What makes stars tick?
... us to see it glowing from hundreds of light-years away. What could hold such a massive object together? And how does the pent-up energy not blow it apart? Over the past century, astronomers have learned an immense amount about stars. They’ve pieced together the life cycles of different stars to lear ...
... us to see it glowing from hundreds of light-years away. What could hold such a massive object together? And how does the pent-up energy not blow it apart? Over the past century, astronomers have learned an immense amount about stars. They’ve pieced together the life cycles of different stars to lear ...
The Milky Way Galaxy
... Center of Milky Way Galaxy Apparently, there is an enormous black hole at the center of the galaxy, which is the source of these phenomena An accretion disk surrounding the black hole emits enormous amounts of radiation Observations on three stars that are orbiting the core region at a distance ran ...
... Center of Milky Way Galaxy Apparently, there is an enormous black hole at the center of the galaxy, which is the source of these phenomena An accretion disk surrounding the black hole emits enormous amounts of radiation Observations on three stars that are orbiting the core region at a distance ran ...
imaging spectroscopy of the centers of nearby agn
... It therefore seems likely that nuclear starbursts are episodic in nature. Given that the star formation occurs on scales of < 50 pc, it is inevitable that it and the AGN will have some mutual influence on each other. Our data hint at a possible relationship between the characteristic age of the star ...
... It therefore seems likely that nuclear starbursts are episodic in nature. Given that the star formation occurs on scales of < 50 pc, it is inevitable that it and the AGN will have some mutual influence on each other. Our data hint at a possible relationship between the characteristic age of the star ...
LESSON 8: STARS
... eight minutes to reach the Earth, about 4.3 years from the nearest star, and hundreds of years from the most distant visible stars. Stars are extremely bright and massive objects, but they are so incredibly distant that they appear as mere points of light in our sky. ...
... eight minutes to reach the Earth, about 4.3 years from the nearest star, and hundreds of years from the most distant visible stars. Stars are extremely bright and massive objects, but they are so incredibly distant that they appear as mere points of light in our sky. ...
2013. CCAT. All Rights Reserved.
... spectral surveys of galaxies, measuring the bright atomic fine-structure and molecular rotational transitions which cool the interstellar gas. Detected lines will provide redshifts for and interstellar gas conditions in tens of thousands of galaxies ranging from the early universe (z > 6) to the pre ...
... spectral surveys of galaxies, measuring the bright atomic fine-structure and molecular rotational transitions which cool the interstellar gas. Detected lines will provide redshifts for and interstellar gas conditions in tens of thousands of galaxies ranging from the early universe (z > 6) to the pre ...
The Hertzsprung-Russell Diagramm
... Stars of the same spectral class can have different luminosities. A further system, the M organKeenan (M -K) system, was introduced to make the distinction between the different luminosity classes (1943; Atlas of Stellar Spectra by W.W. M organ and P. C. Keenan). These luminosity classes range from ...
... Stars of the same spectral class can have different luminosities. A further system, the M organKeenan (M -K) system, was introduced to make the distinction between the different luminosity classes (1943; Atlas of Stellar Spectra by W.W. M organ and P. C. Keenan). These luminosity classes range from ...
Star Information ppt.
... • How hot are stars? • The surface temperatures of the hottest stars exceed 40,000 K and those of the coolest stars are less than 3,000 K. We measure a star’s surface temperature from its color or spectrum, and we classify spectra according to the sequence of spectral types OBAFGKM, which runs from ...
... • How hot are stars? • The surface temperatures of the hottest stars exceed 40,000 K and those of the coolest stars are less than 3,000 K. We measure a star’s surface temperature from its color or spectrum, and we classify spectra according to the sequence of spectral types OBAFGKM, which runs from ...
The Milky Way`s Restless Swarms of Stars
... Our galaxy’s gluttony actually adds a few clusters here and there. When dwarf galaxies spiral into our own, gravitational tides shred them as well. This is happening now to a loose agglomeration of stars called the Sagittarius dwarf (Science, 7 January 2000, p. 62); indeed, Majewski’s group sees tid ...
... Our galaxy’s gluttony actually adds a few clusters here and there. When dwarf galaxies spiral into our own, gravitational tides shred them as well. This is happening now to a loose agglomeration of stars called the Sagittarius dwarf (Science, 7 January 2000, p. 62); indeed, Majewski’s group sees tid ...
Crash Galaxies
... own merry way after the accident, bruised and beaten, but otherwise intact. The footballer and dancer metaphors break down, as they (believe it or not) never pass right through each other. When the velocities and sizes of two galaxies are such that they coast to a halt and fall together, staying hap ...
... own merry way after the accident, bruised and beaten, but otherwise intact. The footballer and dancer metaphors break down, as they (believe it or not) never pass right through each other. When the velocities and sizes of two galaxies are such that they coast to a halt and fall together, staying hap ...
Solar-like oscillations in intermediate red giants
... modelling theories and for understanding the structure and interior processes within the sun. It was able to rule out the possibility that the solar neutrino problem was due to incorrect models. ...
... modelling theories and for understanding the structure and interior processes within the sun. It was able to rule out the possibility that the solar neutrino problem was due to incorrect models. ...
Astronomy 252: Short Project 2 Stellar Spectra: Their Classification
... 2. To determine fundamental stellar properties using spectral information. Background: From the lectures you already know that stars come in a wide range of sizes and temperatures. The hottest stars in the sky have temperatures in excess of 40,000 K, whereas the coolest stars that we can detect opti ...
... 2. To determine fundamental stellar properties using spectral information. Background: From the lectures you already know that stars come in a wide range of sizes and temperatures. The hottest stars in the sky have temperatures in excess of 40,000 K, whereas the coolest stars that we can detect opti ...
Measuring Stars` Properties - Test 1 Study Guide
... • For a few close, big stars, they can be seen in a telescope as non-point objects • Measure angular size; if know distance then get size of star Example: Betelgeuse 300 times larger radius than the Sun • If further away but a binary star, get size of stars when they eclipse each other ! length o ...
... • For a few close, big stars, they can be seen in a telescope as non-point objects • Measure angular size; if know distance then get size of star Example: Betelgeuse 300 times larger radius than the Sun • If further away but a binary star, get size of stars when they eclipse each other ! length o ...
The Properties of Stars Early in its history, the universe organized
... astronomers Ejnar Hertzsprung and Henry N. Russell to plot the luminosities of stars on a vertical axis with their surface temperatures on a horizontal axis. In their honor, such plots are now known as Hertzsprung-Russell diagrams. Because of the StefanBoltzmann law, these diagrams also contain info ...
... astronomers Ejnar Hertzsprung and Henry N. Russell to plot the luminosities of stars on a vertical axis with their surface temperatures on a horizontal axis. In their honor, such plots are now known as Hertzsprung-Russell diagrams. Because of the StefanBoltzmann law, these diagrams also contain info ...
Neutron Stars
... Novae: white dwarf re-ignition in binary system • Nova is a faint star suddenly brightens by a factor of 104 to 108 over a few days or hours • It reaches a peak luminosity of about 105 Lsun • A nova is different from supernova (luminosity of 109 Lsun) • Material from an ordinary star in a close bin ...
... Novae: white dwarf re-ignition in binary system • Nova is a faint star suddenly brightens by a factor of 104 to 108 over a few days or hours • It reaches a peak luminosity of about 105 Lsun • A nova is different from supernova (luminosity of 109 Lsun) • Material from an ordinary star in a close bin ...
Ramin A. Skibba - Southern California Center for Galaxy Evolution
... significant fraction of halos, the BHG is not the central galaxy. This fraction is large and increases from ≈25% in low-mass halos to ≈40% in massive halos. We argue that the large fraction of halos with satellite BHGs is due to recently accreted relatively massive satellite galaxies that have not m ...
... significant fraction of halos, the BHG is not the central galaxy. This fraction is large and increases from ≈25% in low-mass halos to ≈40% in massive halos. We argue that the large fraction of halos with satellite BHGs is due to recently accreted relatively massive satellite galaxies that have not m ...
Chapter 7 Formation of Stars
... stars near the Orion Nebula. In the top image, the star responsible for the jets is hidden in the dark dust cloud lying in the center of the image. The entire width of this image is about one light year. The Herbig–Haro objects are designated HH-1 and HH-2, and correspond to the nebulosity at the en ...
... stars near the Orion Nebula. In the top image, the star responsible for the jets is hidden in the dark dust cloud lying in the center of the image. The entire width of this image is about one light year. The Herbig–Haro objects are designated HH-1 and HH-2, and correspond to the nebulosity at the en ...
Exam #2 Solutions
... The cooler giant stars are mostly K and M giants with temperatures around 5,000 K to 3,000K and luminosities between 50 and 5,000 solar luminosities. The stars are all larger in radius than the Sun, being between 1 and 100 solar radii. All these stars will have very short lifetimes compared to ...
... The cooler giant stars are mostly K and M giants with temperatures around 5,000 K to 3,000K and luminosities between 50 and 5,000 solar luminosities. The stars are all larger in radius than the Sun, being between 1 and 100 solar radii. All these stars will have very short lifetimes compared to ...
Chemical Composition of Planetary Nebulae: The Galaxy and the
... the SMC extends to even lower metallicities, namely (O) 7.0. Taking into account the Galactic and MC nebulae by Stasińska et al. [18], these results are confirmed and extended, especially at lower metallicities, (O) < 8.0, for which their sample is richer than ours. Correlations Involving N An a ...
... the SMC extends to even lower metallicities, namely (O) 7.0. Taking into account the Galactic and MC nebulae by Stasińska et al. [18], these results are confirmed and extended, especially at lower metallicities, (O) < 8.0, for which their sample is richer than ours. Correlations Involving N An a ...
Celebrating the centennial of a celestial yardstick
... assume that it has smatterings of other heavy metals, including gold, silver, and platinum. The planet has also had abundant volcanic activity (and may have some ongoing activity today), which is involved in concentrating such elements. Yet the amounts of these elements, their distribution, and many ...
... assume that it has smatterings of other heavy metals, including gold, silver, and platinum. The planet has also had abundant volcanic activity (and may have some ongoing activity today), which is involved in concentrating such elements. Yet the amounts of these elements, their distribution, and many ...
The Life Cycle of A Star
... which are some 5 or more times as massive as our Sun. After the outer layers of the star have swollen into a red supergiant (i.e., a very big red giant), the core begins to yield to gravity and starts to shrink. As it shrinks, it grows hotter and denser, and a new series of nuclear reactions begin t ...
... which are some 5 or more times as massive as our Sun. After the outer layers of the star have swollen into a red supergiant (i.e., a very big red giant), the core begins to yield to gravity and starts to shrink. As it shrinks, it grows hotter and denser, and a new series of nuclear reactions begin t ...
Chapter 8 Formation of Stars
... stars near the Orion Nebula. In the top image, the star responsible for the jets is hidden in the dark dust cloud lying in the center of the image. The entire width of this image is about one light year. The Herbig–Haro objects are designated HH-1 and HH-2, and correspond to the nebulosity at the en ...
... stars near the Orion Nebula. In the top image, the star responsible for the jets is hidden in the dark dust cloud lying in the center of the image. The entire width of this image is about one light year. The Herbig–Haro objects are designated HH-1 and HH-2, and correspond to the nebulosity at the en ...
pg. 271 - Cornell University
... on the lack of evidence of freshly synthesized carbon, concluded that the third dredge-up did not occur. For the first time, complete mid-infrared spectra (from 5.3 to 40 m) for this nebula are available. The infrared region of the spectrum is very useful for several reasons. The lines seen in the ...
... on the lack of evidence of freshly synthesized carbon, concluded that the third dredge-up did not occur. For the first time, complete mid-infrared spectra (from 5.3 to 40 m) for this nebula are available. The infrared region of the spectrum is very useful for several reasons. The lines seen in the ...
Contents ISP 205 Section 2 Study Guide for Test 3 28 March 2007
... o Giants burn hydrogen in a shell, helium, or other elements White dwarfs are earth-sized, dead stars. Main sequence is a mass sequence o O stars are massive o M stars have least mass Hot massive stars live a short life and cool stars live a long time o Lifetime=mass/luminosity o Comparison: If sun ...
... o Giants burn hydrogen in a shell, helium, or other elements White dwarfs are earth-sized, dead stars. Main sequence is a mass sequence o O stars are massive o M stars have least mass Hot massive stars live a short life and cool stars live a long time o Lifetime=mass/luminosity o Comparison: If sun ...
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.