Killer Skies
... known as the Crab Nebula. The Crab Nebula is called so for its many-legged shape. The ‘legs’ are filaments of gas that are moving away from the site of the explosion at about 1,400 km/s. Comparing the nebula’s radius, 1.35 pc, with its velocity of expansion reveals that the nebula began expanding ni ...
... known as the Crab Nebula. The Crab Nebula is called so for its many-legged shape. The ‘legs’ are filaments of gas that are moving away from the site of the explosion at about 1,400 km/s. Comparing the nebula’s radius, 1.35 pc, with its velocity of expansion reveals that the nebula began expanding ni ...
Astronomy and Survey of Information
... because of likely extreme variations in surface temperature during different parts of the orbit. ...
... because of likely extreme variations in surface temperature during different parts of the orbit. ...
How Bright is that star?
... Luminosity is the amount of energy a star gives off as light. Measured in Watts or Solar Units or “Sols” However for all practical purposes Absolute magnitude and Luminosity of a star measure the same thing. Absolute Magnitude Approximate Luminosity ...
... Luminosity is the amount of energy a star gives off as light. Measured in Watts or Solar Units or “Sols” However for all practical purposes Absolute magnitude and Luminosity of a star measure the same thing. Absolute Magnitude Approximate Luminosity ...
Document
... Our Milky Way I. Select bright objects that you can see throughout the Milky Way and trace their directions and distances II. Observe objects at wavelengths other than visible (to eliminate problems caused by dust, gas, other galactic bodies, etc), and catalogue their directions and distances ...
... Our Milky Way I. Select bright objects that you can see throughout the Milky Way and trace their directions and distances II. Observe objects at wavelengths other than visible (to eliminate problems caused by dust, gas, other galactic bodies, etc), and catalogue their directions and distances ...
The galactic metallicity gradient Martín Hernández, Nieves Leticia
... discovered a large number of these star forming clouds scattered across the Milky Way. In some cases, these clouds appear as dark regions silhouetted against a glowing background nebulosity, such as the Horsehead Nebula (Figure 3 left). In other cases, they appear as dark patches that obscure the ba ...
... discovered a large number of these star forming clouds scattered across the Milky Way. In some cases, these clouds appear as dark regions silhouetted against a glowing background nebulosity, such as the Horsehead Nebula (Figure 3 left). In other cases, they appear as dark patches that obscure the ba ...
HR Diagram Explorer Worksheet
... Open the HR Diagram Explorer. Begin by familiarizing yourself with the capabilities of the HertzsprungRussell Diagram Explorer through experimentation. An actual HR Diagram is provided in the upper right panel with an active location indicated by a red x. This active location can be dragged around ...
... Open the HR Diagram Explorer. Begin by familiarizing yourself with the capabilities of the HertzsprungRussell Diagram Explorer through experimentation. An actual HR Diagram is provided in the upper right panel with an active location indicated by a red x. This active location can be dragged around ...
Lesson Plan G2 The Stars
... good indicator of its distance. In Starry Night they will examine several different stars and they will see how some stars end their lives. ...
... good indicator of its distance. In Starry Night they will examine several different stars and they will see how some stars end their lives. ...
Oscillating White Dwarf Stars Background on White Dwarfs
... DO: Ionized helium strongest DZ: Metal lines dominate DQ: Carbon Features DX, DXP: Unidentified features (polarization) + temperature index = 50400/Teff ...
... DO: Ionized helium strongest DZ: Metal lines dominate DQ: Carbon Features DX, DXP: Unidentified features (polarization) + temperature index = 50400/Teff ...
PC3692: Physics of Stellar Structure (and Evolution)
... right. This sequence is called main sequence. You also see a clump of to the right of the main sequence, these stars are called red clump stars, and the stars further to the right, red giants. You can also vaguely see some stars in the bottom left; these are white dwarf stars, they are hot and very ...
... right. This sequence is called main sequence. You also see a clump of to the right of the main sequence, these stars are called red clump stars, and the stars further to the right, red giants. You can also vaguely see some stars in the bottom left; these are white dwarf stars, they are hot and very ...
Chapter 17 Measuring the Stars
... Measuring Stellar Masses in Binary Stars In order to measure stellar masses in a binary star, the period and semimajor axis of the orbit must be measured. Once this is done, Kepler’s third law gives the sum of the masses of the two stars. Then the relative speeds of the two stars can be measured usi ...
... Measuring Stellar Masses in Binary Stars In order to measure stellar masses in a binary star, the period and semimajor axis of the orbit must be measured. Once this is done, Kepler’s third law gives the sum of the masses of the two stars. Then the relative speeds of the two stars can be measured usi ...
Celebrating the centennial of a celestial yardstick
... Cloud has been prepared by Miss Leavitt.” The new, larger sample enabled Leavitt to find what she called “a remarkable relation between the brightness of these variables and the length of their periods.” Leavitt pointed out that since all the stars in the Small Magellanic Cloud are at nearly the sam ...
... Cloud has been prepared by Miss Leavitt.” The new, larger sample enabled Leavitt to find what she called “a remarkable relation between the brightness of these variables and the length of their periods.” Leavitt pointed out that since all the stars in the Small Magellanic Cloud are at nearly the sam ...
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.