Getting to know classical novae with Swift

  title={Getting to know classical novae with Swift},
  author={Julian P. Osborne},
  journal={Journal of High Energy Astrophysics},
  • J. Osborne
  • Published 8 July 2015
  • Physics
  • Journal of High Energy Astrophysics
Supersoft X-Ray Sources Identified with Be Binaries in the Magellanic Clouds
We investigated four luminous supersoft X-ray sources (SSS) in the Magellanic Clouds suspected to have optical counterparts of Be spectral type. If the origin of the X-rays is in a very hot
Surveying the X-Ray Behavior of Novae as They Emit γ-Rays
The detection of GeV γ-ray emission from Galactic novae by the Fermi-Large Area Telescope has become routine since 2010, and is generally associated with shocks internal to the nova ejecta. These
X-Ray Flashes in Recurrent Novae: M31N 2008-12a and the Implications of the Swift Non-detection
Models of nova outbursts suggest that an X-ray flash should occur just after hydrogen ignition. However, this X-ray flash has never been observationally confirmed. We present four theoretical light
The 2019 eruption of recurrent nova V3890 Sgr: observations by Swift, NICER, and SMARTS
V3890 Sgr is a recurrent nova which has been seen in outburst three times so far, with the most recent eruption occurring on 2019 August 27 UT. This latest outburst was followed in detail by the Neil
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
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
Observations of galactic and extragalactic novae
The recent GAIA DR2 measurements of distances to galactic novae have allowed to re-analyse some properties of nova populations in the Milky Way and in external galaxies on new and more solid
High-energy Emission from Nonrelativistic Radiative Shocks: Application to Gamma-Ray Novae
Multiwavelength radiation from relativistic particles accelerated at shocks in novae and other astrophysical sources carries a wealth of information about the outflow properties and the microphysical


Binary orbits as the driver of γ-ray emission and mass ejection in classical novae
High-resolution radio imaging of the γ-ray-emitting nova V959 Mon finds that its ejecta were shaped by the motion of the binary system: some gas was expelled rapidly along the poles as a wind from the white dwarf, while denser material drifted out along the equatorial plane, propelled by orbital motion.
An accreting white dwarf near the Chandrasekhar limit in the andromeda galaxy
The intermediate Palomar Transient Factory (iPTF) detection of the most recent outburst of the recurrent nova (RN) system RX J0045.4+4154 in the Andromeda galaxy has enabled the unprecedented study
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.
Swift Observations of the 2006 Outburst of the Recurrent Nova RS Ophiuchi. I. Early X-Ray Emission from the Shocked Ejecta and Red Giant Wind
RS Ophiuchi began its latest outburst on 2006 February 12. Previous outbursts have indicated that high-velocity ejecta interact with a preexisting red giant wind, setting up shock systems analogous
X-Ray Emission from an Asymmetric Blast Wave and a Massive White Dwarf in the Gamma Ray Emitting Nova V407 CYG
Classical nova events in symbiotic stars, although rare, offer a unique opportunity to probe the interaction between ejecta and a dense environment in stellar explosions. In this work, we use X-ray
An X-ray-emitting blast wave from the recurrent nova RS Ophiuchi
The early onset of deceleration indicates that the ejected shell had a low mass, the white dwarf has a high mass, and that RS Ophiuchi is therefore a progenitor of the type of supernova (type Ia) integral to studies of the expansion of the Universe.
Following the Swift X-ray observations of the 2006 outburst of the recurrent nova RS Ophiuchi, we developed hydrodynamical models of mass ejection from which the forward shock velocities were used to
Swift observations of 52 Galactic/Magellanic Cloud novae are presented indicating that additional factors beyond the white dwarf mass and binary separation play important roles in the evolution of a nova outburst and two optical phenomena are confirmed that are correlated with strong, soft X-ray emission which can be used to further increase the efficiency ofX-ray campaigns.
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
Swift observations of the X-ray and UV evolution of V2491 Cyg (Nova Cyg 2008 No. 2)
Observing the X-ray emission from only one day after the nova discovery, the source is followed through the initial brightening, the super-soft source phase and back to the pre-outburst flux level, demonstrating the evolution of the spectrum throughout the outburst.