Astronomy, Astrophysics, and Cosmology
... Stars are born when gaseous clouds (mostly hydrogen) contract due to pull of gravity Huge gas cloud fragments into numerous contracting masses Each mass is centered in area where density is only slightly greater than @ nearby points Once such “globules” formed gravity would cause each to contract in ...
... Stars are born when gaseous clouds (mostly hydrogen) contract due to pull of gravity Huge gas cloud fragments into numerous contracting masses Each mass is centered in area where density is only slightly greater than @ nearby points Once such “globules” formed gravity would cause each to contract in ...
When Stars Attack! In Search of Killer Supernovae
... In our Milky Way galaxy: Ø About 1 SN/century Ø Most far away: spectacular but ...
... In our Milky Way galaxy: Ø About 1 SN/century Ø Most far away: spectacular but ...
transparencies - Rencontres de Blois
... Distribution of baryons determines the distribution of dark matter-Halo with structure. ...
... Distribution of baryons determines the distribution of dark matter-Halo with structure. ...
Lecture 2. Isolated Neutron Stars – I.
... the part of the problem was his personality, which implied strongly that people were idiots if they did not believe in neutron stars.” ...
... the part of the problem was his personality, which implied strongly that people were idiots if they did not believe in neutron stars.” ...
Neutron Stars
... Notice that in this case the mass density ρ = n /c 2 is due entirely to neutrons and greatly exceeds ρ0 whenever the neutrons are extremely relativistic. ...
... Notice that in this case the mass density ρ = n /c 2 is due entirely to neutrons and greatly exceeds ρ0 whenever the neutrons are extremely relativistic. ...
Bob Mathieu (Wisconsin) – Observations of Open Clusters
... Optimal Cluster Properties (with an observational bias) • Rich several thousand members to 0.1 Mo • evolution without complete evaporation • meaningful statistics • “Old” age greater than 1 Gyr • multiple relaxation times • solar-mass evolution • “Nearby” d < 2 kpc • accessible main-sequence binary ...
... Optimal Cluster Properties (with an observational bias) • Rich several thousand members to 0.1 Mo • evolution without complete evaporation • meaningful statistics • “Old” age greater than 1 Gyr • multiple relaxation times • solar-mass evolution • “Nearby” d < 2 kpc • accessible main-sequence binary ...
chemical abundances for a-and f-type supergiant stars
... eventually evolve back into a blue supergiant phase (Walmswell et al. 2015). During the red supergiant phase, the convective zone mixes materials of the H-burning shell, which are subsequently released to the surface by the 1DUP event, causing changes in the observed CNO abundance patterns. The amou ...
... eventually evolve back into a blue supergiant phase (Walmswell et al. 2015). During the red supergiant phase, the convective zone mixes materials of the H-burning shell, which are subsequently released to the surface by the 1DUP event, causing changes in the observed CNO abundance patterns. The amou ...
Slide 1
... hundred pulses and this is very uniform. But individual component pulses or subpulses can be very different from one another, varying in intensity, shape and in the phase at which they occur within the integrated profile. The figure shows a sequence of pulses in time compared to the average envelope ...
... hundred pulses and this is very uniform. But individual component pulses or subpulses can be very different from one another, varying in intensity, shape and in the phase at which they occur within the integrated profile. The figure shows a sequence of pulses in time compared to the average envelope ...
Slide 1
... SNO+ can detect the huge burst of neutrinos which comes from a supernova – the collapse and explosion of a massive star – in our galaxy. Analysis of these neutrinos will add much to the understanding of these important astrophysical processes and provide a glimpse at neutrino properties (neutrino ma ...
... SNO+ can detect the huge burst of neutrinos which comes from a supernova – the collapse and explosion of a massive star – in our galaxy. Analysis of these neutrinos will add much to the understanding of these important astrophysical processes and provide a glimpse at neutrino properties (neutrino ma ...
The ISO–SWS Spectrum of Planetary Nebula NGC 7027
... In Table 2.2 the fluxes measured for the infrared (IR) lines are listed. In total around 80 lines were measured. Calibration errors are larger at longer wavelengths but on average amount to about 20%. Random measurement errors depend on the flux strength: weak lines (I < 5, where I is in 10−12 erg c ...
... In Table 2.2 the fluxes measured for the infrared (IR) lines are listed. In total around 80 lines were measured. Calibration errors are larger at longer wavelengths but on average amount to about 20%. Random measurement errors depend on the flux strength: weak lines (I < 5, where I is in 10−12 erg c ...
Pair instability supernovae: Evolution, explosion, nucleosynthesis
... supernovae are exploding in the visible Universe each second, and at present there are a few of them discovered every day. The average peak luminosity of a supernova competes with that of entire galaxies. Supernovae are the main contributor of heavy elements, energy and momentum to the interstellar ...
... supernovae are exploding in the visible Universe each second, and at present there are a few of them discovered every day. The average peak luminosity of a supernova competes with that of entire galaxies. Supernovae are the main contributor of heavy elements, energy and momentum to the interstellar ...
Origin of close binary systems
... - example: the multiplicities of the Orion Trapezium stars and the companion star frequency of high-mass vs. low-mass stars - SPH simulations: hierarchical star cluster formation and the merging of subclusters as a model for the origin of Trapezia - origin due to formation or early dynamical N-body ...
... - example: the multiplicities of the Orion Trapezium stars and the companion star frequency of high-mass vs. low-mass stars - SPH simulations: hierarchical star cluster formation and the merging of subclusters as a model for the origin of Trapezia - origin due to formation or early dynamical N-body ...
Chapter 2
... • Energy from Big Bang transformed into matter (more details of this matter/energy relationship in Chapter 21). • Fusing of fundamental/subatomic particles (protons/neutrons) created atomic nuclei. ...
... • Energy from Big Bang transformed into matter (more details of this matter/energy relationship in Chapter 21). • Fusing of fundamental/subatomic particles (protons/neutrons) created atomic nuclei. ...
The Secrets of Cosmic Grains - Max-Planck
... the matrix of the meteoritic rock. Some of the isotopes in these grains exhibit dramatic, distinctive features. Investigations by Peter Hoppe, also from the Max Planck Institute for Chemistry in Mainz, show that, while the isotope ra- ...
... the matrix of the meteoritic rock. Some of the isotopes in these grains exhibit dramatic, distinctive features. Investigations by Peter Hoppe, also from the Max Planck Institute for Chemistry in Mainz, show that, while the isotope ra- ...
PWFeb13jenkins_PUBLISHED
... Were it not for a particular excited state of the carbon-12 nucleus known as the Hoyle state, the universe would look very different. In particular, there would be essentially no carbon and hence life as we know it would not have evolved, nor would other heavy elements exist. In hindsight, it is rem ...
... Were it not for a particular excited state of the carbon-12 nucleus known as the Hoyle state, the universe would look very different. In particular, there would be essentially no carbon and hence life as we know it would not have evolved, nor would other heavy elements exist. In hindsight, it is rem ...
find - UNAM
... gamma-ray burst would be sufficient to avoid excessive baryon contamination. We find that some mass (of the order of 1023 ±1022 M() may be dynamically ejected from the system, and could thus contribute substantially to the amount of observed r-process material in the galaxy. We calculate the gravita ...
... gamma-ray burst would be sufficient to avoid excessive baryon contamination. We find that some mass (of the order of 1023 ±1022 M() may be dynamically ejected from the system, and could thus contribute substantially to the amount of observed r-process material in the galaxy. We calculate the gravita ...
Concept Tests 16 17
... ConcepTest 16.5c Proton and Electron III A proton and an electron are held apart a distance of 1 m and then let go. Where would they meet? ...
... ConcepTest 16.5c Proton and Electron III A proton and an electron are held apart a distance of 1 m and then let go. Where would they meet? ...
X-ray Sources in Nearby Galaxies Q. Daniel Wang University of Massachusetts
... • Feeding of AGNs • Evolution of HMXBs and LMXBs (talk by Andreas Zezas). • Discrete source populations such as SNe, SNRs, YSOs. • Effects of AGN energy injection, accretion from the IGM, clustering environment on diffuse hot plasma. • Diffuse hard X-rays: e.g., reflection, inverse Compton scat ...
... • Feeding of AGNs • Evolution of HMXBs and LMXBs (talk by Andreas Zezas). • Discrete source populations such as SNe, SNRs, YSOs. • Effects of AGN energy injection, accretion from the IGM, clustering environment on diffuse hot plasma. • Diffuse hard X-rays: e.g., reflection, inverse Compton scat ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.