Physical Attributes of Stars
... • Super giants: Older and larger • Virtually non-existent: Used to be other stars but are slowly burning out ...
... • Super giants: Older and larger • Virtually non-existent: Used to be other stars but are slowly burning out ...
The Relationship Between a Star`s Color, Temperature, and
... • Kirchoff realized that any object that would be a perfect absorber of light would also be a perfect emitter…but the amount of light energy it would give off each second (its brightness or luminosity) and the color of the light would be related to the object’s temperature. ...
... • Kirchoff realized that any object that would be a perfect absorber of light would also be a perfect emitter…but the amount of light energy it would give off each second (its brightness or luminosity) and the color of the light would be related to the object’s temperature. ...
Where do we come from?
... years The growth of black holes. Clusters of gargantuan black holes (1011 solar masses) in place of clusters of galaxies. Moving black holes radiate gravitational waves (ripples in space-time). ...
... years The growth of black holes. Clusters of gargantuan black holes (1011 solar masses) in place of clusters of galaxies. Moving black holes radiate gravitational waves (ripples in space-time). ...
9binary1i
... Medium-bright yellow stars have solar masses (M ~ 0.8-2 Msun) Hot, bright stars have high mass (M ~ 2-40 Msun) ...
... Medium-bright yellow stars have solar masses (M ~ 0.8-2 Msun) Hot, bright stars have high mass (M ~ 2-40 Msun) ...
Astro 3 Spring, 2004 (Prof
... The Helium Flash occurs when the inert helium core of a red giant star suddenly detonates and helium begins fusing into carbon and oxygen. This occurs in stars with less than 2-3 solar masses. In stars with masses above 2-3 solar masses, helium burning occurs more gradually. Degenerate matter is mat ...
... The Helium Flash occurs when the inert helium core of a red giant star suddenly detonates and helium begins fusing into carbon and oxygen. This occurs in stars with less than 2-3 solar masses. In stars with masses above 2-3 solar masses, helium burning occurs more gradually. Degenerate matter is mat ...
Astronomy 115 Homework Set #1 – Due: Thursday, Feb
... 2. How many hydrogen atoms are converted to helium each second in order to power the Sun’s luminosity? To arrive at the solution, answer the following: (a) What is the mass of 4 hydrogen atoms? (b) What is the mass of 1 helium atom? (c) How much more mass is there in the 4 hydrogen atoms than in the ...
... 2. How many hydrogen atoms are converted to helium each second in order to power the Sun’s luminosity? To arrive at the solution, answer the following: (a) What is the mass of 4 hydrogen atoms? (b) What is the mass of 1 helium atom? (c) How much more mass is there in the 4 hydrogen atoms than in the ...
PDF version (two pages, including the full text)
... brighter one is about half again as bright as our sun, the fainter about half as bright as the sun. Separated by about 23 times the distance from the Earth to the sun, they take 80 years to orbit each other. For many years it was believed that these were the two nearest stars to our own sun. But a t ...
... brighter one is about half again as bright as our sun, the fainter about half as bright as the sun. Separated by about 23 times the distance from the Earth to the sun, they take 80 years to orbit each other. For many years it was believed that these were the two nearest stars to our own sun. But a t ...
Slide 1
... End of H He burning in the core of MS star Red Giant phase with inert He-core and outer H-burning shell; star expands and cools, but is brighter Climbs up the RG branch until He-flash in the core Core expands and cools; H-burning decreases; outer layers contract; luminosity decreases but temperatu ...
... End of H He burning in the core of MS star Red Giant phase with inert He-core and outer H-burning shell; star expands and cools, but is brighter Climbs up the RG branch until He-flash in the core Core expands and cools; H-burning decreases; outer layers contract; luminosity decreases but temperatu ...
Astronomy 1
... The Milky Way Galaxy, commonly referred to as just the Milky Way, or sometimes simply as the Galaxy,[a] is the home galaxy of the Solar System, and of Earth. It is agreed that the Milky Way is a spiral galaxy, with observations suggesting that it is a barred spiral galaxy. It contains 100-400 billio ...
... The Milky Way Galaxy, commonly referred to as just the Milky Way, or sometimes simply as the Galaxy,[a] is the home galaxy of the Solar System, and of Earth. It is agreed that the Milky Way is a spiral galaxy, with observations suggesting that it is a barred spiral galaxy. It contains 100-400 billio ...
Document
... presence of the Urca shell the energy losses owing to neutrino emission and the entropy increase resulting from non-equilibrium beta reactions are much smaller than the rate of decrease of the energy of pulsations by the excitation of shortwavelength acoustic waves. The dissipation of the vibrationa ...
... presence of the Urca shell the energy losses owing to neutrino emission and the entropy increase resulting from non-equilibrium beta reactions are much smaller than the rate of decrease of the energy of pulsations by the excitation of shortwavelength acoustic waves. The dissipation of the vibrationa ...
Cosmic Collisions
... scattered in random directions, but gravity acts so gradually that planetary orbits are not disturbed. A collision takes about a billion years; during the last billion years, life on Earth evolved from single-celled organisms to amazingly primative apes who still think digital watches are pretty nea ...
... scattered in random directions, but gravity acts so gradually that planetary orbits are not disturbed. A collision takes about a billion years; during the last billion years, life on Earth evolved from single-celled organisms to amazingly primative apes who still think digital watches are pretty nea ...
Modelling the Stellar Populations of The Milky Way and Andromeda
... LCDM and stellar halos Hierarchical structure formation leads to idea that stellar halos formed from accreted, disrupted galaxies (~Searle & Zinn). Stellar halo studies provide means to: Measure accretion rates: Stellar streams around galaxies Probe early star formation: Chemical abundance patterns ...
... LCDM and stellar halos Hierarchical structure formation leads to idea that stellar halos formed from accreted, disrupted galaxies (~Searle & Zinn). Stellar halo studies provide means to: Measure accretion rates: Stellar streams around galaxies Probe early star formation: Chemical abundance patterns ...
CCR 22: Scattering of Starlight
... Starlight, like all other kinds of electromagnetic (EM) radiation, is absorbed and scattered by the gas molecules and dust in the interstellar medium (ISM). These processes depend on the atomic and molecular composition of the ISM. In addition, the second process depends on the size of the dust part ...
... Starlight, like all other kinds of electromagnetic (EM) radiation, is absorbed and scattered by the gas molecules and dust in the interstellar medium (ISM). These processes depend on the atomic and molecular composition of the ISM. In addition, the second process depends on the size of the dust part ...
14.5 Galactic Spiral Arms
... 14.6 The Mass of the Milky Way Galaxy Once all the galaxy is within an orbit, the velocity should diminish with distance, as the dashed curve shows. It doesn’t; more than twice the mass of the galaxy would have to be outside the visible part to reproduce the ...
... 14.6 The Mass of the Milky Way Galaxy Once all the galaxy is within an orbit, the velocity should diminish with distance, as the dashed curve shows. It doesn’t; more than twice the mass of the galaxy would have to be outside the visible part to reproduce the ...
Spectroscopic Investigation of Companion Stars in Herbig
... Herbig AeBe (HAEBE) binary systems are good environments for the study of pre-main sequence stellar evolution in companion stars whose mass may be significantly lower than that of the primary star. Measurements of the spectral type and surface gravity of the companion star in the system allow it to ...
... Herbig AeBe (HAEBE) binary systems are good environments for the study of pre-main sequence stellar evolution in companion stars whose mass may be significantly lower than that of the primary star. Measurements of the spectral type and surface gravity of the companion star in the system allow it to ...
Goal: To understand how Saturn formed and what its core is
... Evolution to Hot Jupiter • As the planet moves in it is closer to material that was previously too close. • It is also now larger and will eat that material as well. • This will produce a run away effect that only ends when the gas giant either gets very close to the star or the protostar turns int ...
... Evolution to Hot Jupiter • As the planet moves in it is closer to material that was previously too close. • It is also now larger and will eat that material as well. • This will produce a run away effect that only ends when the gas giant either gets very close to the star or the protostar turns int ...
The Electromagnetic Spectrum
... • Thin gases emit emission spectra. • When light passes through cool gas, colors are removed, forming an absorption spectrum. ...
... • Thin gases emit emission spectra. • When light passes through cool gas, colors are removed, forming an absorption spectrum. ...
ASTRONOMY 313
... hydrogen at 1215 Å (corresponding to a transition between the first and second energy levels of neutral hydrogen atoms) is observed in the optical spectrum of HS1946+7658 to be in emission at a wavelength of 4884.3 Å, in the blue-green region. a. ...
... hydrogen at 1215 Å (corresponding to a transition between the first and second energy levels of neutral hydrogen atoms) is observed in the optical spectrum of HS1946+7658 to be in emission at a wavelength of 4884.3 Å, in the blue-green region. a. ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.