Chapter 18 Notes - Valdosta State University
... An artificial eclipse can be created using a coronograph. This is an instrument with an opaque disk that blocks out the light from the photosphere. It is used to study the chromosphere and corona. The corona is a tenuous, white halo surrounding the Sun that is only visible during a solar eclipse or ...
... An artificial eclipse can be created using a coronograph. This is an instrument with an opaque disk that blocks out the light from the photosphere. It is used to study the chromosphere and corona. The corona is a tenuous, white halo surrounding the Sun that is only visible during a solar eclipse or ...
Ch.1, Sec.3 - Mapping the Stars
... When you put those numbers together, you get an estimate of 1024 stars in the entire Universe or a 1 followed by 24 zeroes (called one septillion)! That’s 1,000,000,000,000,000,000,000,000 stars or more than all the combined grains of sand on planet Earth!!!! ...
... When you put those numbers together, you get an estimate of 1024 stars in the entire Universe or a 1 followed by 24 zeroes (called one septillion)! That’s 1,000,000,000,000,000,000,000,000 stars or more than all the combined grains of sand on planet Earth!!!! ...
Astronomy
... Red shift: as a source of visible light moves away from the observer, the wavelengths increase, creating a shift toward the red end of the visible spectrum. Star: a fixed luminous point in the night sky that is a large, remote incandescent body like the sun. Solar System: includes our Sun, the nine ...
... Red shift: as a source of visible light moves away from the observer, the wavelengths increase, creating a shift toward the red end of the visible spectrum. Star: a fixed luminous point in the night sky that is a large, remote incandescent body like the sun. Solar System: includes our Sun, the nine ...
Stars and Deep Time
... • The atoms that now form your body’s molecules came from substances here on Earth that were part of the nebula which formed our solar system 4.5 billion years ago! • These have been in many things before becoming part of you. • You are part of a larger process than you ever imagined! ...
... • The atoms that now form your body’s molecules came from substances here on Earth that were part of the nebula which formed our solar system 4.5 billion years ago! • These have been in many things before becoming part of you. • You are part of a larger process than you ever imagined! ...
Stellar Evolution 1 Star Formation 2 Nebulae
... tends to compress the star into a smaller volume), and gas pressure (which tends to expand the star into a larger volume. For the long middle period of a star’s life, these two opposing forces balance, and so the star is in a fairly constant state. The birth and death phases of a star’s life are typ ...
... tends to compress the star into a smaller volume), and gas pressure (which tends to expand the star into a larger volume. For the long middle period of a star’s life, these two opposing forces balance, and so the star is in a fairly constant state. The birth and death phases of a star’s life are typ ...
PHYS 2410 General Astronomy Homework 7
... 20. We know that the central object in a planetary nebula has a surface temperature of at least _________ because the nebula contains large amounts of ionized hydrogen. ...
... 20. We know that the central object in a planetary nebula has a surface temperature of at least _________ because the nebula contains large amounts of ionized hydrogen. ...
Galaxy clusters - University of Iowa Astrophysics
... source, we can figure out the total mass in the lens. This provides an independent confirmation of dark matter. • A lense can act as a huge telescope. The deepest images of the most distant galaxies are obtained with clusters acting as gravitational lenses. ...
... source, we can figure out the total mass in the lens. This provides an independent confirmation of dark matter. • A lense can act as a huge telescope. The deepest images of the most distant galaxies are obtained with clusters acting as gravitational lenses. ...
Today`s Powerpoint
... Determine luminosity from apparent brightness and distance, determine temperature from spectrum (black-body curve or spectral lines), then find surface area, then find radius (sphere surface area is 4 p R2) ...
... Determine luminosity from apparent brightness and distance, determine temperature from spectrum (black-body curve or spectral lines), then find surface area, then find radius (sphere surface area is 4 p R2) ...
The Milky Way Galaxy
... • The Milky Way galaxy is home to 400 billion stars and our own Sun and Solar System. • It is a barred spiral galaxy. • Scientists think the centre of the galaxy contains a super massive black hole. • The Milky Way is full of dust, gas and stars. • The Milky Way, along with everything else, is ...
... • The Milky Way galaxy is home to 400 billion stars and our own Sun and Solar System. • It is a barred spiral galaxy. • Scientists think the centre of the galaxy contains a super massive black hole. • The Milky Way is full of dust, gas and stars. • The Milky Way, along with everything else, is ...
Pre-Main Sequence Evolution
... The Milky Way has several thousand of these objects, each with masses of 104 M8< M < 107 M8, and sizes between 10 and 100 pc. Although the average density of these clouds is ~ 100 cm-3, these objects are very clumpy, with large numbers of colder, dense cores. Orion is the one of the nearest (but n ...
... The Milky Way has several thousand of these objects, each with masses of 104 M8< M < 107 M8, and sizes between 10 and 100 pc. Although the average density of these clouds is ~ 100 cm-3, these objects are very clumpy, with large numbers of colder, dense cores. Orion is the one of the nearest (but n ...
Slide 1 - Physics @ IUPUI
... somewhere. • Where does the energy the pulsars emit come from? • A) heat • B) nuclear fusion • C) gravity • D) Spin ...
... somewhere. • Where does the energy the pulsars emit come from? • A) heat • B) nuclear fusion • C) gravity • D) Spin ...
November 2008 - Otterbein University
... • Stars thinned out very fast at right angles to Milky Way • In the plane of the Milky Way the thinning was slower and depended upon the direction in which he looked ...
... • Stars thinned out very fast at right angles to Milky Way • In the plane of the Milky Way the thinning was slower and depended upon the direction in which he looked ...
100 X size of Sun - East Penn School District
... • In the magnitude scale, lower numbers are associated with brighter stars. • Star A has an apparent magnitude = 5.4 and star B has an apparent magnitude = 2.4. Which star is brighter? • We can't actually move stars around, but we can calculate how bright a star would be if placed at the agreed-upon ...
... • In the magnitude scale, lower numbers are associated with brighter stars. • Star A has an apparent magnitude = 5.4 and star B has an apparent magnitude = 2.4. Which star is brighter? • We can't actually move stars around, but we can calculate how bright a star would be if placed at the agreed-upon ...
Week 9 Concept Summary - UC Berkeley Astronomy w
... intrinsic luminosity and the mass: L ∝ M 4 , and the main sequence lifetime goes as t ∝ M −3 . Knowing the color of a main sequence star tells you the temperature, and uminosity, which in turn tells you the radius of the star and how far away it is. 3. Stellar Birth: Stars form out of giant gas clou ...
... intrinsic luminosity and the mass: L ∝ M 4 , and the main sequence lifetime goes as t ∝ M −3 . Knowing the color of a main sequence star tells you the temperature, and uminosity, which in turn tells you the radius of the star and how far away it is. 3. Stellar Birth: Stars form out of giant gas clou ...
Life Cycle of a Star
... massive they collapse into an object called a black hole • Light can not escape a black holes gravity because it is so massive • They are only detected through x-rays that can determine a black hole through materials from stars filtering ...
... massive they collapse into an object called a black hole • Light can not escape a black holes gravity because it is so massive • They are only detected through x-rays that can determine a black hole through materials from stars filtering ...
What are stars?
... Compare the development of a less-massive star with that of a more-massive star. ___________________________________________________________________ ___________________________________________________________________ ___________________________________________________________________ _______________ ...
... Compare the development of a less-massive star with that of a more-massive star. ___________________________________________________________________ ___________________________________________________________________ ___________________________________________________________________ _______________ ...
Revealing Galactic Scale Bars with the help of Galaxy Zoo
... Lintott et al. 2008) to identify a sample of local disc galaxies with reliable bar identifications. These data, combined with information on the atomic gas content from the ALFALFA survey (Haynes et al. 2011) show that disc galaxies with higher gas content have lower bar fractions. We use a gas defi ...
... Lintott et al. 2008) to identify a sample of local disc galaxies with reliable bar identifications. These data, combined with information on the atomic gas content from the ALFALFA survey (Haynes et al. 2011) show that disc galaxies with higher gas content have lower bar fractions. We use a gas defi ...
Chapter 8, Lesson 4, 2nd Packet, pdf
... Compare the development of a less-massive star with that of a more-massive star. ___________________________________________________________________ ___________________________________________________________________ ___________________________________________________________________ _______________ ...
... Compare the development of a less-massive star with that of a more-massive star. ___________________________________________________________________ ___________________________________________________________________ ___________________________________________________________________ _______________ ...
General Astronomy - Stockton University
... Although astronomy has been practiced for thousands of years, it consisted mostly of observing and cataloguing the motions of stars. The use of spectroscopy to determine the properties of stars (c.a. 1814) allowed astronomers to investigate the the stars scientifically. ...
... Although astronomy has been practiced for thousands of years, it consisted mostly of observing and cataloguing the motions of stars. The use of spectroscopy to determine the properties of stars (c.a. 1814) allowed astronomers to investigate the the stars scientifically. ...
Stages in the Life of a Star
... uses up the hydrogen in its core. This compresses and heats the core. (B)The heated core ignites the surrounding gas to make a shell source, and the outer layers of the star expand, turning it into a red giant. ...
... uses up the hydrogen in its core. This compresses and heats the core. (B)The heated core ignites the surrounding gas to make a shell source, and the outer layers of the star expand, turning it into a red giant. ...
PHYS-633: Problem set #2
... burning H in the shell around the hot He core. How long (in Myr) can it last in this stage before it doubles the amount given in part c for H consumed by core burning during the full main sequence. 4. Planetary nebula emission and expansion Suppose we observe the Hα line from a spherical planetary n ...
... burning H in the shell around the hot He core. How long (in Myr) can it last in this stage before it doubles the amount given in part c for H consumed by core burning during the full main sequence. 4. Planetary nebula emission and expansion Suppose we observe the Hα line from a spherical planetary n ...
Document
... All stars are huge balls of glowing gas that produce or have produced energy by fusion Stars differ in size, brightness, and temperature ...
... All stars are huge balls of glowing gas that produce or have produced energy by fusion Stars differ in size, brightness, and temperature ...
ASTR-1020: Astronomy II Course Lecture Notes - Faculty
... 1. The central nuclear region of the Galaxy is completely invisible at visible wavelengths due to dust and gas obscuration. 2. However, we can see it in radio waves, since dust and gas are transparent to radio waves. The center of the galaxy is the brightest radio source in the sky =⇒ called Sagitta ...
... 1. The central nuclear region of the Galaxy is completely invisible at visible wavelengths due to dust and gas obscuration. 2. However, we can see it in radio waves, since dust and gas are transparent to radio waves. The center of the galaxy is the brightest radio source in the sky =⇒ called Sagitta ...
Observational Overview
... NUCLEUS – centre of our Galaxy, and contains a 2 × 106 M black hole. The centre is totally obscured from direct view at visible λ’s because the dust scatters the starlight. We use infrared/radio observations to probe its nature. HALO – surrounds disk and has a radius of at least 50 kpc. It contains ...
... NUCLEUS – centre of our Galaxy, and contains a 2 × 106 M black hole. The centre is totally obscured from direct view at visible λ’s because the dust scatters the starlight. We use infrared/radio observations to probe its nature. HALO – surrounds disk and has a radius of at least 50 kpc. It contains ...
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.