Dark Weak Force and Condensed Matter Contents
... not. For a long time the hypothesis was that the charges are feeded to larger space-time sheets in this length scale rather than screened by vacuum charges so that an effective screening results in electro-weak length scale. A more promising approach inspired by the TGD based view about dark matter ...
... not. For a long time the hypothesis was that the charges are feeded to larger space-time sheets in this length scale rather than screened by vacuum charges so that an effective screening results in electro-weak length scale. A more promising approach inspired by the TGD based view about dark matter ...
26 Non-WIMP dark matter
... To begin contemplating how the physics and the cosmological evolution of VM and DM may be related, we first consider some of the relevant properties of VM. It has been long established that the relic abundance of VM is due to an excess of matter over antimatter in the today’s universe. The evidence ...
... To begin contemplating how the physics and the cosmological evolution of VM and DM may be related, we first consider some of the relevant properties of VM. It has been long established that the relic abundance of VM is due to an excess of matter over antimatter in the today’s universe. The evidence ...
and galaxies
... This discovery was important because • It’s a feature of H (most abundant element) • It occurs only in low density regions • It indicates the presence of neutral ( i.e.nonionised and non-molecular) HI atoms • It is not easily absorbed by interstellar gas. This means that 21cm radiation emission from ...
... This discovery was important because • It’s a feature of H (most abundant element) • It occurs only in low density regions • It indicates the presence of neutral ( i.e.nonionised and non-molecular) HI atoms • It is not easily absorbed by interstellar gas. This means that 21cm radiation emission from ...
astro-ph/9505110 PDF
... Our results are shown in Figures 4 and 5 (Garnett et al. 1994, 1995). We nd that the C/O ratio increases monotonically as a function of O/H, from about 1/4 solar at the lowest metallicities up to solar values. At the same time, C/N also appears to increase with O/H in the irregular galaxies, but th ...
... Our results are shown in Figures 4 and 5 (Garnett et al. 1994, 1995). We nd that the C/O ratio increases monotonically as a function of O/H, from about 1/4 solar at the lowest metallicities up to solar values. At the same time, C/N also appears to increase with O/H in the irregular galaxies, but th ...
Evolution of galaxy morphology - Lecture 1 - NCRA-TIFR
... gravitationally bound agglomerations of stars, dust, gas, dark matter. Mass ratio Gas:Stars:Dark Matter - 1:10:100 they are the basic building blocks of the Universe on large scales they show a broad range in their physical properties Understanding of galaxy formation and evolution is one of the mai ...
... gravitationally bound agglomerations of stars, dust, gas, dark matter. Mass ratio Gas:Stars:Dark Matter - 1:10:100 they are the basic building blocks of the Universe on large scales they show a broad range in their physical properties Understanding of galaxy formation and evolution is one of the mai ...
Full-Text PDF
... they proposed some candidates to explain them. Modifying general relativity opens a way to a large class of alternative theories of gravity ranging from higher dimensional physics to non-minimally coupled (scalar) fields. On the other hand, one of the interesting dreams of physicists is finding a co ...
... they proposed some candidates to explain them. Modifying general relativity opens a way to a large class of alternative theories of gravity ranging from higher dimensional physics to non-minimally coupled (scalar) fields. On the other hand, one of the interesting dreams of physicists is finding a co ...
Exploring Neutral Hydrogen and Galaxy Evolution with the SKA
... follow a bimodal distribution in colour as a function of stellar mass (Baldry et al. (2004)); most galaxies are either located in the so-called blue cloud or on the red sequence, indicating that star formation is either still ongoing or was quenched billions of years ago. Furthermore, the galaxy ‘ma ...
... follow a bimodal distribution in colour as a function of stellar mass (Baldry et al. (2004)); most galaxies are either located in the so-called blue cloud or on the red sequence, indicating that star formation is either still ongoing or was quenched billions of years ago. Furthermore, the galaxy ‘ma ...
The local density of matter mapped by Hipparcos
... is estimated to lie in the range rvis 0:06; 0:10 M( pc23 . Another study using Hipparcos data was made by Pham (1997), who used a different method to study F stars, where he determined scaleheights and velocity dispersions for his chosen sample and then, assuming isothermality, used the 2pGh2z r ...
... is estimated to lie in the range rvis 0:06; 0:10 M( pc23 . Another study using Hipparcos data was made by Pham (1997), who used a different method to study F stars, where he determined scaleheights and velocity dispersions for his chosen sample and then, assuming isothermality, used the 2pGh2z r ...
Morphology and Environment
... Galaxies are not distributed at random – they occur in pairs, groups, and clusters containing up to 103 members. These systems define the environments in which galaxies are formed and transformed. ...
... Galaxies are not distributed at random – they occur in pairs, groups, and clusters containing up to 103 members. These systems define the environments in which galaxies are formed and transformed. ...
elt science case
... New observational facilities in the coming decade will try to address these questions. Furthermore, new fundamental question may arise: the evidence for dark energy was found only recently, and it added a new component to the Universe, the biggest component in terms of energy density at low redshift ...
... New observational facilities in the coming decade will try to address these questions. Furthermore, new fundamental question may arise: the evidence for dark energy was found only recently, and it added a new component to the Universe, the biggest component in terms of energy density at low redshift ...
A new view of galaxy evolution
... mass: the amount of mass in gas, such as hydrogen, which can form into stars, and therefore can increase or decrease with time; and the dark matter mass. The dark matter mass can be up to ten times the stellar mass, based on observations in the nearby universe. These two types of masses – gaseous an ...
... mass: the amount of mass in gas, such as hydrogen, which can form into stars, and therefore can increase or decrease with time; and the dark matter mass. The dark matter mass can be up to ten times the stellar mass, based on observations in the nearby universe. These two types of masses – gaseous an ...
Conformal Gravity
... standard theory for gravity. But nowadays there is data from far more distant objects, like other galaxies or galaxy clusters. On these distance scales there arise several problems. For example the measurement of rotational velocities of stars or gas in galaxies differs very strongly from the expect ...
... standard theory for gravity. But nowadays there is data from far more distant objects, like other galaxies or galaxy clusters. On these distance scales there arise several problems. For example the measurement of rotational velocities of stars or gas in galaxies differs very strongly from the expect ...
mg_colloq - University of Massachusetts Amherst
... Residuals consistent with NORMAL surface density of intervening sources ...
... Residuals consistent with NORMAL surface density of intervening sources ...
SOME CONSTRAINTS ON GALAXY EVOLUTION IMPOSED BY
... frequency < S > = 9.3 in nine cD/E galaxies is higher than that in 34 E + S0 galaxies for which < S > = 5.1. Furthermore, the specific frequency < S > = 0.8 in eight late-type spirals (Sb - Scd) is significantly lower than the value < S > = 1.9 in three bulge-dominated Sa and Sab galaxies. In summar ...
... frequency < S > = 9.3 in nine cD/E galaxies is higher than that in 34 E + S0 galaxies for which < S > = 5.1. Furthermore, the specific frequency < S > = 0.8 in eight late-type spirals (Sb - Scd) is significantly lower than the value < S > = 1.9 in three bulge-dominated Sa and Sab galaxies. In summar ...
The Evolution of the Universe - Western Washington University
... in the first place. In fact, the closer we look to time "zero," the less certain we are about what actually happened, because our current description of physical laws do not yet apply to such extremes of nature. The Big Bang scenario simply assumes that space, time, and energy already existed. But i ...
... in the first place. In fact, the closer we look to time "zero," the less certain we are about what actually happened, because our current description of physical laws do not yet apply to such extremes of nature. The Big Bang scenario simply assumes that space, time, and energy already existed. But i ...
Dark matter
Dark matter is a hypothetical kind of matter that cannot be seen with telescopes but would account for most of the matter in the universe. The existence and properties of dark matter are inferred from its gravitational effects on visible matter, on radiation, and on the large-scale structure of the universe. Dark matter has not been detected directly, making it one of the greatest mysteries in modern astrophysics.Dark matter neither emits nor absorbs light or any other electromagnetic radiation at any significant level. According to the Planck mission team, and based on the standard model of cosmology, the total mass–energy of the known universe contains 4.9% ordinary matter, 26.8% dark matter and 68.3% dark energy. Thus, dark matter is estimated to constitute 84.5% of the total matter in the universe, while dark energy plus dark matter constitute 95.1% of the total mass–energy content of the universe.Astrophysicists hypothesized the existence of dark matter to account for discrepancies between the mass of large astronomical objects determined from their gravitational effects, and their mass as calculated from the observable matter (stars, gas, and dust) that they can be seen to contain. Their gravitational effects suggest that their masses are much greater than the observable matter survey suggests. Dark matter was postulated by Jan Oort in 1932, albeit based upon insufficient evidence, to account for the orbital velocities of stars in the Milky Way. In 1933, Fritz Zwicky was the first to use the virial theorem to infer the existence of unseen matter, which he referred to as dunkle Materie 'dark matter'. More robust evidence from galaxy rotation curves was discovered by Horace W. Babcock in 1939, but was not attributed to dark matter. The first hypothesis to postulate ""dark matter"" based upon robust evidence was formulated by Vera Rubin and Kent Ford in the 1960s–1970s, using galaxy rotation curves. Subsequently, many other observations have indicated the presence of dark matter in the universe, including gravitational lensing of background objects by galaxy clusters such as the Bullet Cluster, the temperature distribution of hot gas in galaxies and clusters of galaxies and, more recently, the pattern of anisotropies in the cosmic microwave background. According to consensus among cosmologists, dark matter is composed primarily of a not yet characterized type of subatomic particle.The search for this particle, by a variety of means, is one of the major efforts in particle physics today.Although the existence of dark matter is generally accepted by the mainstream scientific community, some alternative theories of gravity have been proposed, such as MOND and TeVeS, which try to account for the anomalous observations without requiring additional matter. However, these theories cannot account for the properties of galaxy clusters.