The Gemini Observatory: Moving into Science Operations
... In other words, as previously suggested by van de Ven et al. (2006) and Sollima et al. (2009), the dynamics of the outer parts of Cen, where there is but a small fraction of the total mass, are dominated by external influences. What’s needed, if you want to enquire as to whether there is any evide ...
... In other words, as previously suggested by van de Ven et al. (2006) and Sollima et al. (2009), the dynamics of the outer parts of Cen, where there is but a small fraction of the total mass, are dominated by external influences. What’s needed, if you want to enquire as to whether there is any evide ...
MS Word version
... predictions about the locations and motions of the stars as time advances. After drawing in your predictions you should use the simulator to check your answer. If your original prediction was in error, redraw your star paths to reflect the correct motion. a) Draw in the location of the North Celesti ...
... predictions about the locations and motions of the stars as time advances. After drawing in your predictions you should use the simulator to check your answer. If your original prediction was in error, redraw your star paths to reflect the correct motion. a) Draw in the location of the North Celesti ...
Folie 1
... one of the defining candidates of T-Tauri stars present on all time scales short time, mostly small changes: rotation ocultations from disk ‘flickering’ long time, larger amplitudes: EX Lup (EXor) FU Ori (FUor) duration for FUor unclear, frequency 5-50kyr from infrared ...
... one of the defining candidates of T-Tauri stars present on all time scales short time, mostly small changes: rotation ocultations from disk ‘flickering’ long time, larger amplitudes: EX Lup (EXor) FU Ori (FUor) duration for FUor unclear, frequency 5-50kyr from infrared ...
Density, Mass and Surface Area
... Put each sphere one at a time on the scale and get its mass. The scale is just like your doctor’s scale: add up the readings on each beam to get total mass. Enter these masses in the appropriate box in the table above. 1) Compare the two steel spheres. Which one is heavier? Which one has more mass? ...
... Put each sphere one at a time on the scale and get its mass. The scale is just like your doctor’s scale: add up the readings on each beam to get total mass. Enter these masses in the appropriate box in the table above. 1) Compare the two steel spheres. Which one is heavier? Which one has more mass? ...
Some Introductory Physics of Sound
... complete vacuum. There is matter lying between the stars – and even between galaxies – in space. These may not form an ‘atmosphere’ as we would obviously recognise it, as such regions are at much lower densities than we ever experience on Earth. The air molecules in this room only occupy about 1/100 ...
... complete vacuum. There is matter lying between the stars – and even between galaxies – in space. These may not form an ‘atmosphere’ as we would obviously recognise it, as such regions are at much lower densities than we ever experience on Earth. The air molecules in this room only occupy about 1/100 ...
Black Hole Accretion
... Mass can be measured in the Newtonian limit using test particles (e.g., stellar companion) at large radii ...
... Mass can be measured in the Newtonian limit using test particles (e.g., stellar companion) at large radii ...
The Stellar Population Synthesis Technique Charlie Conroy Princeton
... Lets construct a flexible dust model: • Two dust components: 1. dust around young stars with optical depth τ1 i.e. stars embedded in molecular cloud 2. dust around old stars with optical depth τ2 i.e. cirrus dust a) old dust can be clumpy, with gaussian PDF characterized by dispersion σclump • Trans ...
... Lets construct a flexible dust model: • Two dust components: 1. dust around young stars with optical depth τ1 i.e. stars embedded in molecular cloud 2. dust around old stars with optical depth τ2 i.e. cirrus dust a) old dust can be clumpy, with gaussian PDF characterized by dispersion σclump • Trans ...
Leverhulme lectures on stellar magnetism. 1. Overview
... For detailed study of stars, spectra are particularly powerful data because of rich information content of lines Spectral lines arise from atomic transitions between two energy states or levels Detection of magnetic field is possible because energy levels of atoms and ions are perturbed by a field, ...
... For detailed study of stars, spectra are particularly powerful data because of rich information content of lines Spectral lines arise from atomic transitions between two energy states or levels Detection of magnetic field is possible because energy levels of atoms and ions are perturbed by a field, ...
Pattern recognition of star constellations for spacecraft
... of the imaging device is known, and thus the attitude of the spacecraft. One approach is to sweep the sky with a spectral sensitive device in order to recognize a known spectral distribution from a specific star. When the star is recognized the attitude control system locks on the specific star. Ano ...
... of the imaging device is known, and thus the attitude of the spacecraft. One approach is to sweep the sky with a spectral sensitive device in order to recognize a known spectral distribution from a specific star. When the star is recognized the attitude control system locks on the specific star. Ano ...
five minute episode script
... the northwestern sky. There it is, standing on its handle – the Big Dipper. The formation of those seven bright stars is unmistakable. DEAN: Four stars make the scoop of the Big Dipper and three more make up the handle. Now where’s that Big Bear that’ll turn my asterism into a constellation? ...
... the northwestern sky. There it is, standing on its handle – the Big Dipper. The formation of those seven bright stars is unmistakable. DEAN: Four stars make the scoop of the Big Dipper and three more make up the handle. Now where’s that Big Bear that’ll turn my asterism into a constellation? ...
Galaxies - cloudfront.net
... billions of stars. Galaxies are divided into three types according to shape: spiral, elliptical, and irregular galaxies. • Spiral galaxies spin and appear as a rotating disk of stars and dust, with a bulge in the middle. Several spiral arms reach outward from the central bulge like the arms of a pin ...
... billions of stars. Galaxies are divided into three types according to shape: spiral, elliptical, and irregular galaxies. • Spiral galaxies spin and appear as a rotating disk of stars and dust, with a bulge in the middle. Several spiral arms reach outward from the central bulge like the arms of a pin ...
![The P Cygni supergiant [OMN2000] LS1](http://s1.studyres.com/store/data/014882705_1-5f78b60dc5267f0c5ad35fc8d810ae0e-300x300.png)
Climbing the Distance Ladder
... We don’t directly measure a star’s luminosity. We measure its flux (f): the wattage collected per square meter of our telescope mirror. ...
... We don’t directly measure a star’s luminosity. We measure its flux (f): the wattage collected per square meter of our telescope mirror. ...
PDF only
... to the nature of the companion star in the system (from Ref. [3-b]). (b) Measured surface temperatures of isolated neutron stars; the ages reported in abscissa are obtained from the rotating dipole model, and the solid line represents a standard cooling simulation (from Ref. [6-b]). We thus see how ...
... to the nature of the companion star in the system (from Ref. [3-b]). (b) Measured surface temperatures of isolated neutron stars; the ages reported in abscissa are obtained from the rotating dipole model, and the solid line represents a standard cooling simulation (from Ref. [6-b]). We thus see how ...
81 KB - CSIRO Publishing
... zone of avoidance are special cases which are probably not in equilibrium but are in the throes of disruption. However the zone of avoidance is rapidly being filled, with several UCD-like objects having measured half-light sizes as large as 100 pc. If having a half-light size greater than ,100 pc is ...
... zone of avoidance are special cases which are probably not in equilibrium but are in the throes of disruption. However the zone of avoidance is rapidly being filled, with several UCD-like objects having measured half-light sizes as large as 100 pc. If having a half-light size greater than ,100 pc is ...
Measuring the Rotational Speed of Spiral Galaxies and
... emission line is in the red region of the visible spectrum. Because most of the gas in galaxies is made of hydrogen, this can be a very strong emission line if young, massive, hot stars are present, as they are in the disks of spiral galaxies. Halpha photons have a rest wavelength (λrest) 6563 Å (An ...
... emission line is in the red region of the visible spectrum. Because most of the gas in galaxies is made of hydrogen, this can be a very strong emission line if young, massive, hot stars are present, as they are in the disks of spiral galaxies. Halpha photons have a rest wavelength (λrest) 6563 Å (An ...
class 2, S11
... We are on a planet, orbiting a star, in a galaxy (which is a member of the Local Group of galaxies in the Local Supercluster) • How did we come to be? • How can we know what the universe was like in the past? • Can we see the entire universe? ...
... We are on a planet, orbiting a star, in a galaxy (which is a member of the Local Group of galaxies in the Local Supercluster) • How did we come to be? • How can we know what the universe was like in the past? • Can we see the entire universe? ...
Is There a Ring Around Milky Way?
... forming a ring structure around our Galaxy. In fact, such satellite-stellar systems may be considered to be the parts of the ring structure around our Galaxy. If the mass and the radius of our Galaxy are 10-15% less than what we have assumed above, we get one orbit within the orbit of LMC which, of ...
... forming a ring structure around our Galaxy. In fact, such satellite-stellar systems may be considered to be the parts of the ring structure around our Galaxy. If the mass and the radius of our Galaxy are 10-15% less than what we have assumed above, we get one orbit within the orbit of LMC which, of ...
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.