Chapter 28 Vocabulary
... Main sequence star - A star that is at the point in its life cycle in which it is actively fusing hydrogen nuclei into helium nuclei; also the band of the Hertzsprun-Russell diagram depicting such stars. ...
... Main sequence star - A star that is at the point in its life cycle in which it is actively fusing hydrogen nuclei into helium nuclei; also the band of the Hertzsprun-Russell diagram depicting such stars. ...
Measuring Stellar Distances
... moment – suppose you had no prior knowledge of what stars actually were – that you lived in a time where they could be anything. If you simply look up into the night sky you have no idea how far away these objects are or whether or not they are part of our atmosphere, in our solar system, or located ...
... moment – suppose you had no prior knowledge of what stars actually were – that you lived in a time where they could be anything. If you simply look up into the night sky you have no idea how far away these objects are or whether or not they are part of our atmosphere, in our solar system, or located ...
Chapter 24 Vocabulary
... 2. magnitude- in earthquake studies, a measure of the energy released by an earthquake; the Richter scale is used to describe earthquake magnitude 3. parallax- the apparent shift in position of an object when viewed from two different points, such as your left eye and right eye 4. light-year- unit u ...
... 2. magnitude- in earthquake studies, a measure of the energy released by an earthquake; the Richter scale is used to describe earthquake magnitude 3. parallax- the apparent shift in position of an object when viewed from two different points, such as your left eye and right eye 4. light-year- unit u ...
Document
... Mizar, 88 light years distant, is the middle star in the handle of the Big Dipper. It was the first binary star system to be imaged with a telescope. Spectroscopic observations show periodic Doppler shifts in the spectra of Mizar A and B, indicating that they are each binary stars. But they were too ...
... Mizar, 88 light years distant, is the middle star in the handle of the Big Dipper. It was the first binary star system to be imaged with a telescope. Spectroscopic observations show periodic Doppler shifts in the spectra of Mizar A and B, indicating that they are each binary stars. But they were too ...
Stars
... Mizar, 88 light years distant, is the middle star in the handle of the Big Dipper. It was the first binary star system to be imaged with a telescope. Spectroscopic observations show periodic Doppler shifts in the spectra of Mizar A and B, indicating that they are each binary stars. But they were too ...
... Mizar, 88 light years distant, is the middle star in the handle of the Big Dipper. It was the first binary star system to be imaged with a telescope. Spectroscopic observations show periodic Doppler shifts in the spectra of Mizar A and B, indicating that they are each binary stars. But they were too ...
22DistanceMotion
... night. Some of these change with very regular patterns. – For one kind of variable star, called Cepheid variables, one finds from nearby objects with parallax, that there is relation between variation period and intrinsic brightness – The nice thing about Cepheids is they are intrinsically very brig ...
... night. Some of these change with very regular patterns. – For one kind of variable star, called Cepheid variables, one finds from nearby objects with parallax, that there is relation between variation period and intrinsic brightness – The nice thing about Cepheids is they are intrinsically very brig ...
Parallax class activity (in MSword)
... Parallax class activity. How far away are the stars? Fun with Math! person 1: Measure out some distance X, and stand at point 1. This is like the distance to a star, which in real life we can’t measure with a tape measure!. (If there is time, we will do two distances, one quite short, say 10 feet, a ...
... Parallax class activity. How far away are the stars? Fun with Math! person 1: Measure out some distance X, and stand at point 1. This is like the distance to a star, which in real life we can’t measure with a tape measure!. (If there is time, we will do two distances, one quite short, say 10 feet, a ...
ASTR 553/554 (1) : Questions
... When your supervisor next asks you whether you have "fire in the belly" for your work, you can honestly reply, "more, even, than the sun and stars!" (4) Alien Astronomers in Virgo study the Milky Way Galaxy disks often have exponential surface brightness profiles: I(R) = I(0) exp(-R/Rd), where Rd is ...
... When your supervisor next asks you whether you have "fire in the belly" for your work, you can honestly reply, "more, even, than the sun and stars!" (4) Alien Astronomers in Virgo study the Milky Way Galaxy disks often have exponential surface brightness profiles: I(R) = I(0) exp(-R/Rd), where Rd is ...
Review Quiz No. 17
... The radius in the interior of a star where fusion processes can no longer take place. The point in time of a star’s life when nuclear fusion of hydrogen into helium ceases. The point in time of a star’s life when nuclear fusion processes cease alltogether. The point in a rotating star cluster beyond ...
... The radius in the interior of a star where fusion processes can no longer take place. The point in time of a star’s life when nuclear fusion of hydrogen into helium ceases. The point in time of a star’s life when nuclear fusion processes cease alltogether. The point in a rotating star cluster beyond ...
Chapter 21 power point - Laconia School District
... the upper left to the lower right and includes more than 90% of all stars. ...
... the upper left to the lower right and includes more than 90% of all stars. ...
AGN-Hubble
... The Hubble Constant and the Age of the Universe If you plot the scale of the Universe vs time, the Hubble constant is the slope of the line now. If it’s really constant, then the age of the Universe is just 1/H [since H=v/D=(d/t)/d]. That’s because if you know how fast we are expanding, you can run ...
... The Hubble Constant and the Age of the Universe If you plot the scale of the Universe vs time, the Hubble constant is the slope of the line now. If it’s really constant, then the age of the Universe is just 1/H [since H=v/D=(d/t)/d]. That’s because if you know how fast we are expanding, you can run ...
Characteristics of Stars
... Star Brightness (magnitude) • Absolute Magnitude: the “Real” brightness of the star. How much light it really gives off.(Need to know the distance to the Star) • Apparent Magnitude: How bright the star appears to be. ...
... Star Brightness (magnitude) • Absolute Magnitude: the “Real” brightness of the star. How much light it really gives off.(Need to know the distance to the Star) • Apparent Magnitude: How bright the star appears to be. ...
Globular Clusters
... • CCDs can detect photons but not color so we used filters to detect photons of different wavelengths. ...
... • CCDs can detect photons but not color so we used filters to detect photons of different wavelengths. ...
3.6 spectral classes
... The method of parallax is used in measuring the distances to nearby stars. The position of a star is carefully determined relative to other stars. Six months later, when Earth’s revolution has carried telescopes halfway around the Sun, the star’s position is measured again. Nearby stars appear to sh ...
... The method of parallax is used in measuring the distances to nearby stars. The position of a star is carefully determined relative to other stars. Six months later, when Earth’s revolution has carried telescopes halfway around the Sun, the star’s position is measured again. Nearby stars appear to sh ...
Measuring the Hubble Constant through Cepheid Distances
... Cepheids, improved calibration • With improved Udalski data, adopted period-luminosity relations become: • And the true distance modulus for galaxies: • where ...
... Cepheids, improved calibration • With improved Udalski data, adopted period-luminosity relations become: • And the true distance modulus for galaxies: • where ...
Section 25.1 Properties of Stars
... Binary Stars and Stellar Mass A binary star is one of two stars revolving around a common center of mass under their mutual gravitational attraction. Binary stars are used to determine the star property most difficult to calculate—its mass. Common Center of Mass ...
... Binary Stars and Stellar Mass A binary star is one of two stars revolving around a common center of mass under their mutual gravitational attraction. Binary stars are used to determine the star property most difficult to calculate—its mass. Common Center of Mass ...
Astronomy word grid
... 38. The moon of Jupiter with an active volcano 40. The largest planet 42. The line in the sky along which the Sun and the planets move Down 1. An object with an escape velocity greater than the speed of light 2. A huge cloud of low density gas sometimes shining 3. A huge collection of some hundred t ...
... 38. The moon of Jupiter with an active volcano 40. The largest planet 42. The line in the sky along which the Sun and the planets move Down 1. An object with an escape velocity greater than the speed of light 2. A huge cloud of low density gas sometimes shining 3. A huge collection of some hundred t ...
PPT
... galaxies - anaemic spirals. 2. Velocity distribution - in-falling population ? 3. Mean column density 1020 atoms cm-2. 4. What is the relation between the cluster/field luminosity function and HI mass function ? 5. What debris from the galaxy formation process has or is assembling itself into the c ...
... galaxies - anaemic spirals. 2. Velocity distribution - in-falling population ? 3. Mean column density 1020 atoms cm-2. 4. What is the relation between the cluster/field luminosity function and HI mass function ? 5. What debris from the galaxy formation process has or is assembling itself into the c ...
AN INTRODUCTION TO ASTRONOMY Dr. Uri Griv Department of Physics, Ben-Gurion University
... • The velocity dispersion V ≈ (3kT /m)1/2 or in q a stellar system PN V = (1/N ) i=1 (vi − v̄)2 where PN v̄ = (1/N ) i=1 vi is the mean velocity and N is the total number of stars • A true MB distribution has a “tail” • Stars will be lost from the cluster • The escape speed ve = 2V ...
... • The velocity dispersion V ≈ (3kT /m)1/2 or in q a stellar system PN V = (1/N ) i=1 (vi − v̄)2 where PN v̄ = (1/N ) i=1 vi is the mean velocity and N is the total number of stars • A true MB distribution has a “tail” • Stars will be lost from the cluster • The escape speed ve = 2V ...
Definitions
... Spectroscopy – is the systematic study of spectra and spectral lines Blackbody – is a hypothetical body that is a perfect absorber and emitter of EMR C spectrum – consists of a continuous range of frequencies w/o either bright or dark lines, appearing as a continuous range of colours E spectrum – co ...
... Spectroscopy – is the systematic study of spectra and spectral lines Blackbody – is a hypothetical body that is a perfect absorber and emitter of EMR C spectrum – consists of a continuous range of frequencies w/o either bright or dark lines, appearing as a continuous range of colours E spectrum – co ...
Ch. 27 Stars & Galaxies
... small dense area of neutrons = neutron star o Some may emit beams of radiation called pulsars ...
... small dense area of neutrons = neutron star o Some may emit beams of radiation called pulsars ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.