Interacting Binary Star System Activity
... types of variable stars. Some are single stars that vary in brightness due to the point in stellar evolution that they are at, exploding, or because they have become unstable brightening and dimming as they literally change size. Some variable stars are really part of a pair of stars that change bri ...
... types of variable stars. Some are single stars that vary in brightness due to the point in stellar evolution that they are at, exploding, or because they have become unstable brightening and dimming as they literally change size. Some variable stars are really part of a pair of stars that change bri ...
Studying explosive phenomena in astrophysics by the example of
... The formation of the first stars hundreds of millions of years after the Big-Bang marks the end of the so-called Dark Ages. Currently, we have no direct observations on how the primordial stars (Population III stars) formed, but according to modern theory of stellar evolution these stars should be v ...
... The formation of the first stars hundreds of millions of years after the Big-Bang marks the end of the so-called Dark Ages. Currently, we have no direct observations on how the primordial stars (Population III stars) formed, but according to modern theory of stellar evolution these stars should be v ...
The Capabilities and Applications of FY
... Color versions of one or more of the figures in this paper are available online at http://ieeexplore.ieee.org. Digital Object Identifier 10.1109/TGRS.2012.2207388 ...
... Color versions of one or more of the figures in this paper are available online at http://ieeexplore.ieee.org. Digital Object Identifier 10.1109/TGRS.2012.2207388 ...
Observational Evidence for Dark Matter Simona Murgia, SLAC-KIPAC XXXIX SLAC Summer Institute
... (protons and electron form neutral hydrogen and become transparent to photons, ~100,000s years after Big Bang, ~ eV) Universe was isotropic and homogeneous at large scales Very small temperature fluctuations, too small to evolve into structure observed today T = 2.725 K ➡ Require additional matter t ...
... (protons and electron form neutral hydrogen and become transparent to photons, ~100,000s years after Big Bang, ~ eV) Universe was isotropic and homogeneous at large scales Very small temperature fluctuations, too small to evolve into structure observed today T = 2.725 K ➡ Require additional matter t ...
Chemical Signatures in Dwarf Galaxies
... those that form through a-captures during nucleosynthesis (i.e., the capture of a helium nucleus, e.g., oxygen, magnesium, silicon, calcium, during quiescent helium burning in the core of massive stars). Thus the alpha/iron ratio is similar to examining the yields from hydrostatic burning in massive ...
... those that form through a-captures during nucleosynthesis (i.e., the capture of a helium nucleus, e.g., oxygen, magnesium, silicon, calcium, during quiescent helium burning in the core of massive stars). Thus the alpha/iron ratio is similar to examining the yields from hydrostatic burning in massive ...
Atmospheric Abundances of Light Elements in the F
... and Martin Laming (1995). Most of the gf values for each line were taken from the The equivalent widths of the absorption lines for light metals were measured using an IRAF routine splot We literature. When reliable data were not available, solar also measured the Fel lines in order to utilize them ...
... and Martin Laming (1995). Most of the gf values for each line were taken from the The equivalent widths of the absorption lines for light metals were measured using an IRAF routine splot We literature. When reliable data were not available, solar also measured the Fel lines in order to utilize them ...
NATS 1311 From the Cosmos to Earth
... appeared as a bright point of light; it appears larger than a point in the photograph only because of overexposure. ...
... appeared as a bright point of light; it appears larger than a point in the photograph only because of overexposure. ...
Galaxy Formation, Theory and Modelling
... results for datasets with different luminosity and colour selections. ...
... results for datasets with different luminosity and colour selections. ...
Properties of Stars Measuring Stars Apparent Magnitude, m Range
... 120,000 stars. (0.001" is the angular size of a golf ball at the other side of the Atlantic) ...
... 120,000 stars. (0.001" is the angular size of a golf ball at the other side of the Atlantic) ...
Lecture 2. Isolated Neutron Stars – I.
... Then using there average lifetime we can estimate the birth rate and total numbers (with a given age of the Galaxy and assuming constant rate) taking into account SFR~3 solar mass per year. [see also Ch.1 in Shapiro, Teukolsky] ...
... Then using there average lifetime we can estimate the birth rate and total numbers (with a given age of the Galaxy and assuming constant rate) taking into account SFR~3 solar mass per year. [see also Ch.1 in Shapiro, Teukolsky] ...
Ch 32) Elementary Particles
... In the late 1940s, after World War II, it was found that if the incoming particle in a nuclear reaction (Section 31–1) has sufficient energy, new types of particles can be produced. The earliest experiments used cosmic rays—particles that impinge on the Earth from space. In the laboratory, various t ...
... In the late 1940s, after World War II, it was found that if the incoming particle in a nuclear reaction (Section 31–1) has sufficient energy, new types of particles can be produced. The earliest experiments used cosmic rays—particles that impinge on the Earth from space. In the laboratory, various t ...
High Energy Emission From Pulsar Wind Nebulae • What`s new in
... 5 ms (dashed curves) and 20 ms (full curves). The initial expansion velocity of the nebula is 2 × 108 cm s−1 and its mass is 4 M and the density of surrounding medium is 0.3 cm−3. (B) The expansion velocity of the nebula (thick curves) and the strength of the magnetic field at the shock region (thi ...
... 5 ms (dashed curves) and 20 ms (full curves). The initial expansion velocity of the nebula is 2 × 108 cm s−1 and its mass is 4 M and the density of surrounding medium is 0.3 cm−3. (B) The expansion velocity of the nebula (thick curves) and the strength of the magnetic field at the shock region (thi ...
atmospheric extinction
... occurs at 912 Å = 13.6 eV At frequencies higher than 13.6 eV part of the X-ray flux is Absorbed, in a frequency-dependent way Morrison & McCammon (1983, ApJ, 270, 119) have computed this dependence in the 0.03 - 10 keV energy interval, taking into account cosmic abundances ...
... occurs at 912 Å = 13.6 eV At frequencies higher than 13.6 eV part of the X-ray flux is Absorbed, in a frequency-dependent way Morrison & McCammon (1983, ApJ, 270, 119) have computed this dependence in the 0.03 - 10 keV energy interval, taking into account cosmic abundances ...
Atomic Structure
... theory of the atom. This later became known as Dalton’s atomic theory. The general tenets of this theory were as follows: 1. All matter is composed of extremely small particles called atoms. 2. Atoms of a given element are identical in size, mass, and other properties. Atoms of different elements di ...
... theory of the atom. This later became known as Dalton’s atomic theory. The general tenets of this theory were as follows: 1. All matter is composed of extremely small particles called atoms. 2. Atoms of a given element are identical in size, mass, and other properties. Atoms of different elements di ...
Cooling neutron stars: Theory and observations
... seems to be <= 1/30 of modified Urca • Coldest observed stars are more massive; their neutrino luminosity should be > 30 of modified Urca (any enhanced neutrino emission would do) • Neutron star masses at which neutrino cooling is enhanced are not constrained • The real physical model of neutron sta ...
... seems to be <= 1/30 of modified Urca • Coldest observed stars are more massive; their neutrino luminosity should be > 30 of modified Urca (any enhanced neutrino emission would do) • Neutron star masses at which neutrino cooling is enhanced are not constrained • The real physical model of neutron sta ...
Stellar Remnants White Dwarfs Type Ia Supernovae Neutron Stars
... © 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley ...
... © 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley ...
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.