Lunar Parallax Method of Astro Navigation

TeV neutrinos and gamma-rays from pulsars

“…Though there are about 1800 pulsars known through radio detections, only a few have been detected in the gamma-rays. From observations made with gamma-ray telescopes on satellites so far, only seven high-confidence gamma-ray pulsars are known in the energy range up to a few GeV (Thompson 2003). Besides, three other pulsars (PSR B1046−58, B0656+14 and J0218+4232) are considered to be gamma-ray emitters with a lower confidence level (Thompson 2003) in the same energy region.…”

“…From observations made with gamma-ray telescopes on satellites so far, only seven high-confidence gamma-ray pulsars are known in the energy range up to a few GeV (Thompson 2003). Besides, three other pulsars (PSR B1046−58, B0656+14 and J0218+4232) are considered to be gamma-ray emitters with a lower confidence level (Thompson 2003) in the same energy region. Some basic properties of the high-confidence young gamma-ray pulsars, namely distance (D), spin-down age, period (P), the calculated magnetic field strength at the neutron star surface, surface temperature and pulsar duty cycle (f b ), are listed in Table 1.…”

Toward a standard model of core collapse supernovae

“…In this region, the radiation and electron components of the LS EOS are used, while an ideal gas of 28 Si is assumed for the nuclear component. For typical hydrodynamic timesteps (∼ .1 millisecond), silicon burning occurs within a single timestep for T ∼ 5 GK [26]; therefore, when a fluid element exceeds a temperature of 5 GK in our simulation, the silicon is instantaneously burned, achieving NSE and releasing thermal energy equal to the difference in nuclear binding energy between 28 Si and the composition determined by the LS EOS. Figure 1, taken from the simulation of Mezzacappa et al [27], shows the radius-versus-time trajectories of equal mass (0.01M ⊙ ) shells in the stellar iron core and silicon layer in a Newtonian simulation initiated from the 13 M ⊙ progenitor.…”

“…Given the outcome of these numerical experiments, the fundamental assumption made by Wilson et al should be reexamined. However, it is also important to note that the equilibration experiments carried out by Bruenn and Dineva have to be repeated in light of energy exchange channels between the muon and tau neutrinos and the stellar core matter that have recently been identified (e.g., see the contribution by Thompson and Burrows in this volume [28]). …”

Simulations of stellar core collapse, bounce, and postbounce evolution with Boltzmann neutrino transport, and implications for the core collapse supernova mechanism

“…Given the outcome of these numerical experiments, the fundamental assumption made by Wilson et al should be reexamined. However, it is also important to note that the equilibration experiments carried out by Bruenn and Dineva have to be repeated in light of energy exchange channels between the muon and tau neutrinos and the stellar core matter that have recently been identified [15].…”