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Interaction of Type Ia Supernovae with Their Surroundings
Type Ia supernovae (SNe) are presumed to arise from white dwarf progenitors, which may not appreciably modify their ambient medium. We study the interaction of the resulting supernova remnants with a
SN 2013ej - A type IIL supernova with weak signs of interaction
We present optical photometric and spectroscopic observations of supernova 2013ej. It is one of the brightest type II supernovae exploded in a nearby ($\sim 10$ Mpc) galaxy NGC 628. The light curve
Science with the Cherenkov Telescope Array
The Cherenkov Telescope Array, CTA, will be the major global observatory for very high energy gamma-ray astronomy over the next decade and beyond. The scientific potential of CTA is extremely broad:
The Presupernova H II Region around SN 1987A
The slow expansion of the bright ring around SN 1987A and the large size estimated for the radio source at an age of ~1500 days suggest a low mass-loss rate, , from the blue supergiant progenitor
The Evolution of Supernovae in Circumstellar Wind-Blown Bubbles. I. Introduction and One-Dimensional Calculations
Mass loss from massive stars (8 M☉) can result in the formation of circumstellar wind-blown cavities surrounding the star, bordered by a thin, dense, cold shell. When the star explodes as a
The evolution of supernovae in circumstellar wind bubbles. II. Case of a wolf-rayet star
Mass loss from massive stars leads to the formation of circumstellar wind-blown bubbles surrounding the star, bordered by a dense shell. When the star ends its life in a supernova (SN) explosion, the
We present very high energy (VHE) imaging of MGRO J2019+37 obtained with the VERITAS observatory. The bright extended (~2°) unidentified Milagro source is located toward the rich star formation
What are published X-ray light curves telling us about young supernova expansion?
Massive stars lose mass in the form of stellar winds and outbursts. This material accumulates around the star. When the star explodes as a supernova the resulting shock wave expands within this
Discovery of TeV gamma-ray emission toward supernova remnant SNR G78.2+2.1
We report the discovery of an unidentified, extended source of very-high-energy gamma-ray emission, VER J2019+407, within the radio shell of the supernova remnant SNR G78.2+2.1, using 21.4 hr of data
Gamma-Ray Observations of Tycho’s Supernova Remnant with VERITAS and $Fermi$
High-energy gamma-ray emission from supernova remnants (SNRs) has provided a unique perspective for studies of Galactic cosmic-ray acceleration. Tycho’s SNR is a particularly good target because it