We analyze the confining effect of cloud collapse on an expanding supernova shockfront. We solve the differential equation for the forces on the shockfront due to ram pressure, supernova energy, and gravity. We find that the expansion of the shockfront is slowed and in fact reversed by the collapsing cloud. Including radiative losses and a potential time lag between supernova explosion and clou...

From the late 1980s, an opinion exists that the SS arose as a result of interaction between a supernova and a presolar gas–dust cloud. Such a hypothesis is a result of detection of small grains of different chemical compositions with isotopic anomalies in the fine-grained matrix of some primitive meteorites [1]. A number of the researchers believe that the anomalies result from the presolar ori...

Helium star–neutron star binaries are widely believed to be the progenitors of the observed double pulsar systems. In these, the second neutron star is presumed to be the compact remnant of the helium star supernova. Here, the observational implications of such a supernova are discussed, and in particular are explored as a candidate γ-ray burst mechanism. In this scenario the supernova results ...

Wide-field, very long baseline interferometry (VLBI) observations of the nearby starburst galaxy NGC 253, obtained with the Australian Long Baseline Array (LBA), have produced a 2.3 GHz image with a maximum angular resolution of 15 mas (0.3 pc). Six sources were detected, all corresponding to sources identified in higher frequency (> 5 GHz) VLA images. One of the sources, su-pernova remnant 5.4...

Wide-field, very long baseline interferometry (VLBI) observations of the nearby starburst galaxy NGC 253, obtained with the Australian Long Baseline Array (LBA), have produced a 2.3 GHz image with a maximum angular resolution of 15 mas (0.3 pc). Six sources were detected, all corresponding to sources identified in higher frequency (> 5 GHz) VLA images. One of the sources, su-pernova remnant 5.4...

We use the HST ACS imaging of the two GOODS fields during Cycles 11, 12, and 13 to derive the Type Ia supernova rate in four redshift intervals in the range 0.2 < z < 1.8. Compared to our previous results based on Cycle 11 observations only, we have increased the coverage of the search by a factor 2.7, making the total area searched equivalent to one square degree. The sample now consists of 56...

Supernovae are explosions of stars which are triggered either by the implosion of the core of a star or a thermonuclear runaway, causing a bright optical display lasting for weeks to years. This chapter first explains the main explosion types, how they are classified and the principles that determine their lightcurves. It then discusses in more detail some of the most important supernova types,...

Measurements of standard candles and measurements of standard rulers give an inconsistent picture of the history of the universe. This discrepancy can be explained if photon number is not conserved as computations of the luminosity distance must be modified. I show that photon number is not conserved when photons mix with chameleons in the presence of a magnetic field. The strong magnetic field...

A principal ‘supernova neutrino challenge’ is the computational difficulty of six-dimensional neutrino radiation hydrodynamics. The variety of resulting approximations has provoked a long history of uncertainty in the core-collapse supernova explosion mechanism, but recent work highlighting low-mode convection and a newlyrecognized instability in spherical accretion shocks may signal (yet anoth...

We report on Australia Telescope Compact Array observations in the direction of the young high magnetic-Ðeld pulsar J1119[6127. In the resulting images we identify a nonthermal radio shell of diameter 15@, which we classify as a previously uncataloged young supernova remnant, G292.2[0.5. This supernova remnant is positionally coincident with PSR J1119[6127, and we conclude that the two objects ...