Science East Meteor Radiant Worksheet finished
... Meteors: Pieces of this dust or debris that enter the atmosphere and burns up. These are also known as ‘shooting stars’ or ‘falling stars’. Most burn up and never land at the surface. Fireball: Is simply a very bright meteor, generated by a larger chunk or rock. Fireballs can make it to the ground, ...
... Meteors: Pieces of this dust or debris that enter the atmosphere and burns up. These are also known as ‘shooting stars’ or ‘falling stars’. Most burn up and never land at the surface. Fireball: Is simply a very bright meteor, generated by a larger chunk or rock. Fireballs can make it to the ground, ...
Homologous Stellar Models and Polytropes Main Sequence Stars
... must still be on the Main Sequence, even if they are as old as the Universe. • Low-Mass Stars (0.7 6 M 6 2M ) in most cases end up losing most of their mass to become planetary nebulae before evolving on to the white dwarf cooling track. • Intermediate-Mass Stars (2 6 M 6 8M ) have evolution tracks ...
... must still be on the Main Sequence, even if they are as old as the Universe. • Low-Mass Stars (0.7 6 M 6 2M ) in most cases end up losing most of their mass to become planetary nebulae before evolving on to the white dwarf cooling track. • Intermediate-Mass Stars (2 6 M 6 8M ) have evolution tracks ...
D ASTROPHYSICS
... A galaxy is a creation of stars, gas, and dust held together by gravity and containing billions of stars. The Milky Way contains about 3 × 10 11 stars and, probably, at least this number of planets. Some galaxies exist in isolation but the majority of them occur in groups known as clusters that have ...
... A galaxy is a creation of stars, gas, and dust held together by gravity and containing billions of stars. The Milky Way contains about 3 × 10 11 stars and, probably, at least this number of planets. Some galaxies exist in isolation but the majority of them occur in groups known as clusters that have ...
Characteristics of Our Galaxy
... variables (useful for judging distances), pre-main sequence stars, T-Tauri stars, Herbigharo objects, and even some A stars can be found in the arms. These stars are very metal rich and have highly circular orbits, although they comprise likely less than one percent of Milky Way stars. Young thin d ...
... variables (useful for judging distances), pre-main sequence stars, T-Tauri stars, Herbigharo objects, and even some A stars can be found in the arms. These stars are very metal rich and have highly circular orbits, although they comprise likely less than one percent of Milky Way stars. Young thin d ...
PH607lec11-4gal2
... This arrangement produces a spiral density wave: spiral arms are caused by a density perturbation that moves along at a speed different from the speed of the objects within it. The density wave resists the spiral’s tendency to wind up and causes a rigidly rotating spiral pattern Properties of spira ...
... This arrangement produces a spiral density wave: spiral arms are caused by a density perturbation that moves along at a speed different from the speed of the objects within it. The density wave resists the spiral’s tendency to wind up and causes a rigidly rotating spiral pattern Properties of spira ...
Star formation and internal kinematics of irregular galaxies
... (a few times) the local scale height. In most cases this is a few hundred parsecs. This is the picture that I will proceed with in this thesis; that star formation is a local process, with the same basic physics occuring in independent cells with dimensions between tens of parsecs and a couple of ki ...
... (a few times) the local scale height. In most cases this is a few hundred parsecs. This is the picture that I will proceed with in this thesis; that star formation is a local process, with the same basic physics occuring in independent cells with dimensions between tens of parsecs and a couple of ki ...
Using Star Charts
... There are many different types of star charts available, in a variety of forms, each designed to get around the problem that the appearance of the sky changes with time. To use any of them usually requires a little practice. The star chart that you will be introduced to in this assignment are those ...
... There are many different types of star charts available, in a variety of forms, each designed to get around the problem that the appearance of the sky changes with time. To use any of them usually requires a little practice. The star chart that you will be introduced to in this assignment are those ...
Chromospherically young, kinematically old stars
... outer envelope convection is expected to drive the chromospheric activity. Nevertheless, not only young single stars present high rotation rates. Close and contact binaries can keep high rotation over several billion years. In such stars, the rotational angular momentum loss is balanced by the proxi ...
... outer envelope convection is expected to drive the chromospheric activity. Nevertheless, not only young single stars present high rotation rates. Close and contact binaries can keep high rotation over several billion years. In such stars, the rotational angular momentum loss is balanced by the proxi ...
Galaxies
... • What is the evidence for dark matter in clusters of galaxies? – Masses measured from galaxy motions, temperature of hot gas, and gravitational lensing all indicate that the vast majority of matter in clusters is dark ...
... • What is the evidence for dark matter in clusters of galaxies? – Masses measured from galaxy motions, temperature of hot gas, and gravitational lensing all indicate that the vast majority of matter in clusters is dark ...
argo and other tidal structures around the milky way
... sample was limited to −25◦ < b < +25◦ , in order to avoid the Magellanic Clouds. The solar position is X = −8 kpc, Y = 0 kpc. A number of known structures can be seen in these plots: The Monoceros stream, Sagittarius, the TriAnd and Perseus systems (Rocha-Pinto et al. 2004). The large southern hemis ...
... sample was limited to −25◦ < b < +25◦ , in order to avoid the Magellanic Clouds. The solar position is X = −8 kpc, Y = 0 kpc. A number of known structures can be seen in these plots: The Monoceros stream, Sagittarius, the TriAnd and Perseus systems (Rocha-Pinto et al. 2004). The large southern hemis ...
Stellar Masses
... stably. Objects with masses slightly below this limit are called brown dwarfs, and are ‘star like’ in the sense that nuclear burning of deuterium occurs in their core. Below a mass of 0.015M⊙ (roughly 16 times the mass of Jupiter) not even deuterium burning can occur, and these objects are perhaps b ...
... stably. Objects with masses slightly below this limit are called brown dwarfs, and are ‘star like’ in the sense that nuclear burning of deuterium occurs in their core. Below a mass of 0.015M⊙ (roughly 16 times the mass of Jupiter) not even deuterium burning can occur, and these objects are perhaps b ...
Cassiopeia (constellation)
Cassiopeia is a constellation in the northern sky, named after the vain queen Cassiopeia in Greek mythology, who boasted about her unrivalled beauty. Cassiopeia was one of the 48 constellations listed by the 2nd-century Greek astronomer Ptolemy, and it remains one of the 88 modern constellations today. It is easily recognizable due to its distinctive 'M' shape when in upper culmination but in higher northern locations when near lower culminations in spring and summer it has a 'W' shape, formed by five bright stars. It is bordered by Andromeda to the south, Perseus to the southeast, and Cepheus to the north. It is opposite the Big Dipper.In northern locations above 34ºN latitude it is visible year-round and in the (sub)tropics it can be seen at its clearest from September to early November in its characteristic 'M' shape. Even in low southern latitudes below 25ºS is can be seen low in the North.