Chapter 26: Stars, Galaxies, and the Universe Stars
... To see an example or parallax, try holding your finger about 1 foot (30 cm) in front of your eyes. Now, while focusing on your finger, close one eye and then the other. Alternate back and forth between eyes, and pay attention to how your finger appears to move. The shift in position of your finger ...
... To see an example or parallax, try holding your finger about 1 foot (30 cm) in front of your eyes. Now, while focusing on your finger, close one eye and then the other. Alternate back and forth between eyes, and pay attention to how your finger appears to move. The shift in position of your finger ...
Chapter 4 notes
... • The food Calorie (C) is a unit used by nutritionists to measure how much energy you get from various foods1 C is equivalent to about 4,184 J. • Every gram of fat a person consumes can supply 9 C of energy. • Carbohydrates and proteins each supply about 4 C of energy per gram. ...
... • The food Calorie (C) is a unit used by nutritionists to measure how much energy you get from various foods1 C is equivalent to about 4,184 J. • Every gram of fat a person consumes can supply 9 C of energy. • Carbohydrates and proteins each supply about 4 C of energy per gram. ...
Topics in Early Universe Cosmology
... Chapter 2 and 3 explore bouncing universe models containing fields coming from the Lee-Wick standard model. It was known that these fields could give rise to a non-singular bounce in the matter sector. We showed that this is not the case anymore when we add up gauge fields to the system [20]. First, ...
... Chapter 2 and 3 explore bouncing universe models containing fields coming from the Lee-Wick standard model. It was known that these fields could give rise to a non-singular bounce in the matter sector. We showed that this is not the case anymore when we add up gauge fields to the system [20]. First, ...
The Fundamental Physics of Electromagnetic Waves
... they come to rest … provided the periodic time of the gentle blows is precisely the same as the periodic time of the body’s own vibrations, very large and powerful oscillations may result. But if the periodic time of the regular blows is different from the periodic time of the oscillations, the resu ...
... they come to rest … provided the periodic time of the gentle blows is precisely the same as the periodic time of the body’s own vibrations, very large and powerful oscillations may result. But if the periodic time of the regular blows is different from the periodic time of the oscillations, the resu ...
HON 392 - Chapman University
... The Contemporary Universe (Einstein/Hubble): We live on rotating planet, spinning at about 1000 mph, revolving in its one year long elliptical path around a medium size star--the Sun--at roughly 19 miles per second (67,000 miles per hour). Our Sun and Solar system as a whole--located about 2/3’s fro ...
... The Contemporary Universe (Einstein/Hubble): We live on rotating planet, spinning at about 1000 mph, revolving in its one year long elliptical path around a medium size star--the Sun--at roughly 19 miles per second (67,000 miles per hour). Our Sun and Solar system as a whole--located about 2/3’s fro ...
A100H–Exploring the Universe: Dark Matter, Dark Energy Martin D
... Masses measured from galaxy motions, temperature of hot gas, and gravitational lensing all indicate that the vast majority of matter in clusters is dark ...
... Masses measured from galaxy motions, temperature of hot gas, and gravitational lensing all indicate that the vast majority of matter in clusters is dark ...
astronomy advisory panel strategy
... Understanding the birth of stars is fundamental to astrophysics. Any realistic explanation of the formation and evolution of galaxies requires us to know what determines the rate of star formation, what determines any variation in the mass distribution of stars formed, and what determines the charac ...
... Understanding the birth of stars is fundamental to astrophysics. Any realistic explanation of the formation and evolution of galaxies requires us to know what determines the rate of star formation, what determines any variation in the mass distribution of stars formed, and what determines the charac ...
An analogy
... • What would you like to know about cities? – how does your own city look like? how big is it? what is its population? history? how did it develop? – how does it compare to other cities? is it bigger, smaller? are there many young ...
... • What would you like to know about cities? – how does your own city look like? how big is it? what is its population? history? how did it develop? – how does it compare to other cities? is it bigger, smaller? are there many young ...
Curriculum Vitae - Centre for Astrophysics and Supercomputing
... September 2008 – MPA Cosmology Seminar, Max-Planck-Institute for Astrophysics, Germany November 2007 – Seminar at the Center for Astrophysics of the University of Porto, Portugal ...
... September 2008 – MPA Cosmology Seminar, Max-Planck-Institute for Astrophysics, Germany November 2007 – Seminar at the Center for Astrophysics of the University of Porto, Portugal ...
Cosmological Consequences of Topological Defects
... that any stable lattice of frustrated walls must obey and propose a class of models which, in the limit of large number N of coupled scalar fields, approaches the so-called ‘ideal’ model (in terms of its potential to lead to network frustration). By using the results of the largest and most accurate ...
... that any stable lattice of frustrated walls must obey and propose a class of models which, in the limit of large number N of coupled scalar fields, approaches the so-called ‘ideal’ model (in terms of its potential to lead to network frustration). By using the results of the largest and most accurate ...
Efficiently Extracting Energy from Cosmological
... More recently, there has been interest in the possibility of detecting cosmological neutrinos in beta-decay experiments such as KATRIN and MARE [19, 20]. In these cases the observational signature is a distortion in the energy spectra of the electrons emitted by unstable nuclei that arises because ...
... More recently, there has been interest in the possibility of detecting cosmological neutrinos in beta-decay experiments such as KATRIN and MARE [19, 20]. In these cases the observational signature is a distortion in the energy spectra of the electrons emitted by unstable nuclei that arises because ...
The Big Bang
... • Galaxies “Here and Now” vs. “There and Then” • The “faint blue excess” galaxies • Nature vs. Nurture for establishing galaxy morphology • Active Galaxies and QUASARS ...
... • Galaxies “Here and Now” vs. “There and Then” • The “faint blue excess” galaxies • Nature vs. Nurture for establishing galaxy morphology • Active Galaxies and QUASARS ...
arXiv:1505.07406v1 [hep-ph] 27 May 2015
... The great expectation we have of a quantum theory of gravity is that it will be able to tame the singularities arising in General Relativity. In particular, it should provide us with a consistent, non-singular scenario for the initial stages of our universe. It is hoped that this goal can be achieve ...
... The great expectation we have of a quantum theory of gravity is that it will be able to tame the singularities arising in General Relativity. In particular, it should provide us with a consistent, non-singular scenario for the initial stages of our universe. It is hoped that this goal can be achieve ...
1 Cosmology: a brief refresher course
... • Suppose that ΩΛ = 0. In that case, the value of ΩK depends on the total matter density. If this is greater than the critical density, then ΩK < 0 and hence K > 0; in other words, the Universe is closed. On the other hand, if the total matter density is less than the critical density, then ΩK > 0, ...
... • Suppose that ΩΛ = 0. In that case, the value of ΩK depends on the total matter density. If this is greater than the critical density, then ΩK < 0 and hence K > 0; in other words, the Universe is closed. On the other hand, if the total matter density is less than the critical density, then ΩK > 0, ...
The Cosmological Distance Ladder
... Implications of the Hubble constant Ho is (velocity/distance) so has the dimensions of (1/time). 1/Ho is the expansion age of the universe (how old the Universe would be if no forces acting) = 15.3 billion yrs For simplest model universe with only gravity acting, age of universe would be 10.2 billi ...
... Implications of the Hubble constant Ho is (velocity/distance) so has the dimensions of (1/time). 1/Ho is the expansion age of the universe (how old the Universe would be if no forces acting) = 15.3 billion yrs For simplest model universe with only gravity acting, age of universe would be 10.2 billi ...
The Comprehensible Universe
... during the time and reach of the inflation, ii) expansion of the Universe and in turn formation of galaxies having stars, planets, and other celestial bodies in the reach between outer boundary of the inflation and the South Pole of the Universe due to decrease or reductionin the speed and temperatu ...
... during the time and reach of the inflation, ii) expansion of the Universe and in turn formation of galaxies having stars, planets, and other celestial bodies in the reach between outer boundary of the inflation and the South Pole of the Universe due to decrease or reductionin the speed and temperatu ...
The cosmic distance scale
... Use the relation you found in one of the preparatory exercises and the min/max magnitudes of each Cepheid to calculate the observed mean magnitudes. These have to be corrected for interstellar extinction. The light traveling to us from M100 is not just passing through the vacuum of space, some of it ...
... Use the relation you found in one of the preparatory exercises and the min/max magnitudes of each Cepheid to calculate the observed mean magnitudes. These have to be corrected for interstellar extinction. The light traveling to us from M100 is not just passing through the vacuum of space, some of it ...
Quantum Mechanics Potential energy
... at infinity is by far the more preferable choice, even if the idea of ...
... at infinity is by far the more preferable choice, even if the idea of ...
Penentuan Jarak dalam Astronomi II
... be the key parameter responsible for RR Lyrae optical luminosity ...
... be the key parameter responsible for RR Lyrae optical luminosity ...
Edwin Hubble (1889
... Shapley defended his conclusions in the so-called "Great Debate" before the National Academy of Sciences on 26 April 1920. His major concern was the size of the galaxy. His model of a drastically larger galaxy, with the solar system far from its center, was largely correct. But he was on less solid ...
... Shapley defended his conclusions in the so-called "Great Debate" before the National Academy of Sciences on 26 April 1920. His major concern was the size of the galaxy. His model of a drastically larger galaxy, with the solar system far from its center, was largely correct. But he was on less solid ...
Dark energy
In physical cosmology and astronomy, dark energy is an unknown form of energy which is hypothesized to permeate all of space, tending to accelerate the expansion of the universe. Dark energy is the most accepted hypothesis to explain the observations since the 1990s indicating that the universe is expanding at an accelerating rate. Assuming that the standard model of cosmology is correct, the best current measurements indicate that dark energy contributes 68.3% of the total energy in the present-day observable universe. The mass–energy of dark matter and ordinary matter contribute 26.8% and 4.9%, respectively, and other components such as neutrinos and photons contribute a very small amount. Again on a mass–energy equivalence basis, the density of dark energy (6.91 × 10−27 kg/m3) is very low, much less than the density of ordinary matter or dark matter within galaxies. However, it comes to dominate the mass–energy of the universe because it is uniform across space.Two proposed forms for dark energy are the cosmological constant, a constant energy density filling space homogeneously, and scalar fields such as quintessence or moduli, dynamic quantities whose energy density can vary in time and space. Contributions from scalar fields that are constant in space are usually also included in the cosmological constant. The cosmological constant can be formulated to be equivalent to vacuum energy. Scalar fields that do change in space can be difficult to distinguish from a cosmological constant because the change may be extremely slow.High-precision measurements of the expansion of the universe are required to understand how the expansion rate changes over time and space. In general relativity, the evolution of the expansion rate is parameterized by the cosmological equation of state (the relationship between temperature, pressure, and combined matter, energy, and vacuum energy density for any region of space). Measuring the equation of state for dark energy is one of the biggest efforts in observational cosmology today.Adding the cosmological constant to cosmology's standard FLRW metric leads to the Lambda-CDM model, which has been referred to as the ""standard model of cosmology"" because of its precise agreement with observations. Dark energy has been used as a crucial ingredient in a recent attempt to formulate a cyclic model for the universe.