Binary orbits as the driver of γ-ray emission and mass ejection in classical novae

  title={Binary orbits as the driver of $\gamma$-ray emission and mass ejection in classical novae},
  author={Laura B. Chomiuk and Justin D. Linford and Jun Yang and T. J. O’brien and Zsolt Paragi and Amy J. Mioduszewski and R. J. Beswick and C. C. Cheung and Koji Mukai and Thomas J. Nelson and Val{\'e}rio A. R. M. Ribeiro and Michael P. Rupen and J. L. Sokoloski and Jennifer Weston and Yong-gang Zheng and Michael F. Bode and S. P. S. Eyres and Nirupam Roy and Gregory B. Taylor},
Classical novae are the most common astrophysical thermonuclear explosions, occurring on the surfaces of white dwarf stars accreting gas from companions in binary star systems. Novae typically expel about 10−4 solar masses of material at velocities exceeding 1,000 kilometres per second. However, the mechanism of mass ejection in novae is poorly understood, and could be dominated by the impulsive flash of thermonuclear energy, prolonged optically thick winds or binary interaction with the nova… 

Direct evidence for shock-powered optical emission in a nova

Classical novae are thermonuclear explosions that occur on the surfaces of white dwarf stars in interacting binary systems 1 . It has long been thought that the luminosity of classical novae is

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

Gamma-ray novae as probes of relativistic particle acceleration at non-relativistic shocks

The Fermi LAT discovery that classical novae produce >100 MeV gamma-rays establishes that shocks and relativistic particle acceleration are key features of these events. These shocks are likely to be

X-ray evolution of the nova V959 Mon suggests a delayed ejection and a non-radiative shock

X-ray observations of shocked gas in novae can provide a useful probe of the dynamics of the ejecta. Here we report on X-ray observations of the nova V959 Mon, which was also detected in GeV

Gamma-ray emission from internal shocks in novae

Gamma-ray emission at energies >100MeV has been detected from nine novae using the Fermi-LAT, and it can be explained by particle acceleration at shocks in these systems. Eight out of these nine

Shocks in nova outflows. II. Synchrotron radio emission

The discovery of GeV gamma-rays from classical novae indicates that shocks and relativistic particle acceleration are energetically key in these events. Further evidence for shocks comes from thermal

Novae as Tevatrons: prospects for CTA and IceCube

The discovery of novae as sources of ~GeV gamma-rays highlights the key role of shocks and relativistic particle acceleration in these transient systems. Although there is evidence for a spectral

Non-thermal radio emission from colliding flows in classical nova V1723 Aql

The importance of shocks in nova explosions has been highlighted by Fermi's discovery of \gamma-ray producing novae. Over three years of multi-band VLA radio observations of the 2010 nova V1723 Aql

NuSTAR Detection of X-Rays Concurrent with Gamma-Rays in the Nova V5855 Sgr

We report the first detection of hard (>10 keV) X-ray emission simultaneous with gamma-rays in a nova eruption. Observations of the nova V5855 Sgr carried out with the NuSTAR satellite on Day 12 of



Gamma-ray emission concurrent with the nova in the symbiotic binary V407 Cygni.

This work reports the Fermi Large Area Telescope detection of variable gamma-ray emission from the recently detected optical nova of the symbiotic star V407 Cygni and proposes that the material of the nova shell interacts with the dense ambient medium of the red giant primary and that particles can be accelerated effectively to produce pi(0) decay gamma-rays from proton-proton interactions.

Uncovering the Nature of Nova Jets: A Radio Image of Highly Collimated Outflows from RS Ophiuchi

Novae occur when hydrogen-rich fuel provided by a companion star ignites on the surface of a white dwarf (WD). Although the surface of the WD is nearly spherical, observations indicate that at least

Fermi Establishes Classical Novae as a Distinct Class of Gamma-ray Sources

A classical nova results from runaway thermonuclear explosions on the surface of a white dwarf that accretes matter from a low-mass main-sequence stellar companion. In 2012 and 2013, three novae were

An asymmetric shock wave in the 2006 outburst of the recurrent nova RS Ophiuchi

The detection of spatially resolved structure in RS Ophiuchi from two weeks after its 12 February 2006 outburst is reported, producing a remnant similar to that of a type II supernova but evolving over months rather than millennia.

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

The radio and X-ray emission from type II supernovae.

The interaction of the outer parts of a supernova envelope with circumstellar matter gives rise to a high-energy density shell. The equation of motion of the shell is deduced based on the


Nova Monocerotis 2012 is the third γ-ray transient identified with a thermonuclear runaway on a white dwarf, that is, a nova event. Swift monitoring has revealed the distinct evolution of the harder

Novae as a Class of Transient X-Ray Sources

Motivated by the recently discovered class of faint (1034-1035 ergs s−1) X-ray transients in the Galactic center region, we investigate the 2-10 keV properties of classical and recurrent novae.

Nucleosynthesis in Classical Novae and Its Contribution to the Interstellar Medium

Classical novae, explosions that result from thermonuclear runaways (TNRs) on the surfaces of white dwarfs (WDs) accreting hydrogen‐rich matter in close binary systems, are sporadically injecting

Gamma-ray binaries and related systems

After initial claims and a long hiatus, it is now established that several binary stars emit high- (0.1–100 GeV) and very high-energy (>100 GeV) gamma rays. A new class has emerged called “gamma-ray