Forming disk galaxies in magneto-hydro
... In addition, we were for the first time able to predict the expected structure of the magnetic field in a spiral galaxy directly from the initial conditions left behind after the hot Big Bang. It turns out that already an extremely tiny magnetic field left behind by the Big Bang is sufficient to exp ...
... In addition, we were for the first time able to predict the expected structure of the magnetic field in a spiral galaxy directly from the initial conditions left behind after the hot Big Bang. It turns out that already an extremely tiny magnetic field left behind by the Big Bang is sufficient to exp ...
Stars - gilbertmath.com
... thousands of years, the ____________ from the core gradually reaches the star’s outside and the star “switches on” and begins to __________. ...
... thousands of years, the ____________ from the core gradually reaches the star’s outside and the star “switches on” and begins to __________. ...
Page pour l`impression
... The main difference between terrestrial and giant planets concerns their density : one cubic centimeter of a terrestrial planet weights between 4 and 6 grams whereas one cubic centimeter of a giant planet weighs between 1 and 2 grams. ...
... The main difference between terrestrial and giant planets concerns their density : one cubic centimeter of a terrestrial planet weights between 4 and 6 grams whereas one cubic centimeter of a giant planet weighs between 1 and 2 grams. ...
Celestial Distances - Wayne State University
... Summary of Tools for Measuring Celestial Distances Within the solar system, distances are determined by timing how long it takes radar signals to travel from the Earth to a planet or other body and then return Distances to nearest stars can be measured using the parallax (triangulation) method For ...
... Summary of Tools for Measuring Celestial Distances Within the solar system, distances are determined by timing how long it takes radar signals to travel from the Earth to a planet or other body and then return Distances to nearest stars can be measured using the parallax (triangulation) method For ...
apparent magnitude - Harding University
... – A majority of the stars (about 90%) fall along a diagonal; from hot, luminous stars to cool, dim stars. This diagonal is called the main sequence, and stars falling along this line are often referred to as dwarf stars. – Another group of very luminous, yet cool (red) stars occurs in the upper righ ...
... – A majority of the stars (about 90%) fall along a diagonal; from hot, luminous stars to cool, dim stars. This diagonal is called the main sequence, and stars falling along this line are often referred to as dwarf stars. – Another group of very luminous, yet cool (red) stars occurs in the upper righ ...
hubble_refurb
... supersonic shock wave in the surrounding medium and making the material glow. The Hubble visible-light image reveals, deep within the remnant, a crescent-shaped cloud of pink emission from hydrogen gas and soft purple wisps that correspond to regions of glowing oxygen. A dense background of colorful ...
... supersonic shock wave in the surrounding medium and making the material glow. The Hubble visible-light image reveals, deep within the remnant, a crescent-shaped cloud of pink emission from hydrogen gas and soft purple wisps that correspond to regions of glowing oxygen. A dense background of colorful ...
April 2017 - Newbury Astronomical Society
... Dwarf companion. Hydrogen is pulled off the red giant and spirals inwards towards the white dwarf and forms a rotating disc. The Hydrogen gas eventually falls on to the surface of the white dwarf and is compressed by the enormous gravity into a shallow but very dense layer on the surface. The size o ...
... Dwarf companion. Hydrogen is pulled off the red giant and spirals inwards towards the white dwarf and forms a rotating disc. The Hydrogen gas eventually falls on to the surface of the white dwarf and is compressed by the enormous gravity into a shallow but very dense layer on the surface. The size o ...
Slide 1
... our best estimates are around 9 billion years. To compare, our estimates for the Universe are that it is around 13 billion years old. So the Milky Way has been around for most of the life of the Universe. ...
... our best estimates are around 9 billion years. To compare, our estimates for the Universe are that it is around 13 billion years old. So the Milky Way has been around for most of the life of the Universe. ...
Atomic Physics Explaining the Universe
... Relaxing Structure Most of the mass is in-between the clusters, with kT ~ 1-10 keV. Hydrostatic equilibrium plus radiative cooling implies that at some point the temperature at the core must collapse (to ~104 K, whereupon the gas forms stars). This is inevitable unless the gas is heated. However, “ ...
... Relaxing Structure Most of the mass is in-between the clusters, with kT ~ 1-10 keV. Hydrostatic equilibrium plus radiative cooling implies that at some point the temperature at the core must collapse (to ~104 K, whereupon the gas forms stars). This is inevitable unless the gas is heated. However, “ ...
key for the HR Diagram Lab Handout
... dim. For example, Spica is a blue star at approximately 25,000 K with a high brightness, and Barnard’s star is a red star at approximately 3,000 Suns with with low brightness. 2.) What is the relationship between temperature/color and expected lifetime? Which stars will die first and why? (2 points) ...
... dim. For example, Spica is a blue star at approximately 25,000 K with a high brightness, and Barnard’s star is a red star at approximately 3,000 Suns with with low brightness. 2.) What is the relationship between temperature/color and expected lifetime? Which stars will die first and why? (2 points) ...
Stellar Parallax Problems
... C. The original Gaia mission cost about a Billion dollars. This hypothetical mission might coust about the same even though it is farther away since the development costs have already been covered. Would you be willing to vote to fund such a mission as part of an international consortium? ...
... C. The original Gaia mission cost about a Billion dollars. This hypothetical mission might coust about the same even though it is farther away since the development costs have already been covered. Would you be willing to vote to fund such a mission as part of an international consortium? ...
sun.galaxy.notes
... • A light year is the distance that light travels in a year • We use the light year to measure very distant objects such as stars and galaxies • Light travels at 300,000 km/s or about 9,500,000,000,000 trillion kilometers in one year (9.5 x 1012 km/yr) 299 ,792 km/ s • Nothing is faster than light • ...
... • A light year is the distance that light travels in a year • We use the light year to measure very distant objects such as stars and galaxies • Light travels at 300,000 km/s or about 9,500,000,000,000 trillion kilometers in one year (9.5 x 1012 km/yr) 299 ,792 km/ s • Nothing is faster than light • ...
– 1 – 1. Feedback From The First Stars
... Distant GRBs have been observed in the NIR from with ground-based telescopes to get spectroscopic redshifts z ∼ 6.7 and their spectral energy distribution. There are claims for even higher redshift GRBs based on photometric data only. A few of the more frequent lower redshift GRBs have been observed ...
... Distant GRBs have been observed in the NIR from with ground-based telescopes to get spectroscopic redshifts z ∼ 6.7 and their spectral energy distribution. There are claims for even higher redshift GRBs based on photometric data only. A few of the more frequent lower redshift GRBs have been observed ...
What we can measure
... more heat; • more heat and compactness means more energy production by fusion; • more energy production means more luminosity. ...
... more heat; • more heat and compactness means more energy production by fusion; • more energy production means more luminosity. ...
Balmer lines
... lines emitted by the Sun, and the bright lines emitted by elements in the lab. Kirchhoff described this relation in the form of three 'laws': 1. A hot opaque body, such as the ideal black body, or a star, emits a continuous spectrum. 2. A hot transparent gas produces an emission line spectrum. 3. A ...
... lines emitted by the Sun, and the bright lines emitted by elements in the lab. Kirchhoff described this relation in the form of three 'laws': 1. A hot opaque body, such as the ideal black body, or a star, emits a continuous spectrum. 2. A hot transparent gas produces an emission line spectrum. 3. A ...
A Very Dense Low-Mass Molecular Condensation in Taurus
... of 0.2-0.3 km s _ 1 at 2000-3000 AU in order to reproduce the asymmetric absorption profiles. When the infall velocity reaches that value at 2000-3000 AU in inside-out collapse, the infall velocity at 1000 AU must exceed at least 0.5 km s _ 1 (figure 4), which is inconsistent with the present result ...
... of 0.2-0.3 km s _ 1 at 2000-3000 AU in order to reproduce the asymmetric absorption profiles. When the infall velocity reaches that value at 2000-3000 AU in inside-out collapse, the infall velocity at 1000 AU must exceed at least 0.5 km s _ 1 (figure 4), which is inconsistent with the present result ...
Star-Forming Nuclear Rings in Spiral Galaxies
... the vicinity of hot O- or B-type stars. Given that the ionisation energy for the He i line is higher than that of Brg, it requires the presence of hotter and more massive stars, and hence its brightness falls off more rapidly after an instantaneous burst than that of the Brg line. The time range cov ...
... the vicinity of hot O- or B-type stars. Given that the ionisation energy for the He i line is higher than that of Brg, it requires the presence of hotter and more massive stars, and hence its brightness falls off more rapidly after an instantaneous burst than that of the Brg line. The time range cov ...
Sun, Moon, Earth,
... • In the densest part of a Nebula gravity begins pulling the gas and dust together. – A Protostar is formed when there is enough mass (gas and dust) concentrated to form a star. ...
... • In the densest part of a Nebula gravity begins pulling the gas and dust together. – A Protostar is formed when there is enough mass (gas and dust) concentrated to form a star. ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.