Astronomy 12 - hrsbstaff.ednet.ns.ca
... E. Estimate Main-Sequence Life of Sun. Estimate the main-sequence lifetime of the Sun: i.e., how long the Sun will burn hydrogen into helium in its core. Assume that the Sun was initially entirely composed of hydrogen, and that the Sun's current mass was its mass before main-sequence burning. You wi ...
... E. Estimate Main-Sequence Life of Sun. Estimate the main-sequence lifetime of the Sun: i.e., how long the Sun will burn hydrogen into helium in its core. Assume that the Sun was initially entirely composed of hydrogen, and that the Sun's current mass was its mass before main-sequence burning. You wi ...
7/3 Some stars were found in regions above the main sequence
... Giant Stars — about the same mass as main sequence stars but much larger — small densities — range form a hundredth to a tenth of the density of water. Supergiant Stars — still no more massive than main sequence stars but much much larger — 0.00000001 to 0.001 times the density of water. White Dwarf ...
... Giant Stars — about the same mass as main sequence stars but much larger — small densities — range form a hundredth to a tenth of the density of water. Supergiant Stars — still no more massive than main sequence stars but much much larger — 0.00000001 to 0.001 times the density of water. White Dwarf ...
Lecture 5: The H-R diagram, standard candles and cosmic distances
... temperature and radius are related by: L=4πR2 σT4 • Hence stars of a fixed size would populate a line from top left to bottom right - the main sequence is almost such a line • However, it is steeper - hotter stars on the MS are also larger • The two populated regions above the MS are much larger ...
... temperature and radius are related by: L=4πR2 σT4 • Hence stars of a fixed size would populate a line from top left to bottom right - the main sequence is almost such a line • However, it is steeper - hotter stars on the MS are also larger • The two populated regions above the MS are much larger ...
Jupiter-Sized Star Smallest Ever Detected
... spectroscopic orbit provides a unique value of the mass of the companion, once the mass of the Until recently, very few observations had been larger star is known. made and little was known about low-mass stars. At this moment, exact values of the radii are known The astronomers find that OGLE-TR-12 ...
... spectroscopic orbit provides a unique value of the mass of the companion, once the mass of the Until recently, very few observations had been larger star is known. made and little was known about low-mass stars. At this moment, exact values of the radii are known The astronomers find that OGLE-TR-12 ...
Astro twopages
... or 300,000 km away and the pause is the travel time of the radio waves. The Sun is 8 light minutes away. If the Sun suddenly stopped producing energy, it will still take 8 minutes for the Earth to know it. Incidentally the sun is about 1 light second in radius as well. Pluto is the edge of the plane ...
... or 300,000 km away and the pause is the travel time of the radio waves. The Sun is 8 light minutes away. If the Sun suddenly stopped producing energy, it will still take 8 minutes for the Earth to know it. Incidentally the sun is about 1 light second in radius as well. Pluto is the edge of the plane ...
Seyfert Galaxies - Otterbein University
... • A relation between the rotation speed of a spiral galaxy and its luminosity • The more mass a galaxy has the brighter it is the faster it rotates the wider the spectral lines are • Measuring rotation speed allows us to estimate luminosity; comparing to observed (apparent) brightness then tell ...
... • A relation between the rotation speed of a spiral galaxy and its luminosity • The more mass a galaxy has the brighter it is the faster it rotates the wider the spectral lines are • Measuring rotation speed allows us to estimate luminosity; comparing to observed (apparent) brightness then tell ...
Observational Data
... RGB star radial density profile • 1) crowded central part: a = 0’.0 – 2’.0, completeness from 80 to 90 % at I = 23m; • 2) old exponential disk extending well beyond the previously estimated size of the galaxy: a = 2’.0 – 5’.5, S-L 1’.03 ± 0’.03; • 3) discovered old “halo”: a = 5’.5 – 7’.5, S-L 1’.8 ...
... RGB star radial density profile • 1) crowded central part: a = 0’.0 – 2’.0, completeness from 80 to 90 % at I = 23m; • 2) old exponential disk extending well beyond the previously estimated size of the galaxy: a = 2’.0 – 5’.5, S-L 1’.03 ± 0’.03; • 3) discovered old “halo”: a = 5’.5 – 7’.5, S-L 1’.8 ...
Highlights of the Month - Bridgend Astronomical Society
... skies, see a region which is darker than the surroundings. This is called the Cygnus Rift and is caused by the obscuration of light from distant stars by a lane of dust in our local spiral arm. the dust comes from elements such as carbon which have been built up in stars and ejected into space in ex ...
... skies, see a region which is darker than the surroundings. This is called the Cygnus Rift and is caused by the obscuration of light from distant stars by a lane of dust in our local spiral arm. the dust comes from elements such as carbon which have been built up in stars and ejected into space in ex ...
A stars
... the nature of the star The situation becomes even more extreme in the case of a red dwarf, such as Barnard's Star (M4: about 2,000 times less luminous than the Sun), the HZ of which would extend only between about 750,000 and 2 million km (0.02 to 0.06 AU). However: if planets exist too close to its ...
... the nature of the star The situation becomes even more extreme in the case of a red dwarf, such as Barnard's Star (M4: about 2,000 times less luminous than the Sun), the HZ of which would extend only between about 750,000 and 2 million km (0.02 to 0.06 AU). However: if planets exist too close to its ...
Astronomy_Stars_n_Galaxies_PowerPoint
... • Astronomers theorize that the universe formed in an instant in an enormous explosion. This theory is called the Big Bang Theory. Before the explosion, astronomers believe that the universe we see now was no larger than a dot. Since the big bang, the size of the universe has ...
... • Astronomers theorize that the universe formed in an instant in an enormous explosion. This theory is called the Big Bang Theory. Before the explosion, astronomers believe that the universe we see now was no larger than a dot. Since the big bang, the size of the universe has ...
Lecture 16
... A later scheme, called the B-V Index, classed stars according to a logarithmic ratio of the peak amount of radiation in the blue and violet colors. The current scheme is to class stars according to color in a way which is more or less logarithmically proportional to temperature. In this scheme stars ...
... A later scheme, called the B-V Index, classed stars according to a logarithmic ratio of the peak amount of radiation in the blue and violet colors. The current scheme is to class stars according to color in a way which is more or less logarithmically proportional to temperature. In this scheme stars ...
Hertzsprung-Russell Diagram
... A star has a high luminosity (100 solar luminosities) and a surface temperature of 3500 K. What type of star is it? ...
... A star has a high luminosity (100 solar luminosities) and a surface temperature of 3500 K. What type of star is it? ...
Physica 133-11f: Sample Final Exam Here are sample questions for
... A) Before that time, the gas in the universe was dense and ionized and thus did not allow light to travel freely. B) 380,000 years after the Big Bang marks the time when stars were first born, and thus began to shine the light by which we can see the universe. C) Before that time, the universe was d ...
... A) Before that time, the gas in the universe was dense and ionized and thus did not allow light to travel freely. B) 380,000 years after the Big Bang marks the time when stars were first born, and thus began to shine the light by which we can see the universe. C) Before that time, the universe was d ...
M. Meixner
... resolving power to analyze the mass-loss return from stars to galaxies in the Local Volume of galaxies. For example, color magnitude diagrams from photometric imaging with NIRCam and MIRI can be used to identify dusty evolved stars which can then be compared to precomputed models such as GRAMS to de ...
... resolving power to analyze the mass-loss return from stars to galaxies in the Local Volume of galaxies. For example, color magnitude diagrams from photometric imaging with NIRCam and MIRI can be used to identify dusty evolved stars which can then be compared to precomputed models such as GRAMS to de ...
Stars
... Kepler’s 3rd law) imply a mass of 2.6106 solar masses inside a volume 0.03 light years in diameter. It is impossible to pack stars together that tightly – they would collide, destroying each other very quickly. It is likely that the object at the center of our galaxy is a super massive black hole. ...
... Kepler’s 3rd law) imply a mass of 2.6106 solar masses inside a volume 0.03 light years in diameter. It is impossible to pack stars together that tightly – they would collide, destroying each other very quickly. It is likely that the object at the center of our galaxy is a super massive black hole. ...
Stages - A Summary - University of Dayton
... the exact value is not known) are producing sufficient energy by just using the proton-proton chain of nuclear reactions, higher-mass stars must primarily rely on the carbon cycle to produce their greater requirements of energy to balance their greater gravity. The carbon atoms help the hydrogen ato ...
... the exact value is not known) are producing sufficient energy by just using the proton-proton chain of nuclear reactions, higher-mass stars must primarily rely on the carbon cycle to produce their greater requirements of energy to balance their greater gravity. The carbon atoms help the hydrogen ato ...
File
... The diagram below and to the right shows a galactic star at the bottom left with its spectrum on the bottom right. • Notice the dark absorption lines in the spectrum. • The other three spectra show the spectrum of a nearby galaxy, a medium distance galaxy, and a distant galaxy. Notice how the patte ...
... The diagram below and to the right shows a galactic star at the bottom left with its spectrum on the bottom right. • Notice the dark absorption lines in the spectrum. • The other three spectra show the spectrum of a nearby galaxy, a medium distance galaxy, and a distant galaxy. Notice how the patte ...
Astronomy 162 Lab 4: Stars
... Magnitude on the y-axis. From this diagram, astronomers can study the relationship between temperature and brightness. This relationship leads to some important observations. Firstly, the diagram is divided into three groups: Giants and Super Giants at the top, a long line of Main Sequence stars in ...
... Magnitude on the y-axis. From this diagram, astronomers can study the relationship between temperature and brightness. This relationship leads to some important observations. Firstly, the diagram is divided into three groups: Giants and Super Giants at the top, a long line of Main Sequence stars in ...
Nights of the Heavenly G With
... companion? This is something that few observers can check off on their life lists, but even if you're unable to make the claim to having seen it, even in twilight (hint!), think about the fact that the light from this star has been zooming though space for less than 9 years. Even a fourth grader can ...
... companion? This is something that few observers can check off on their life lists, but even if you're unable to make the claim to having seen it, even in twilight (hint!), think about the fact that the light from this star has been zooming though space for less than 9 years. Even a fourth grader can ...
THE LIFE CYCLE OF STARS
... forces, causing a massive, bright, short-lived explosion called a supernova. During the explosion, shock waves, blow away the star's outer layers. Supernova N132D: 3,000 years after a supernova, ejecting stellar material If the star's remaining mass is between 1 1/2 to 3 times the mass of the Sun, i ...
... forces, causing a massive, bright, short-lived explosion called a supernova. During the explosion, shock waves, blow away the star's outer layers. Supernova N132D: 3,000 years after a supernova, ejecting stellar material If the star's remaining mass is between 1 1/2 to 3 times the mass of the Sun, i ...
AN INTRODUCTION TO ASTRONOMY Dr. Uri Griv Department of Physics, Ben-Gurion University
... → dα = 4.1 × 1018 cm = ...
... → dα = 4.1 × 1018 cm = ...
Quasars - Ann Arbor Earth Science
... lines. Variability shows that the energy must arise in a tiny region, although some quasars have hundreds of time the energy output of normal galaxies. Their radio structures often include jets and lobes similar to what we see from radio galaxies. ...
... lines. Variability shows that the energy must arise in a tiny region, although some quasars have hundreds of time the energy output of normal galaxies. Their radio structures often include jets and lobes similar to what we see from radio galaxies. ...
AY5 Announcements
... of the Sun (as bright as a small galaxy) • Many rare elements will be manufactured in non-equilibrium reactions* ...
... of the Sun (as bright as a small galaxy) • Many rare elements will be manufactured in non-equilibrium reactions* ...
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.