The Interstellar Medium and Star Formation
... planets. Some planets become massive enough to also accumulate Hydrogen and Helium gas. • However, during and after formation, it seems that some planets are able to migrate in their disks, drifting inwards to settle close to the star. We do not know why this did not happen so much in our own Solar ...
... planets. Some planets become massive enough to also accumulate Hydrogen and Helium gas. • However, during and after formation, it seems that some planets are able to migrate in their disks, drifting inwards to settle close to the star. We do not know why this did not happen so much in our own Solar ...
Stars
... amount of energy, but there are billions of reactions per second. Each second, the Sun produces 4 × 1026 joules of energy. It would take 2,000 million nuclear power plants a whole year to produce the same amount of energy on Earth. In the Sun, and in most stars, hydrogen atoms fuse together to form ...
... amount of energy, but there are billions of reactions per second. Each second, the Sun produces 4 × 1026 joules of energy. It would take 2,000 million nuclear power plants a whole year to produce the same amount of energy on Earth. In the Sun, and in most stars, hydrogen atoms fuse together to form ...
Properties of Supernovae
... few months the luminosity of the star is comparable to the luminosity of the entire parent galaxy. Supernovae are rare events, occurring only once or twice per century in a typical galaxy. There have been just six supernovae seen in the Milky Way in recorded history, with the most recent occurring i ...
... few months the luminosity of the star is comparable to the luminosity of the entire parent galaxy. Supernovae are rare events, occurring only once or twice per century in a typical galaxy. There have been just six supernovae seen in the Milky Way in recorded history, with the most recent occurring i ...
Spectral Classification
... O and B stars are so powerful, they live for a very short time. They do not stray far from the area in which they were formed as they don't have the time. They therefore tend to cluster together in what we call OB1 associations. and contains all of the constellation of Orion. They constitute about 0 ...
... O and B stars are so powerful, they live for a very short time. They do not stray far from the area in which they were formed as they don't have the time. They therefore tend to cluster together in what we call OB1 associations. and contains all of the constellation of Orion. They constitute about 0 ...
Document
... Below the lower limit, not enough gravity (mass) to produce the temp and pressure needed to sustain hydrogen fusion. • 0.016 MSun to 0.08 MSun are brown dwarfs. • Jupiter is about 75 times too small to have become a star. (17 times smaller than the smallest brown dwarf.) ...
... Below the lower limit, not enough gravity (mass) to produce the temp and pressure needed to sustain hydrogen fusion. • 0.016 MSun to 0.08 MSun are brown dwarfs. • Jupiter is about 75 times too small to have become a star. (17 times smaller than the smallest brown dwarf.) ...
5-E Galaxy T - McDonald Observatory
... Galaxies, compared to their size, are closer together than stars. They are also much more massive, having the combined mass of billions of stars. So, even over a large distance the force of gravity between galaxies can accelerate them toward each other. Think of bowling balls (galaxies) on a trampol ...
... Galaxies, compared to their size, are closer together than stars. They are also much more massive, having the combined mass of billions of stars. So, even over a large distance the force of gravity between galaxies can accelerate them toward each other. Think of bowling balls (galaxies) on a trampol ...
The Properties of Stars
... sequence and then moves off the sequence when it runs out of fuel. • How long it stays on the main sequence and where it moves to depends on size. ...
... sequence and then moves off the sequence when it runs out of fuel. • How long it stays on the main sequence and where it moves to depends on size. ...
Lecture 11, PPT version
... Many such X-ray binary systems exist in our Galaxy, with black holes that have masses between 4 Msun and 10 Msun ...
... Many such X-ray binary systems exist in our Galaxy, with black holes that have masses between 4 Msun and 10 Msun ...
Slide 1
... • As the core of a star collapses to form a neutron star, it spins fasters and faster • Its magnetic field becomes concentrated, and this results in a beam of radio waves coming out of its ...
... • As the core of a star collapses to form a neutron star, it spins fasters and faster • Its magnetic field becomes concentrated, and this results in a beam of radio waves coming out of its ...
about Stars
... • Astronomers quantify the “color” of a star by using the difference in brightness between the brightness in the B and V spectral regions • The B-V color is related to the slope of the ...
... • Astronomers quantify the “color” of a star by using the difference in brightness between the brightness in the B and V spectral regions • The B-V color is related to the slope of the ...
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.