Lectures 10 & 11 powerpoint (stellar formation) [movie below]
... low density (n ~ 0.1 atom/cm3); gas can remain ionized because of very low density. ...
... low density (n ~ 0.1 atom/cm3); gas can remain ionized because of very low density. ...
Binary Stars (Professor Powerpoint)
... that the stars pass in front of each other as seen from the Earth. Each eclipse will cause the total light from the system to decrease. The amount of the decrease will depend on how much of each star is covered up. The period is from one large dip to the next and with the period you can get the mass ...
... that the stars pass in front of each other as seen from the Earth. Each eclipse will cause the total light from the system to decrease. The amount of the decrease will depend on how much of each star is covered up. The period is from one large dip to the next and with the period you can get the mass ...
Document
... Spectroscopy is a tool of astronomy in which the light produced by a star or other object (called its spectrum) is analyzed. ...
... Spectroscopy is a tool of astronomy in which the light produced by a star or other object (called its spectrum) is analyzed. ...
a star is born reading
... away. Some scientists think a supernova is what caused our Sun and solar system to form. There are also supergiant stars. They are like giants, only bigger. If our Sun was a supergiant, it would reach clear to Uranus. Dead supergiants often turn into black holes! As you wish upon that first star you ...
... away. Some scientists think a supernova is what caused our Sun and solar system to form. There are also supergiant stars. They are like giants, only bigger. If our Sun was a supergiant, it would reach clear to Uranus. Dead supergiants often turn into black holes! As you wish upon that first star you ...
Week 9 Concept Summary - UC Berkeley Astronomy w
... 2. Stellar Census: Not only do most stars lie on the Main Sequence, but they are also mostly cooler, smaller, red stars. Hot stars are easiest to see since they are brightest, but they are far less common in general. On the main sequence, we also find a relation between the intrinsic luminosity and ...
... 2. Stellar Census: Not only do most stars lie on the Main Sequence, but they are also mostly cooler, smaller, red stars. Hot stars are easiest to see since they are brightest, but they are far less common in general. On the main sequence, we also find a relation between the intrinsic luminosity and ...
The Hidden Lives of Galaxies NSTA 2001
... A Balancing Act Energy released from nuclear fusion counteracts inward force of gravity. ...
... A Balancing Act Energy released from nuclear fusion counteracts inward force of gravity. ...
Measuring the Stars
... Space is Big. “Space is big. Really big. You just won't believe how vastly hugely mind-bogglingly big it is. I mean, you may think it's a long way down the road to the chemist, but that's just peanuts to space…” To be fair though, when confronted by the sheer enormity of the distances between the s ...
... Space is Big. “Space is big. Really big. You just won't believe how vastly hugely mind-bogglingly big it is. I mean, you may think it's a long way down the road to the chemist, but that's just peanuts to space…” To be fair though, when confronted by the sheer enormity of the distances between the s ...
File
... HR STAR DIAGRAM OBJECTIVE: Compare a stars color, temperature, brightness, and size to its spectral class. PURPOSE: Plot stars according to brightness and temperature to create an HR diagram. PROCEDURES: 1. Study the star data table on the back. 2. The sun, used as a standard brightness, is given a ...
... HR STAR DIAGRAM OBJECTIVE: Compare a stars color, temperature, brightness, and size to its spectral class. PURPOSE: Plot stars according to brightness and temperature to create an HR diagram. PROCEDURES: 1. Study the star data table on the back. 2. The sun, used as a standard brightness, is given a ...
What color are stars?
... are found in a band from the upper left to the lower right • Giant and supergiant stars are found in the upper right corner • Tiny white dwarf stars are found in the lower left corner of the HR diagram ...
... are found in a band from the upper left to the lower right • Giant and supergiant stars are found in the upper right corner • Tiny white dwarf stars are found in the lower left corner of the HR diagram ...
HW #5 Answers (Due 9/29)
... massive stars, the fuel is used up in a matter of a couple million years. For less massive stars like the Sun, the fuel will last 10 billion years. And for really low mass stars, the fuel will last for hundreds of billions of years. In a star cluster, all the stars form at the same time. The first t ...
... massive stars, the fuel is used up in a matter of a couple million years. For less massive stars like the Sun, the fuel will last 10 billion years. And for really low mass stars, the fuel will last for hundreds of billions of years. In a star cluster, all the stars form at the same time. The first t ...
Stars and Galaxies
... • Nova stars are stars that suddenly increase in brightness and then get dim. • Neutron stars are the smallest stars of all. A typical neutron star has a diameter of only about 16 kilometers. • Surface temperature of a star can be determined by its color. Blue being very hot 35,000 oC and above and ...
... • Nova stars are stars that suddenly increase in brightness and then get dim. • Neutron stars are the smallest stars of all. A typical neutron star has a diameter of only about 16 kilometers. • Surface temperature of a star can be determined by its color. Blue being very hot 35,000 oC and above and ...
Document
... In the early part of this century, astronomer Ejnar Hertzsprung studied the luminosities and types of stars. Soon, he and American astronomer, Henry Russell, developed a graphical representation comparing a star’s temperature against its luminosity (also called absolute magnitude) and types of stars ...
... In the early part of this century, astronomer Ejnar Hertzsprung studied the luminosities and types of stars. Soon, he and American astronomer, Henry Russell, developed a graphical representation comparing a star’s temperature against its luminosity (also called absolute magnitude) and types of stars ...
Life Cycle of Stars
... Life Cycle of Stars • The matter inside the star will be compressed so tightly that its atoms are compacted into a dense shell of neutrons. If the remaining mass of the star is more than about three times that of the Sun, it will collapse so completely that it will literally disappear from the univ ...
... Life Cycle of Stars • The matter inside the star will be compressed so tightly that its atoms are compacted into a dense shell of neutrons. If the remaining mass of the star is more than about three times that of the Sun, it will collapse so completely that it will literally disappear from the univ ...
Stars and Temperature and Color
... surface of the star. • The same is true for the filament in a light bulb or any other hot object. In general, we call radiation from a hot body `black body’ radiation (do demonstration 6B40.10). ...
... surface of the star. • The same is true for the filament in a light bulb or any other hot object. In general, we call radiation from a hot body `black body’ radiation (do demonstration 6B40.10). ...
Astro 2 - Red Hook Central School District
... • Some radiation l absorbed by outer layers. • Can identify elements in outer layers. • If H is present, H will absorb l = to dif ...
... • Some radiation l absorbed by outer layers. • Can identify elements in outer layers. • If H is present, H will absorb l = to dif ...
Section 19.2
... of stars • If you look closely at the stars on a clear night, you might see a slight reddish or bluish tint to some stars. • This is because their surface temperatures are different. ...
... of stars • If you look closely at the stars on a clear night, you might see a slight reddish or bluish tint to some stars. • This is because their surface temperatures are different. ...
AN INTRODUCTION TO ASTRONOMY Dr. Uri Griv Department of Physics, Ben-Gurion University
... • Strictly speaking: L = (4πR2 )(σT 4 ) where R is the radius of a star. On the other hand, L = f · (4πr2 ) → T = (f r2 /R2 σ)1/4 • The basic idea of UBV Photometry is to measure the proportions of radiant energy put out by a thermal body at ultraviolet (U), blue (B), and visual (V) wavelength • fV ...
... • Strictly speaking: L = (4πR2 )(σT 4 ) where R is the radius of a star. On the other hand, L = f · (4πr2 ) → T = (f r2 /R2 σ)1/4 • The basic idea of UBV Photometry is to measure the proportions of radiant energy put out by a thermal body at ultraviolet (U), blue (B), and visual (V) wavelength • fV ...
Stellar Classification Worksheet 2
... Explain how each of the 5 characteristics in the boxes below is used to classify stars. In each box, give 2 examples of stars and their specific characteristics. Use pages 127-129 in the textbook and the examples below to complete the worksheet. ...
... Explain how each of the 5 characteristics in the boxes below is used to classify stars. In each box, give 2 examples of stars and their specific characteristics. Use pages 127-129 in the textbook and the examples below to complete the worksheet. ...
Announcements
... (~104 K) has large fraction of H atoms with excited electrons in the 2nd energy level Colder gas: electrons in lowest enery (ground) state Hotter gas: energetic collisions know electrons out of atom (ionized) ...
... (~104 K) has large fraction of H atoms with excited electrons in the 2nd energy level Colder gas: electrons in lowest enery (ground) state Hotter gas: energetic collisions know electrons out of atom (ionized) ...
File
... only form of energy we can detect with our _____ other forms of energy that come from stars are: ...
... only form of energy we can detect with our _____ other forms of energy that come from stars are: ...
Astronomy 252: Short Project 2 Stellar Spectra: Their Classification
... have temperatures on the order of 2000 - 3000 K. As you might guess, the appearance of the spectrum of a star is very strongly dependent on its temperature. For instance the very hottest stars (called the O-type stars) show absorption lines due to ionized helium (He II), and doubly and even triply i ...
... have temperatures on the order of 2000 - 3000 K. As you might guess, the appearance of the spectrum of a star is very strongly dependent on its temperature. For instance the very hottest stars (called the O-type stars) show absorption lines due to ionized helium (He II), and doubly and even triply i ...
characteristics of stars
... When a star ends its life it runs out of __________ and other fuels needed to produce energy. When this happens the star _________ _________ and begins to cool. RED GIANT - a star near the end of its life, that becomes larger and redder as it runs out of its hydrogen fuel. RED SUPERGIANT - a star wi ...
... When a star ends its life it runs out of __________ and other fuels needed to produce energy. When this happens the star _________ _________ and begins to cool. RED GIANT - a star near the end of its life, that becomes larger and redder as it runs out of its hydrogen fuel. RED SUPERGIANT - a star wi ...
Properties of stars: temperature, colour index and equivalent width
... color-temperature diagram and we have applied this relation to a large amount of stars to get easily their temperature. 2. Through the study of the spectrum of 10 stars at different temperatures we analyzed the trend of the equivalent width of the absorption lines Hα and CaII K, as a function of tem ...
... color-temperature diagram and we have applied this relation to a large amount of stars to get easily their temperature. 2. Through the study of the spectrum of 10 stars at different temperatures we analyzed the trend of the equivalent width of the absorption lines Hα and CaII K, as a function of tem ...
Stellar classification
In astronomy, stellar classification is the classification of stars based on their spectral characteristics. Light from the star is analyzed by splitting it with a prism or diffraction grating into a spectrum exhibiting the rainbow of colors interspersed with absorption lines. Each line indicates an ion of a certain chemical element, with the line strength indicating the abundance of that ion. The relative abundance of the different ions varies with the temperature of the photosphere. The spectral class of a star is a short code summarizing the ionization state, giving an objective measure of the photosphere's temperature and density.Most stars are currently classified under the Morgan–Keenan (MK) system using the letters O, B, A, F, G, K, and M, a sequence from the hottest (O type) to the coolest (M type). Each letter class is then subdivided using a numeric digit with 0 being hottest and 9 being coolest (e.g. A8, A9, F0, F1 form a sequence from hotter to cooler). The sequence has been expanded with classes for other stars and star-like objects that do not fit in the classical system, such class D for white dwarfs and class C for carbon stars.In the MK system a luminosity class is added to the spectral class using Roman numerals. This is based on the width of certain absorption lines in the star's spectrum which vary with the density of the atmosphere and so distinguish giant stars from dwarfs. Luminosity class 0 or Ia+ stars for hypergiants, class I stars for supergiants, class II for bright giants, class III for regular giants, class IV for sub-giants, class V for main-sequence stars, class sd for sub-dwarfs, and class D for white dwarfs. The full spectral class for the Sun is then G2V, indicating a main-sequence star with a temperature around 5,800K.