HR DIAGRAM (Page 1) - McDonald Observatory
... instance, the faintest stars our eyes alone may see are apparent magnitude 6. A fairly bright star like Sirius is magnitude -1.4, while the sun is a blinding -26. For each single step up or down on the magnitude scale, the brightness changes by a factor of 2.512. And for every five steps, the bright ...
... instance, the faintest stars our eyes alone may see are apparent magnitude 6. A fairly bright star like Sirius is magnitude -1.4, while the sun is a blinding -26. For each single step up or down on the magnitude scale, the brightness changes by a factor of 2.512. And for every five steps, the bright ...
The Science of Life in the Universe (Chap 2
... Observations to be Explained Each radioactive nucleus decays at its own characteristic rate, known as its half-life, which can be measured in the laboratory. This is key to radioactive age dating, which is used to determine the ages of rocks. The oldest rocks found anywhere in the solar system ...
... Observations to be Explained Each radioactive nucleus decays at its own characteristic rate, known as its half-life, which can be measured in the laboratory. This is key to radioactive age dating, which is used to determine the ages of rocks. The oldest rocks found anywhere in the solar system ...
Document
... The observation that there are few spiral galaxies in areas of high galaxy density. ...
... The observation that there are few spiral galaxies in areas of high galaxy density. ...
Chapter 12
... During the early stages of a star formation the objects are called a protostars. The internal temperature is not high enough to produce fusion. These objects radiate energy away in the form of light. That energy comes from gravitational energy converted to heat. Once they reach the Main Sequence, T ...
... During the early stages of a star formation the objects are called a protostars. The internal temperature is not high enough to produce fusion. These objects radiate energy away in the form of light. That energy comes from gravitational energy converted to heat. Once they reach the Main Sequence, T ...
Lesson 4 - Scientist in Residence Program
... people a star’s colour and brightness is highly dependent on its size. We can get clues about how hot a star is and a star’s age from a star’s colour. Stars are often classified based on size, temperature and spectra (or its colour). There are 7 main types of stars: O, B, A, F, G, K and M (easy mnem ...
... people a star’s colour and brightness is highly dependent on its size. We can get clues about how hot a star is and a star’s age from a star’s colour. Stars are often classified based on size, temperature and spectra (or its colour). There are 7 main types of stars: O, B, A, F, G, K and M (easy mnem ...
The Science of Life in the Universe (Chap 2
... Observations to be Explained Each radioactive nucleus decays at its own characteristic rate, known as its half-life, which can be measured in the laboratory. This is key to radioactive age dating, which is used to determine the ages of rocks. The oldest rocks found anywhere in the solar system ...
... Observations to be Explained Each radioactive nucleus decays at its own characteristic rate, known as its half-life, which can be measured in the laboratory. This is key to radioactive age dating, which is used to determine the ages of rocks. The oldest rocks found anywhere in the solar system ...
Chapter 3 Notes
... Observations to be Explained Each radioactive nucleus decays at its own characteristic rate, known as its half-life, which can be measured in the laboratory. This is key to radioactive age dating, which is used to determine the ages of rocks. The oldest rocks found anywhere in the solar system ...
... Observations to be Explained Each radioactive nucleus decays at its own characteristic rate, known as its half-life, which can be measured in the laboratory. This is key to radioactive age dating, which is used to determine the ages of rocks. The oldest rocks found anywhere in the solar system ...
Document
... • Think about the continued evolution of Algol and you have the explanation for novae. • If the original primary transfers most of its mass to the original secondary, you are left with a massive main-sequence star and a helium WD. • When the original secondary starts to evolve up the RGB, it transfe ...
... • Think about the continued evolution of Algol and you have the explanation for novae. • If the original primary transfers most of its mass to the original secondary, you are left with a massive main-sequence star and a helium WD. • When the original secondary starts to evolve up the RGB, it transfe ...
Define the following terms in the space provided
... Stars are much larger than planets. Our Sun is over 100 times the radius of the Earth. There are stars some what smaller than the Sun and stars that are vastly larger than the Sun Star clusters come in two principle forms: open clusters and globular clusters. They may consist of several hundred to s ...
... Stars are much larger than planets. Our Sun is over 100 times the radius of the Earth. There are stars some what smaller than the Sun and stars that are vastly larger than the Sun Star clusters come in two principle forms: open clusters and globular clusters. They may consist of several hundred to s ...
Name: Period: ___ Date: ______ Light-year Calculation
... Distances are so great in space that a special unit of measurement is used. It is called a light-year. This sounds like a measurement of time, but it is a unit used to measure distance. By definition a light-year is the distance that light travels in one year. To calculate the distance of one light- ...
... Distances are so great in space that a special unit of measurement is used. It is called a light-year. This sounds like a measurement of time, but it is a unit used to measure distance. By definition a light-year is the distance that light travels in one year. To calculate the distance of one light- ...
Lecture102802 - FSU High Energy Physics
... gains a lot of energy “falling into” small, dense white dwarf heats up collects in shell on outside of white dwarf ...
... gains a lot of energy “falling into” small, dense white dwarf heats up collects in shell on outside of white dwarf ...
What we can measure
... really see them. This is possible for the nearer stars. We can actually see both stars individually and watch one orbit the other. These are called visual binaries. We need to be careful here, since some stars only appear to be close due to our perspective. These are called “optical doubles” and not ...
... really see them. This is possible for the nearer stars. We can actually see both stars individually and watch one orbit the other. These are called visual binaries. We need to be careful here, since some stars only appear to be close due to our perspective. These are called “optical doubles” and not ...
OUR UNIVERSE Problem Set 7 Solutions Question A1 Question A2
... (a) The hydrogen-burning main sequence phase, As the proto-star collapses under its own gravity its atoms (hydrogen about 70 % and helium about 25 %) heat up because they exchange gravitational potential energy for kinetic energy, eventually the atoms in the core reach temperatures of about 15 milli ...
... (a) The hydrogen-burning main sequence phase, As the proto-star collapses under its own gravity its atoms (hydrogen about 70 % and helium about 25 %) heat up because they exchange gravitational potential energy for kinetic energy, eventually the atoms in the core reach temperatures of about 15 milli ...
Stars, Galaxies, and the Universe Section 3 Stars, Galaxies, and the
... and are held together by gravity. The center of mass, or barycenter, is somewhere between the two stars. • In star systems that have more than two stars, two stars may revolve rapidly around a common barycenter, while a third star revolves more slowly at a greater distance from the pair. • Astronome ...
... and are held together by gravity. The center of mass, or barycenter, is somewhere between the two stars. • In star systems that have more than two stars, two stars may revolve rapidly around a common barycenter, while a third star revolves more slowly at a greater distance from the pair. • Astronome ...
ASTR3007/4007/6007, Class 1: Observing the Stars 23 February
... A low value of J − K is the opposite. Thus moving to the right on this diagram corresponds to getting redder, and moving left corresponds to getting bluer. The value of J − K is our proxy for temperature. The first thing to notice about the diagram is that the stars do not fall anything like random ...
... A low value of J − K is the opposite. Thus moving to the right on this diagram corresponds to getting redder, and moving left corresponds to getting bluer. The value of J − K is our proxy for temperature. The first thing to notice about the diagram is that the stars do not fall anything like random ...
MS Word version
... The following sequence of directions are steps an instructor might choose to follow in demonstrating the Eclipsing Binary Simulator in a classroom situation. We provide these suggestions with appropriate questions (shown in bold italics) to pose to the class as an aid in promoting interactivity. We ...
... The following sequence of directions are steps an instructor might choose to follow in demonstrating the Eclipsing Binary Simulator in a classroom situation. We provide these suggestions with appropriate questions (shown in bold italics) to pose to the class as an aid in promoting interactivity. We ...
Stellar Evolution
... force of gravity pulling in, and pressure from the heat of fusion pushing out. • Stars on the main sequence burn hydrogen in their core to produce heat. • Longest phase of a star’s life. ...
... force of gravity pulling in, and pressure from the heat of fusion pushing out. • Stars on the main sequence burn hydrogen in their core to produce heat. • Longest phase of a star’s life. ...
L11
... 3. The luminosity remains approximately constant in spite of internal changes. The track on the HRD is therefore horizontal. For a 15-25M stars we have seen a gradual redwards movement. But for higher mass (or stars with different initial compositions) the star back and forth between low and high e ...
... 3. The luminosity remains approximately constant in spite of internal changes. The track on the HRD is therefore horizontal. For a 15-25M stars we have seen a gradual redwards movement. But for higher mass (or stars with different initial compositions) the star back and forth between low and high e ...
Link again
... The second law is that a line joining a planet and the Sun sweeps out equal areas in equal intervals of time. The third law is that the squares of the sidereal periods of the planets are proportional to the cubes of their semimajor axes. An ellipse is an imperfect circle with a longest diameter call ...
... The second law is that a line joining a planet and the Sun sweeps out equal areas in equal intervals of time. The third law is that the squares of the sidereal periods of the planets are proportional to the cubes of their semimajor axes. An ellipse is an imperfect circle with a longest diameter call ...
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.