The Big Bang Theory:
... D = distance of galaxy to earth • Galaxies are getting farther apart as time progresses, therefore the universe is expanding. – Not only is it expanding… it’s accelerating! ...
... D = distance of galaxy to earth • Galaxies are getting farther apart as time progresses, therefore the universe is expanding. – Not only is it expanding… it’s accelerating! ...
Stars, Galaxies, and the Universe
... • A white dwarf is is a star that has used up all of its hydrogen and is the leftover center of an older star. • Class F stars are yellow-white • The majority of stars in our galaxy are main sequence stars. ...
... • A white dwarf is is a star that has used up all of its hydrogen and is the leftover center of an older star. • Class F stars are yellow-white • The majority of stars in our galaxy are main sequence stars. ...
The Milky Way Galaxy
... 2) Isotropic: In general, the universe looks the same in every direction (applies to expansion). ...
... 2) Isotropic: In general, the universe looks the same in every direction (applies to expansion). ...
History of the universe timeline
... from our tiny, home planet, Earth. The visible Universe contains billions of galaxies, each comprising billions of stars. Within our own Galaxy, hundreds of exoplanets have been discovered orbiting other stars. ...
... from our tiny, home planet, Earth. The visible Universe contains billions of galaxies, each comprising billions of stars. Within our own Galaxy, hundreds of exoplanets have been discovered orbiting other stars. ...
ExpandUniv
... helps to get rid of some spatial dimensions, and keep time as a shown dimension. Here is a diagram with only 2 dimensions, one space and one time. Light is the fastest thing in it, and marks out “lightcones” which determine what can be seen, and when. An object’s existence is a “worldline”. ...
... helps to get rid of some spatial dimensions, and keep time as a shown dimension. Here is a diagram with only 2 dimensions, one space and one time. Light is the fastest thing in it, and marks out “lightcones” which determine what can be seen, and when. An object’s existence is a “worldline”. ...
AY5 Homework for Quiz 4: Spring 2015
... __X__ it is “cold” (i.e. moves slowly compared to the speed of light) __X__ it does not readily interact directly with photons or other matter (i.e. it has a small cross-‐section for interations) _ ...
... __X__ it is “cold” (i.e. moves slowly compared to the speed of light) __X__ it does not readily interact directly with photons or other matter (i.e. it has a small cross-‐section for interations) _ ...
Deep Space and Solar System
... • One light year is how far light travels in one year (based on distance NOT time) • We see all night stars as they were when the light we see left each star ...
... • One light year is how far light travels in one year (based on distance NOT time) • We see all night stars as they were when the light we see left each star ...
document
... NUCLEOSYNTHESIS ENDED AT THIS POINT. A CLOUD OF NUCLEI, ELECTRONS, PROTONS, AND PHOTONS EXISTED AT THIS POINT - A ...
... NUCLEOSYNTHESIS ENDED AT THIS POINT. A CLOUD OF NUCLEI, ELECTRONS, PROTONS, AND PHOTONS EXISTED AT THIS POINT - A ...
THE HISTORY OF THE UNIVERSE IN ONE EASY LESSON
... NUCLEOSYNTHESIS ENDED AT THIS POINT. A CLOUD OF NUCLEI, ELECTRONS, PROTONS, AND PHOTONS EXISTED AT THIS POINT - A PLASMA. ...
... NUCLEOSYNTHESIS ENDED AT THIS POINT. A CLOUD OF NUCLEI, ELECTRONS, PROTONS, AND PHOTONS EXISTED AT THIS POINT - A PLASMA. ...
ASTR100 Class 01 - University of Maryland Department of
... 2. Why is the overall distribution of matter so uniform? 3. Why is the density of the universe so close to the critical density? That is, why does the universe have such a flat geometry? An early episode of rapid inflation can ...
... 2. Why is the overall distribution of matter so uniform? 3. Why is the density of the universe so close to the critical density? That is, why does the universe have such a flat geometry? An early episode of rapid inflation can ...
IOSR Journal of Applied Physics (IOSR-JAP) ISSN: 2278-4861.
... After the super-explosion (The Big-Bang), according to the nebula hypothesis [1], the solar system began as a nebula, an area in the Milky Way Galaxy that was a swirling concentration of cold gas and dust. Due to some perturbation, possibly from the nearby supernova this cloud of gas and dust began ...
... After the super-explosion (The Big-Bang), according to the nebula hypothesis [1], the solar system began as a nebula, an area in the Milky Way Galaxy that was a swirling concentration of cold gas and dust. Due to some perturbation, possibly from the nearby supernova this cloud of gas and dust began ...
The homogeneous and isotropic universe: Cosmology
... Edwin Hubble showed in 1929 that all the galaxies are moving away from us with a velocity v = H0r Not really a constant! This does not break the cosmological principle [imagine baking a cake with raisins in it] ...
... Edwin Hubble showed in 1929 that all the galaxies are moving away from us with a velocity v = H0r Not really a constant! This does not break the cosmological principle [imagine baking a cake with raisins in it] ...
The Universe
... an incredibly small area. The gravitational pull of this region is so great that nothing can escape – not even light. Although black holes cannot be seen, we know they exist from the way they affect nearby dust, stars and galaxies. Many of them are surrounded by discs of material. As the discs swirl ...
... an incredibly small area. The gravitational pull of this region is so great that nothing can escape – not even light. Although black holes cannot be seen, we know they exist from the way they affect nearby dust, stars and galaxies. Many of them are surrounded by discs of material. As the discs swirl ...
Olbers` Paradox
... change position; there is no preferred position in the universe (translational invariance) • Isotropic -> no difference when we look at a different direction • Examples: Surface of uniform cylinder is homogeneous but not isotropic- what about the surface of a sphere – or chessboard ? • Cosmological ...
... change position; there is no preferred position in the universe (translational invariance) • Isotropic -> no difference when we look at a different direction • Examples: Surface of uniform cylinder is homogeneous but not isotropic- what about the surface of a sphere – or chessboard ? • Cosmological ...
24.1 The Study of Light
... dough doubles in size, so does the distance between all the raisins. Those objects located father apart move away from each other more rapidly. ...
... dough doubles in size, so does the distance between all the raisins. Those objects located father apart move away from each other more rapidly. ...
Shape of the universe
The shape of the universe is the local and global geometry of the Universe, in terms of both curvature and topology (though, strictly speaking, the concept goes beyond both). The shape of the universe is related to general relativity which describes how spacetime is curved and bent by mass and energy.There is a distinction between the observable universe and the global universe. The observable universe consists of the part of the universe that can, in principle, be observed due to the finite speed of light and the age of the universe. The observable universe is understood as a sphere around the Earth extending 93 billion light years (8.8 *1026 meters) and would be similar at any observing point (assuming the universe is indeed isotropic, as it appears to be from our vantage point).According to the book Our Mathematical Universe, the shape of the global universe can be explained with three categories: Finite or infinite Flat (no curvature), open (negative curvature) or closed (positive curvature) Connectivity, how the universe is put together, i.e., simply connected space or multiply connected.There are certain logical connections among these properties. For example, a universe with positive curvature is necessarily finite. Although it is usually assumed in the literature that a flat or negatively curved universe is infinite, this need not be the case if the topology is not the trivial one.The exact shape is still a matter of debate in physical cosmology, but experimental data from various, independent sources (WMAP, BOOMERanG and Planck for example) confirm that the observable universe is flat with only a 0.4% margin of error. Theorists have been trying to construct a formal mathematical model of the shape of the universe. In formal terms, this is a 3-manifold model corresponding to the spatial section (in comoving coordinates) of the 4-dimensional space-time of the universe. The model most theorists currently use is the so-called Friedmann–Lemaître–Robertson–Walker (FLRW) model. Arguments have been put forward that the observational data best fit with the conclusion that the shape of the global universe is infinite and flat, but the data are also consistent with other possible shapes, such as the so-called Poincaré dodecahedral space and the Picard horn.