binary stars - El Camino College
... Two-thirds of all stars are part of multiple star systems, where two or more stars are born at the same time from the same gas cloud. Only about 30% of all stars are single, like the Sun. The distances between companion stars ranges from less than 10 million miles (0.1 AU), to over 10,000 AU. Simila ...
... Two-thirds of all stars are part of multiple star systems, where two or more stars are born at the same time from the same gas cloud. Only about 30% of all stars are single, like the Sun. The distances between companion stars ranges from less than 10 million miles (0.1 AU), to over 10,000 AU. Simila ...
Lecture 13 - Main Sequence Stars
... • The idea of the “Vogt-Russell” theorem for stars is that there is only one way to make a star with a given mass and chemical composition – if we start with a just formed protostar of a given mass and chemical composition, we can calculate how that star will evolve over its entire life. • This is e ...
... • The idea of the “Vogt-Russell” theorem for stars is that there is only one way to make a star with a given mass and chemical composition – if we start with a just formed protostar of a given mass and chemical composition, we can calculate how that star will evolve over its entire life. • This is e ...
Small Wonders: Andromeda
... there - especially when you compare it to the two foreground stars that flank it. At mag 13.7, it's a somewhat dim target tho, so the more aperture you can throw at this, the better your chances of finding it. It's certainly doable in a 10" scope from a decent site, and more than likely is catchable ...
... there - especially when you compare it to the two foreground stars that flank it. At mag 13.7, it's a somewhat dim target tho, so the more aperture you can throw at this, the better your chances of finding it. It's certainly doable in a 10" scope from a decent site, and more than likely is catchable ...
Today`s Powerpoint
... temperature from spectrum (black-body curve or spectral lines), then find surface area, then find radius (sphere surface area is 4 p R2) ...
... temperature from spectrum (black-body curve or spectral lines), then find surface area, then find radius (sphere surface area is 4 p R2) ...
January SKY Newsletter 2012
... then reverse direction and wind up back in Leo by early February. This change in position illustrates the retrograde motion of Mars. January is an excellent time to view Mars through a telescope if you want to see the north polar cap and possibly some surface markings. This is also a good time to vi ...
... then reverse direction and wind up back in Leo by early February. This change in position illustrates the retrograde motion of Mars. January is an excellent time to view Mars through a telescope if you want to see the north polar cap and possibly some surface markings. This is also a good time to vi ...
Life Cycle of a Star notes
... As the protostar continues to collapse due to gravity, it will attract more atoms and continually increase in mass and density. The increased density and gravity will cause the core temperature to eventually ...
... As the protostar continues to collapse due to gravity, it will attract more atoms and continually increase in mass and density. The increased density and gravity will cause the core temperature to eventually ...
Slide 1
... approximately the same age! More massive stars evolve more quickly than less massive ones. ...
... approximately the same age! More massive stars evolve more quickly than less massive ones. ...
HR Diagram and Stellar Fusion
... • http://rainman.astro.uiuc.edu/ddr/stellar/arc hive/suntrackson.mpg ...
... • http://rainman.astro.uiuc.edu/ddr/stellar/arc hive/suntrackson.mpg ...
Notes - Bill Wolf
... Absolute and Apparent Magnitude Obviously how bright a star appears on earth is only somewhat related to how bright the star actually is, since varying distances can make a star appear brighter or dimmer. Astronomer then use the word brightness generically to talk about how bright a star appears fro ...
... Absolute and Apparent Magnitude Obviously how bright a star appears on earth is only somewhat related to how bright the star actually is, since varying distances can make a star appear brighter or dimmer. Astronomer then use the word brightness generically to talk about how bright a star appears fro ...
docx - STAO
... galaxies), using appropriate scientific terminology and units (e.g., astronomical units, scientific notation, light years) ...
... galaxies), using appropriate scientific terminology and units (e.g., astronomical units, scientific notation, light years) ...
Chapter 12 Stellar Evolution
... Summary of Chapter 12 • Once hydrogen is gone in the core, a star burns hydrogen in the surrounding shell. The core contracts and heats; the outer atmosphere expands and cools. • Helium begins to fuse in the core, as a helium flash. The star expands into a red giant as the core continues to collaps ...
... Summary of Chapter 12 • Once hydrogen is gone in the core, a star burns hydrogen in the surrounding shell. The core contracts and heats; the outer atmosphere expands and cools. • Helium begins to fuse in the core, as a helium flash. The star expands into a red giant as the core continues to collaps ...
For instance, two hydrogen atoms may fuse together to form one
... For instance, two hydrogen atoms may fuse together to form one helium atom. The process by which light elements fuse into heavier ones is called nuclear fusion. Nuclear fusion releases huge amounts of energy. When the core of a clump becomes a hot, dense ball of hydrogen gas fusing into helium gas, ...
... For instance, two hydrogen atoms may fuse together to form one helium atom. The process by which light elements fuse into heavier ones is called nuclear fusion. Nuclear fusion releases huge amounts of energy. When the core of a clump becomes a hot, dense ball of hydrogen gas fusing into helium gas, ...
Slide 1 - Physics @ IUPUI
... • There is one more thing to change spin • Sometimes there is a break in the crust that can make the star shrink down a little bit or change its state • This makes it spin faster usually. ...
... • There is one more thing to change spin • Sometimes there is a break in the crust that can make the star shrink down a little bit or change its state • This makes it spin faster usually. ...
Space The Life of a Star
... High-mass stars explode after their red giant stage. If the star is massive enough, it will eventually become a black hole. Other high-mass red giants may become neutron stars. A neutron star is usually only 12 miles (20 kilometers) across, but its gravity is thousands of times stronger than Earth’s ...
... High-mass stars explode after their red giant stage. If the star is massive enough, it will eventually become a black hole. Other high-mass red giants may become neutron stars. A neutron star is usually only 12 miles (20 kilometers) across, but its gravity is thousands of times stronger than Earth’s ...
Measuring the distance to Galaxies
... variables can be determined by parallax (a method you will learn in this course) The inverse square law and the periodluminosity relationship of Henrietta Leavitt enables the distance of all observable Cepheid variables to be determined ...
... variables can be determined by parallax (a method you will learn in this course) The inverse square law and the periodluminosity relationship of Henrietta Leavitt enables the distance of all observable Cepheid variables to be determined ...
Properties of Stars Name
... against its absolute magnitude. From such a diagram, other information about a star’s properties and life cycle can be determined. In this lab, you will construct an H-R diagram using data on the 20 stars that are nearest to our sun (Figure 21.1) and the 20 stars that appear brightest in our sky (Fi ...
... against its absolute magnitude. From such a diagram, other information about a star’s properties and life cycle can be determined. In this lab, you will construct an H-R diagram using data on the 20 stars that are nearest to our sun (Figure 21.1) and the 20 stars that appear brightest in our sky (Fi ...
Science Olympiad 2008 Reach for the Stars Division B
... most determines how they will differ? A) location where they are formed B) time they are formed C) luminosity they are formed with D) mass they are formed with E) color they are formed with 111. The spectral sequence sorts stars according to: (choose as many as apply) A) mass B) surface temperature ...
... most determines how they will differ? A) location where they are formed B) time they are formed C) luminosity they are formed with D) mass they are formed with E) color they are formed with 111. The spectral sequence sorts stars according to: (choose as many as apply) A) mass B) surface temperature ...
giant molecular clouds
... Star formation collapse of the cores of giant molecular clouds: Dark, cold, dense clouds obscuring the light of stars behind them. ...
... Star formation collapse of the cores of giant molecular clouds: Dark, cold, dense clouds obscuring the light of stars behind them. ...
Stellar Evolution - Academic Computer Center
... depends on their mass. The H-R diagram showing the • Almost the entire lifetime Main Sequence line (in purple). of a star is spent on the More massive stars are to the upper left, Main Sequence. less massive stars to the lower right. ...
... depends on their mass. The H-R diagram showing the • Almost the entire lifetime Main Sequence line (in purple). of a star is spent on the More massive stars are to the upper left, Main Sequence. less massive stars to the lower right. ...
The Earth`s Orbit and Season Demonstration
... 3. Looking at the Sun notice the constellation directly across from the Sun, Gemini. On June 21 when the Sun appears in the constellation Gemini this is the first day of summer. Rotate the earth on its axis until North America is directly opposite the sun, midnight. Notice the constellation directly ...
... 3. Looking at the Sun notice the constellation directly across from the Sun, Gemini. On June 21 when the Sun appears in the constellation Gemini this is the first day of summer. Rotate the earth on its axis until North America is directly opposite the sun, midnight. Notice the constellation directly ...
The Life of a Star
... If a star, like our sun, does not have much mass in it, it is called a low-mass star. For low-mass stars, when the helium becomes carbon, the center of the star shrinks even more, and the outer layers are pushed far away. The core of a lowmass star becomes a white dwarf, which means it is much small ...
... If a star, like our sun, does not have much mass in it, it is called a low-mass star. For low-mass stars, when the helium becomes carbon, the center of the star shrinks even more, and the outer layers are pushed far away. The core of a lowmass star becomes a white dwarf, which means it is much small ...
Stars and Constellations Power Point
... •A black hole is a region of spacetime from which nothing, not even light, can escape. •Black holes of stellar mass are expected to form when very massive stars collapse at the end of their life cycle. •After a black hole has formed it can continue to grow by absorbing mass from its surroundings. •T ...
... •A black hole is a region of spacetime from which nothing, not even light, can escape. •Black holes of stellar mass are expected to form when very massive stars collapse at the end of their life cycle. •After a black hole has formed it can continue to grow by absorbing mass from its surroundings. •T ...
The star and the trees prostrate
... core that eventually cools and contracts gravitationally to about the size of the Earth. The result is a white dwarf: the more massive it is, the greater its inward gravitational pull, and the smaller it becomes. A teaspoonful of white dwarf material would weigh five-and-a-half tons or more in the E ...
... core that eventually cools and contracts gravitationally to about the size of the Earth. The result is a white dwarf: the more massive it is, the greater its inward gravitational pull, and the smaller it becomes. A teaspoonful of white dwarf material would weigh five-and-a-half tons or more in the E ...
Perseus (constellation)
Perseus, named after the Greek mythological hero Perseus, is a constellation in the northern sky. It was one of 48 listed by the 2nd-century astronomer Ptolemy and among the 88 modern constellations defined by the International Astronomical Union (IAU). It is located in the northern celestial hemisphere near several other constellations named after legends surrounding Perseus, including Andromeda to the west and Cassiopeia to the north. Perseus is also bordered by Aries and Taurus to the south, Auriga to the east, Camelopardalis to the north, and Triangulum to the west.The galactic plane of the Milky Way passes through Perseus but is mostly obscured by molecular clouds. The constellation's brightest star is the yellow-white supergiant Alpha Persei (also called Mirfak), which shines at magnitude 1.79. It and many of the surrounding stars are members of an open cluster known as the Alpha Persei Cluster. The best-known star, however, is Algol (Beta Persei), linked with ominous legends because of its variability, which is noticeable to the naked eye. Rather than being an intrinsically variable star, it is an eclipsing binary. Other notable star systems in Perseus include X Persei, a binary system containing a neutron star, and GK Persei, a nova that peaked at magnitude 0.2 in 1901. The Double Cluster, comprising two open clusters quite near each other in the sky, was known to the ancient Chinese. The constellation gives its name to the Perseus Cluster (Abell 426), a massive galaxy cluster located 250 million light-years from Earth. It hosts the radiant of the annual Perseids meteor shower—one of the most prominent meteor showers in the sky.