagarhalli M. Ashok and Vishal 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… 

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. The

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.

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)

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 mass

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 classical


The recurrent symbiotic nova V745 Sco exploded on 2014 February 6 and was observed on February 22 and 23 by the Chandra X-ray Observatory Transmission Grating Spectrometers. By that time the


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 the

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 at

High spectral resolution monitoring of Nova V339 Delphini with TIGRE

Aims. We investigate the early development of the classical nova V339 Del (Nova Delphini 2013) through high-resolution optical spectroscopy. To study the structure of the ejecta, we focus on the

Physics of nova outbursts: A theoretical model of classical nova outbursts with self-consistent wind mass loss

We present a model for one cycle of a classical nova outburst based on a self-consistent wind mass loss accelerated by the gradient of radiation pressure, i.e., so-called optically thick winds.



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 in

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 thermal


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 Puppis

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 and

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,

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 to

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 observed

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.

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 most

A unified model for the spectrophotometric development of classical and recurrent novae - The role of asphericity of the ejecta

There is increasing evidence that the geometry, and not only the filling factors, of nova ejecta is important in any interpretation of their spectral and photometric developments. Ensembles of