tut35 Magnitudes
... versus daylight sky’s 6.5 magnitude/arcsecond2 has sufficient contrast to be visible just before sunset or just after sunrise. The full Moon’s size and 3.6 magnitude/arcsecond2 makes for an easy daylight sighting. At greatest elongation, Venus’ magnitude/arcsecond2 is 1.9. The large contrast with th ...
... versus daylight sky’s 6.5 magnitude/arcsecond2 has sufficient contrast to be visible just before sunset or just after sunrise. The full Moon’s size and 3.6 magnitude/arcsecond2 makes for an easy daylight sighting. At greatest elongation, Venus’ magnitude/arcsecond2 is 1.9. The large contrast with th ...
Lab: Inverse Square Law
... Introduction: As light travels from a source it spreads out equally in all directions. The brightness of the light is the power (energy per second) per area. We all know that a light, such as a candle or a streetlight, looks dimmer the farther away from it we get. But how does the brightness change ...
... Introduction: As light travels from a source it spreads out equally in all directions. The brightness of the light is the power (energy per second) per area. We all know that a light, such as a candle or a streetlight, looks dimmer the farther away from it we get. But how does the brightness change ...
Chapter 18 The Interstellar Medium - University of Texas Astronomy
... Ultraviolet Astronomy and the “Local Bubble” Ultraviolet observations, which must be done from space, have shown that the interstellar medium is full of “bubbles” and “tunnels” that are very hot and have very low densities. The interior is the hot part, emitting UV spectral lines, the outer shell of ...
... Ultraviolet Astronomy and the “Local Bubble” Ultraviolet observations, which must be done from space, have shown that the interstellar medium is full of “bubbles” and “tunnels” that are very hot and have very low densities. The interior is the hot part, emitting UV spectral lines, the outer shell of ...
Chapter 3 The Interstellar Medium
... of dust in the disc of our Galaxy ' 0.1 of the mass of gas. Generally, the interstellar medium amounts to only a small fraction of a galaxy’s luminous mass, but this fraction is strongly correlated with the galaxy’s morphological type. This fraction is ' 0 % for an elliptical galaxy, 1–25 % for a sp ...
... of dust in the disc of our Galaxy ' 0.1 of the mass of gas. Generally, the interstellar medium amounts to only a small fraction of a galaxy’s luminous mass, but this fraction is strongly correlated with the galaxy’s morphological type. This fraction is ' 0 % for an elliptical galaxy, 1–25 % for a sp ...
Astronomical Formulae
... ESTIMATING ANGULAR DISTANCE Penny, 4 km distant ....................................... 1" Sun, Moon ................................................. 30' (The Moon is approximately 400 times smaller in angular diameter than the Sun, but is approx 400 times closer) Width of little finger at arm's le ...
... ESTIMATING ANGULAR DISTANCE Penny, 4 km distant ....................................... 1" Sun, Moon ................................................. 30' (The Moon is approximately 400 times smaller in angular diameter than the Sun, but is approx 400 times closer) Width of little finger at arm's le ...
Galaxy Formation and Evolution
... Since galaxies are observed over cosmological length and time scales, the description of their formation and evolution must involve cosmology, the study of the properties of space-time on large scales. Modern cosmology is based upon the Cosmological Principle, the hypothesis that the Universe is spa ...
... Since galaxies are observed over cosmological length and time scales, the description of their formation and evolution must involve cosmology, the study of the properties of space-time on large scales. Modern cosmology is based upon the Cosmological Principle, the hypothesis that the Universe is spa ...
flare swg usa
... Fitting SEDS: The long-λ fluxes from cool dust have ambiguous SED fits, while higher spatial resolution, near-IR fluxes from clustered sources are often very much fainter. FLARE can reach ~8 mag deeper than IRAC surveys at 3.5 μm, enabling the measurement of the NIR SEDs of young (<104 yr old) ...
... Fitting SEDS: The long-λ fluxes from cool dust have ambiguous SED fits, while higher spatial resolution, near-IR fluxes from clustered sources are often very much fainter. FLARE can reach ~8 mag deeper than IRAC surveys at 3.5 μm, enabling the measurement of the NIR SEDs of young (<104 yr old) ...
Strongly Interacting Supernovae - The National Centre for Radio
... No indication of reverse shock emission RS moved back to centre and weakened. RS is a cooking shock and the cool shell absorbing this. ...
... No indication of reverse shock emission RS moved back to centre and weakened. RS is a cooking shock and the cool shell absorbing this. ...
Our Local Group of Galaxies
... • These galaxies contain no (or very little gas) so that MHI/LB < 10-2 (solar units). They are not forming stars now, nor have they done so recently in any significant way. • They have a “smooth appearance” and are generally elliptical in shape, with the surface brightness largest in the centre decr ...
... • These galaxies contain no (or very little gas) so that MHI/LB < 10-2 (solar units). They are not forming stars now, nor have they done so recently in any significant way. • They have a “smooth appearance” and are generally elliptical in shape, with the surface brightness largest in the centre decr ...
Distance Measures: Parallax
... methods of determining distances: radar, parallax, standard candles, and the Hubble Law. Each of these methods is most useful at certain distances, with radar being useful nearby (for example, the Moon), and the Hubble Law being useful at the farthest distances. In this exercise, we investigate the ...
... methods of determining distances: radar, parallax, standard candles, and the Hubble Law. Each of these methods is most useful at certain distances, with radar being useful nearby (for example, the Moon), and the Hubble Law being useful at the farthest distances. In this exercise, we investigate the ...
Figueira, Pont, Mordasini, Alibert, Georgy, Benz
... and model-input uncertainties than, for instance, predictions about the thermal history or atmospheric spectrum of exoplanets. Sasselov et al. (2007) discussed the effects of the different sources of uncertainties on the radius predictions, and found that the most significant effect – the equation o ...
... and model-input uncertainties than, for instance, predictions about the thermal history or atmospheric spectrum of exoplanets. Sasselov et al. (2007) discussed the effects of the different sources of uncertainties on the radius predictions, and found that the most significant effect – the equation o ...
Distance Measures: Parallax
... methods of determining distances: radar, parallax, standard candles, and the Hubble Law. Each of these methods is most useful at certain distances, with radar being useful nearby (for example, the Moon), and the Hubble Law being useful at the farthest distances. In this exercise, we investigate the ...
... methods of determining distances: radar, parallax, standard candles, and the Hubble Law. Each of these methods is most useful at certain distances, with radar being useful nearby (for example, the Moon), and the Hubble Law being useful at the farthest distances. In this exercise, we investigate the ...
Planetplanet scattering alone cannot explain the freefloating planet
... A focused wind is also observed in the case of Cyg X-1 (Gies & Bolton 1986; Miller et al. 2005), a high-mass X-ray binary, and it was modelled by Gies & Bolton (1986). Even though the presence of a focused stellar wind in LS 5039 needs further study and is to be modelled properly, it possibly has di ...
... A focused wind is also observed in the case of Cyg X-1 (Gies & Bolton 1986; Miller et al. 2005), a high-mass X-ray binary, and it was modelled by Gies & Bolton (1986). Even though the presence of a focused stellar wind in LS 5039 needs further study and is to be modelled properly, it possibly has di ...
Chapter 4 The Origin and Nature of Light
... 1. As an object heats up, it gets brighter because it emits more electromagnetic radiation. 2. The dominant color or wavelength of the emitted radiation changes with temperature. A cool object emits most of its energy at long wavelengths, such as infrared or red. A hotter object emits most of its en ...
... 1. As an object heats up, it gets brighter because it emits more electromagnetic radiation. 2. The dominant color or wavelength of the emitted radiation changes with temperature. A cool object emits most of its energy at long wavelengths, such as infrared or red. A hotter object emits most of its en ...
Astronomy 114 - Department of Astronomy
... 1. Fragmentation of a giant molecular cloud into clumps 2. Collapse of the clumps due to their own gravity ...
... 1. Fragmentation of a giant molecular cloud into clumps 2. Collapse of the clumps due to their own gravity ...
THE SUN - OoCities
... The process of energy generation results from the enormous pressure and density at the centre of the Sun, which makes it possible for nuclei to overcome electrostatic repulsion. (Nuclei are positive and thus repel each other.) Once in some billions of years a given proton (1H, in which the superscri ...
... The process of energy generation results from the enormous pressure and density at the centre of the Sun, which makes it possible for nuclei to overcome electrostatic repulsion. (Nuclei are positive and thus repel each other.) Once in some billions of years a given proton (1H, in which the superscri ...
The Star-Galaxy Era of Big History in the Light of Universal
... the Universe. In addition, there is no consensus on which galaxies should be regarded as old, and which galaxies should be considered young. The point is that within a single galaxy one can find stars and their aggregates that considerably differ in their type, age, and other parameters. For example ...
... the Universe. In addition, there is no consensus on which galaxies should be regarded as old, and which galaxies should be considered young. The point is that within a single galaxy one can find stars and their aggregates that considerably differ in their type, age, and other parameters. For example ...
01-Star Atlas Project - Mapping the Heavens
... Apparent means what it says, how does it "appear " from where you're standing. If you're standing upon the Earth, it will appear quite differently than if you're standing on ...
... Apparent means what it says, how does it "appear " from where you're standing. If you're standing upon the Earth, it will appear quite differently than if you're standing on ...
Binocular Objects (MS Word)
... Sagittarius contains more Messier objects than any other constellation. The best way to identify them is to take them one by one. The beginner will have to be careful not to confuse the various objects. The principal stars of Sagittarius form the famous “Teapot” asterism. The brightest part of the M ...
... Sagittarius contains more Messier objects than any other constellation. The best way to identify them is to take them one by one. The beginner will have to be careful not to confuse the various objects. The principal stars of Sagittarius form the famous “Teapot” asterism. The brightest part of the M ...
R136a1
RMC 136a1 (usually abbreviated to R136a1) is a Wolf-Rayet star located at the center of R136, the central condensation of stars of the large NGC 2070 open cluster in the Tarantula Nebula. It lies at a distance of about 50 kiloparsecs (163,000 light-years) in the Large Magellanic Cloud. It has the highest mass and luminosity of any known star, at 265 M☉ and 8.7 million L☉, and also one of the hottest at over 50,000 K.