Earth Science Exam Review 1
... A. Earth is billions of light-years away from the Milky Way Galaxy. B. Earth is part of a galaxy that is nearest to the Milky Way Galaxy. C. Earth is located in the Milky Way galaxy but far from the galaxy center. D. Earth is positioned in the center of the ...
... A. Earth is billions of light-years away from the Milky Way Galaxy. B. Earth is part of a galaxy that is nearest to the Milky Way Galaxy. C. Earth is located in the Milky Way galaxy but far from the galaxy center. D. Earth is positioned in the center of the ...
Goal: To understand how stars form.
... collapse and not from nuclear fusion like an adult star. • Eventually, the pressure and density at the core of this protostar increase. This increases the collisions of particles at its core. • This causes the core to heat up quickly. ...
... collapse and not from nuclear fusion like an adult star. • Eventually, the pressure and density at the core of this protostar increase. This increases the collisions of particles at its core. • This causes the core to heat up quickly. ...
star brightness
... Canis minoris (The Sm star of the constellation ion of Orion. near the great constellat ary stars, like our Sun, but bin Many stars are not single of sum the Their brightness is or multiple star systems. ponent stars. the brightness of the com n. htness in a regular patter Some stars change brig ...
... Canis minoris (The Sm star of the constellation ion of Orion. near the great constellat ary stars, like our Sun, but bin Many stars are not single of sum the Their brightness is or multiple star systems. ponent stars. the brightness of the com n. htness in a regular patter Some stars change brig ...
THE HERTZSPRUNG-RUSSELL DIAGRAM (H
... NOTE: Absolute Magnitude IS THE SAME THING AS LUMINOSITY ON THE GRAPH DEFINE: absolute magnitude (Pg. 372 if you don’t know) ...
... NOTE: Absolute Magnitude IS THE SAME THING AS LUMINOSITY ON THE GRAPH DEFINE: absolute magnitude (Pg. 372 if you don’t know) ...
Stars
... • If you know how luminous a star REALLY is and how bright it looks from Earth, you can determine how far away it must be to look that faint. • For any star in the sky, we KNOW: – Apparent Magnitude – Spectral Type (O, B, A, F, G, K, M) – Luminosity Class (Main Sequence, Giant, etc…). These are deno ...
... • If you know how luminous a star REALLY is and how bright it looks from Earth, you can determine how far away it must be to look that faint. • For any star in the sky, we KNOW: – Apparent Magnitude – Spectral Type (O, B, A, F, G, K, M) – Luminosity Class (Main Sequence, Giant, etc…). These are deno ...
Starry Night¨ Times - October 2008
... main sequence star that shines 9,000 times as brightly as our own sun. Good thing it's 432 lightyears away. ...
... main sequence star that shines 9,000 times as brightly as our own sun. Good thing it's 432 lightyears away. ...
File
... plural of supernova), known as Type II (they show hydrogen lines in their spectra, unlike Type I supernovae), mark the violent death of heavyweight stars that have retained at least part of their outer layer of hydrogen. Since the fundamental physical mechanism is the collapse of the iron core, they ...
... plural of supernova), known as Type II (they show hydrogen lines in their spectra, unlike Type I supernovae), mark the violent death of heavyweight stars that have retained at least part of their outer layer of hydrogen. Since the fundamental physical mechanism is the collapse of the iron core, they ...
Life Cycle of a Star - Intervention Worksheet
... A dying red super giant star can suddenly explode. The explosion is called a supernova. After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes whe ...
... A dying red super giant star can suddenly explode. The explosion is called a supernova. After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes whe ...
AST 301 Introduction to Astronomy - University of Texas Astronomy
... 200 pc, but you don’t need to know that.) The more distant star (Spica) appears fainter. Since it is twice as distant as Canopus, it appears 4 times fainter, or ¼ as bright. We could use the magnitude system to describe how much fainter Spica is than Canopus, but I prefer to talk about fluxes instea ...
... 200 pc, but you don’t need to know that.) The more distant star (Spica) appears fainter. Since it is twice as distant as Canopus, it appears 4 times fainter, or ¼ as bright. We could use the magnitude system to describe how much fainter Spica is than Canopus, but I prefer to talk about fluxes instea ...
TYPES OF STARS
... When astronomers look through their telescopes, they see billions of stars. What can they learn from their observations? In class, we’ve learned that the shape of the spectrum (especially, the wavelength at which it reaches its maximum intensity) can be used to determine a star’s temperature. In add ...
... When astronomers look through their telescopes, they see billions of stars. What can they learn from their observations? In class, we’ve learned that the shape of the spectrum (especially, the wavelength at which it reaches its maximum intensity) can be used to determine a star’s temperature. In add ...
HW #4 (due March 27)
... When astronomers look through their telescopes, they see billions of stars. What can they learn from their observations? In class, we’ve learned that the shape of the spectrum (especially, the wavelength at which it reaches its maximum intensity) can be used to determine a star’s temperature. In add ...
... When astronomers look through their telescopes, they see billions of stars. What can they learn from their observations? In class, we’ve learned that the shape of the spectrum (especially, the wavelength at which it reaches its maximum intensity) can be used to determine a star’s temperature. In add ...
Yes - Wichita State University
... 1. We obtain a new O/H gradient of -0.058 +/- .006 dex kpc-1. 2. A good linear model of the data requires the assumption of natural scatter. 3. Observed gradient range ~ -0.02 to -0.06 dex kpc-1. We are at the confusion limit. ...
... 1. We obtain a new O/H gradient of -0.058 +/- .006 dex kpc-1. 2. A good linear model of the data requires the assumption of natural scatter. 3. Observed gradient range ~ -0.02 to -0.06 dex kpc-1. We are at the confusion limit. ...
slides
... Cosmic address of the Earth: Cosmic Web → Virgo super cluster → Local group of clusters → Milky way→ Solar System → Earth Our ancestors thought Earth was at the center and rest of the universe revolved around it. Now we know we are so insignificant compared to the Universe! ...
... Cosmic address of the Earth: Cosmic Web → Virgo super cluster → Local group of clusters → Milky way→ Solar System → Earth Our ancestors thought Earth was at the center and rest of the universe revolved around it. Now we know we are so insignificant compared to the Universe! ...
Homework #3 10 points Question #1 (2 pts) The brightest star in the
... Thermonuclear supernova is an explosion of a white dwarf, which is less massive than a progenitor of a core-collapse supernova. Which produces a larger fractional abundance of iron? You can think the following way: let’s imagine that in a region of space A we found one massive star that exploded as ...
... Thermonuclear supernova is an explosion of a white dwarf, which is less massive than a progenitor of a core-collapse supernova. Which produces a larger fractional abundance of iron? You can think the following way: let’s imagine that in a region of space A we found one massive star that exploded as ...
H-R diagram worksheet
... Mark each of the following on the H-R diagram and label it as indicated. You may use page 15 of your ESRT to help you. 6. Draw and label a long diagonal line showing the approximate location of the main sequence. 7. A large circle indicating the area where you find the biggest diameter stars, labele ...
... Mark each of the following on the H-R diagram and label it as indicated. You may use page 15 of your ESRT to help you. 6. Draw and label a long diagonal line showing the approximate location of the main sequence. 7. A large circle indicating the area where you find the biggest diameter stars, labele ...
PH607lec07
... brighter spiral nebulae spectroscopically. Spectra show emission lines from hot gas, absorption lines from stars. Radial velocities are nearly all positive with values up to several hundred km/s - later to be determined to be due to the expansion of the Universe. 1915: Harlow Shapley (1885-1972) use ...
... brighter spiral nebulae spectroscopically. Spectra show emission lines from hot gas, absorption lines from stars. Radial velocities are nearly all positive with values up to several hundred km/s - later to be determined to be due to the expansion of the Universe. 1915: Harlow Shapley (1885-1972) use ...
Our Sun, Sol - Hobbs High School
... Stellar Old Age Depends on Mass • Stars with masses near our Sun’s, when they have completed helium fusing and have a carbon core, expand again into a red giant. • They ‘puff’ off their outer layers which spread out at 20 to 30 km/s, leaving the core behind. These layers are illuminated by light fr ...
... Stellar Old Age Depends on Mass • Stars with masses near our Sun’s, when they have completed helium fusing and have a carbon core, expand again into a red giant. • They ‘puff’ off their outer layers which spread out at 20 to 30 km/s, leaving the core behind. These layers are illuminated by light fr ...
Characteristics of Stars ppt.
... it’s not hot or cool it’s not large or small. We can compare stars by color, temperature, size, brightness and spectrum. ...
... it’s not hot or cool it’s not large or small. We can compare stars by color, temperature, size, brightness and spectrum. ...
Spectral line mapping of the Milky Way
... of weaker maser components, tracing kinematics and magnetic fields over a more extended region. These observations will also uncover the whole catalog of some particularly interesting OH-emitting evolved objects, of which very few members are known so far, such as post-AGB stars undergoing collimate ...
... of weaker maser components, tracing kinematics and magnetic fields over a more extended region. These observations will also uncover the whole catalog of some particularly interesting OH-emitting evolved objects, of which very few members are known so far, such as post-AGB stars undergoing collimate ...
Spectroscopy in stellar astrophysics
... ASTROPHYSICS : studies the physics of stars, stellar systems and interstellar material. ...
... ASTROPHYSICS : studies the physics of stars, stellar systems and interstellar material. ...
Lecture 9: Stellar Spectra
... Example: the Effects of Dust There is gas and dust in between the stars. Dust particles are very small and scatter blue light more efficiently than red light. Most stars appear to be REDDER than they really are. A star’s color no longer tells you its tempertuare. But the spectrum still does! ...
... Example: the Effects of Dust There is gas and dust in between the stars. Dust particles are very small and scatter blue light more efficiently than red light. Most stars appear to be REDDER than they really are. A star’s color no longer tells you its tempertuare. But the spectrum still does! ...
Answer Key 2
... No justification is necessary. It follows from paragraph 4 (lines 27-33) that W.Herschel a. was the first to use the term planetary nebulae. True/False b. noticed the resemblance between stars and planetary nebulae. True/False c. made mistaken assumptions about the origin of the planetary nebulae. T ...
... No justification is necessary. It follows from paragraph 4 (lines 27-33) that W.Herschel a. was the first to use the term planetary nebulae. True/False b. noticed the resemblance between stars and planetary nebulae. True/False c. made mistaken assumptions about the origin of the planetary nebulae. T ...
3. Galactic Dynamics handout 3 Aim: understand equilibrium of
... Spitzer found for many systems that rg = 2.5rh , where rh is the radius which contains half the mass Virial theorom implies: GM 2 M hv i = rg ...
... Spitzer found for many systems that rg = 2.5rh , where rh is the radius which contains half the mass Virial theorom implies: GM 2 M hv i = rg ...
Photometric Mass-to-Light Ratio In addition to a population`s total
... Another useful quantity to know is the rate of mass loss from stars as a function of time. As before, the key to calculating this is to realize that almost all the mass lost from stars comes during the post main-sequence phase of evolution. Thus, the rate at which a population of stars loses mass is ...
... Another useful quantity to know is the rate of mass loss from stars as a function of time. As before, the key to calculating this is to realize that almost all the mass lost from stars comes during the post main-sequence phase of evolution. Thus, the rate at which a population of stars loses mass is ...
H II region
An H II region is a large, low-density cloud of partially ionized gas in which star formation has recently taken place. The short-lived blue stars forged in these regions emit copious amounts of ultraviolet light that ionize the surrounding gas. H II regions—sometimes several hundred light-years across—are often associated with giant molecular clouds. The first known H II region was the Orion Nebula, which was discovered in 1610 by Nicolas-Claude Fabri de Peiresc.H II regions are named for the large amount of ionised atomic hydrogen they contain, referred to as H II, pronounced H-two by astronomers (an H I region being neutral atomic hydrogen, and H2 being molecular hydrogen). Such regions have extremely diverse shapes, because the distribution of the stars and gas inside them is irregular. They often appear clumpy and filamentary, sometimes showing bizarre shapes such as the Horsehead Nebula. H II regions may give birth to thousands of stars over a period of several million years. In the end, supernova explosions and strong stellar winds from the most massive stars in the resulting star cluster will disperse the gases of the H II region, leaving behind a cluster of birthed stars such as the Pleiades.H II regions can be seen to considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of other galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In the spiral galaxies, including the Milky Way, H II regions are concentrated in the spiral arms, while in the irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.