Stars!!!!
... • If you can travel at the speed of light it would take about 8 minutes to get to the sun and 4.2 years to get to Proxima Centauri. ...
... • If you can travel at the speed of light it would take about 8 minutes to get to the sun and 4.2 years to get to Proxima Centauri. ...
Aging nearby spiral galaxies using H
... » Simulates evolution of single GMC » Input plausible parameters for nearby spirals » Outputs photometry & spectral data ...
... » Simulates evolution of single GMC » Input plausible parameters for nearby spirals » Outputs photometry & spectral data ...
Physics 306
... o HI clouds – clouds of neutral gas, 50-150 pc in diameter, few solar masses, 100K temp (low), 10- few hundred atom/cubic cm (high density) not ionized! *make up about 25% of interstellar mass o Intercloud medium – few thousand K, .1 atom/cubic cm (low density), IONIZED hydrogen (HII), in approx. e ...
... o HI clouds – clouds of neutral gas, 50-150 pc in diameter, few solar masses, 100K temp (low), 10- few hundred atom/cubic cm (high density) not ionized! *make up about 25% of interstellar mass o Intercloud medium – few thousand K, .1 atom/cubic cm (low density), IONIZED hydrogen (HII), in approx. e ...
Nineteenth lecture
... Soooooo, ultimately we wind up with the solar system we call HOME. (Ever wonder why all the planets except for Pluto rotate in the same direction around the sun, in a flat plane?) ...
... Soooooo, ultimately we wind up with the solar system we call HOME. (Ever wonder why all the planets except for Pluto rotate in the same direction around the sun, in a flat plane?) ...
Great Astronomers of the 20th Century
... • Prolific classifier of stars – Spectral Type and Temp. – Uniform database of stars ...
... • Prolific classifier of stars – Spectral Type and Temp. – Uniform database of stars ...
Hubble`s Law is the relation between the recession velocity of a
... star per unit time, or the luminosity, is equal to the energy generation rate at the core of the star. A white dwarf has used up its fuel for nuclear reaction. It generates no energy inside of it, and is cooling. Thus a hot white dwarf is not in thermal equilibrium. (A white dwarf may be hot, but th ...
... star per unit time, or the luminosity, is equal to the energy generation rate at the core of the star. A white dwarf has used up its fuel for nuclear reaction. It generates no energy inside of it, and is cooling. Thus a hot white dwarf is not in thermal equilibrium. (A white dwarf may be hot, but th ...
Astronomy – Interpreting Main Sequence Star Data The
... 2. How does the mass of stars relate to how long they live? 3.a) How would our sun be classified? b) How long is the life time of our sun? c) As our sun ages how will it change? 4. Which star type in the table would be considered a dwarf star? Explain your answer. 5. Which star type is most similar ...
... 2. How does the mass of stars relate to how long they live? 3.a) How would our sun be classified? b) How long is the life time of our sun? c) As our sun ages how will it change? 4. Which star type in the table would be considered a dwarf star? Explain your answer. 5. Which star type is most similar ...
Supernovae - Cloudfront.net
... the amount of energy created in a Type Ia Supernova is always about the same. Thus its luminosity is always the same. A Type Ia Supernova in another galaxy is thus a good standard candle to use to find the distance to the galaxy ...
... the amount of energy created in a Type Ia Supernova is always about the same. Thus its luminosity is always the same. A Type Ia Supernova in another galaxy is thus a good standard candle to use to find the distance to the galaxy ...
The Life of a Star
... life of a low-mass star and that of a star 10 times the Sun’s mass. Low-mass stars cool down and swell up into a red giant. Outer layers drift away and the star shrinks to become a white dwarf which will cool and fade away. High-mass stars swells into a red supergiant which undergoes a supernova. Th ...
... life of a low-mass star and that of a star 10 times the Sun’s mass. Low-mass stars cool down and swell up into a red giant. Outer layers drift away and the star shrinks to become a white dwarf which will cool and fade away. High-mass stars swells into a red supergiant which undergoes a supernova. Th ...
Review for Midterm 1
... What can the spectrum of a star tell us about the star? What else can we learn from spectra? What does the energy of a photon depend on? What is the sun mostly made of; how do we know? What are the different types of light? 3. Births of stars: How are stars born? When are they considered to be “born ...
... What can the spectrum of a star tell us about the star? What else can we learn from spectra? What does the energy of a photon depend on? What is the sun mostly made of; how do we know? What are the different types of light? 3. Births of stars: How are stars born? When are they considered to be “born ...
29 October: Dead Stars 3
... Many white dwarfs have been cataloged http://www.astronomy.villanova.edu/WDCatalog/index.html ...
... Many white dwarfs have been cataloged http://www.astronomy.villanova.edu/WDCatalog/index.html ...
Questions for this book (Word format)
... Copying directly from the book is illegal (plagiarism) and will be penalised. 1. When Eddington suggested in 1926 that stars were powered by hydrogen fusion, why did most physicists quite reasonably reject this suggestion? Explain the phenomenon, unknown in 1926, that allows hydrogen fusion to occur ...
... Copying directly from the book is illegal (plagiarism) and will be penalised. 1. When Eddington suggested in 1926 that stars were powered by hydrogen fusion, why did most physicists quite reasonably reject this suggestion? Explain the phenomenon, unknown in 1926, that allows hydrogen fusion to occur ...
Phys133-Sample MT2
... 10) Compared to the star it evolved from, a red giant is A) cooler and brighter. B) hotter and brighter. C) hotter and dimmer. D) the same temperature and brightness. E) cooler and dimmer. ...
... 10) Compared to the star it evolved from, a red giant is A) cooler and brighter. B) hotter and brighter. C) hotter and dimmer. D) the same temperature and brightness. E) cooler and dimmer. ...
Stars
... • As it expands, its opacity drops and we see to a deeper and deeper and hotter and hotter depth, so the star moves left on the HR diagram • Until… we see the electron degenerate core; the new white dwarf created at the center • This core can now cool, as it can’t collapse further and it is exposed ...
... • As it expands, its opacity drops and we see to a deeper and deeper and hotter and hotter depth, so the star moves left on the HR diagram • Until… we see the electron degenerate core; the new white dwarf created at the center • This core can now cool, as it can’t collapse further and it is exposed ...
1. Compute the deflection angle of a star whose light... limb of the Sun. Also compute the deflection angle of...
... 1. Compute the deflection angle of a star whose light just grazes the limb of the Sun. Also compute the deflection angle of a star whose light just grazes the limb of a 1.4M neutron star, if the neutron star was at the same distance from the Earth as the Sun. State assumptions. 2. Use the Plummer p ...
... 1. Compute the deflection angle of a star whose light just grazes the limb of the Sun. Also compute the deflection angle of a star whose light just grazes the limb of a 1.4M neutron star, if the neutron star was at the same distance from the Earth as the Sun. State assumptions. 2. Use the Plummer p ...
Lars Bildsten - nnpss
... Stars more massive than 6-8 times the Sun get to burn all the way up to the most stable nucleus, 56Fe, at least in their core. After that has happened, no further nuclear burning can halt the gravitational contraction… . . Leading to a catastrophic collapse to densities comparable to that of a nucle ...
... Stars more massive than 6-8 times the Sun get to burn all the way up to the most stable nucleus, 56Fe, at least in their core. After that has happened, no further nuclear burning can halt the gravitational contraction… . . Leading to a catastrophic collapse to densities comparable to that of a nucle ...
Chapter 16 Star Birth Where do stars form? Star
... for infrared and radio photons to escape • Thermal energy then begins to build up inside, increasing the internal pressure ...
... for infrared and radio photons to escape • Thermal energy then begins to build up inside, increasing the internal pressure ...
Chapter 16 Star Birth
... for infrared and radio photons to escape • Thermal energy then begins to build up inside, increasing the internal pressure • Contraction slows down, and the center of the cloud fragment becomes a protostar ...
... for infrared and radio photons to escape • Thermal energy then begins to build up inside, increasing the internal pressure • Contraction slows down, and the center of the cloud fragment becomes a protostar ...
Formation and Evolution of Infalling Disks Around Protostars
... The shell should be self-gravitating before blow out. Expansion velocity should be larger than the sound speed. ...
... The shell should be self-gravitating before blow out. Expansion velocity should be larger than the sound speed. ...
Stars
... • Begin their lives as giant clouds of dust and gas called nebulae • Gravity may cause the nebula to contract • Matter in the gas cloud will begin to condense into a dense region called a protostar • The protostar continues to condense, it heats up. Eventually, it reaches a critical mass and nuclear ...
... • Begin their lives as giant clouds of dust and gas called nebulae • Gravity may cause the nebula to contract • Matter in the gas cloud will begin to condense into a dense region called a protostar • The protostar continues to condense, it heats up. Eventually, it reaches a critical mass and nuclear ...
Lecture Eight (Powerpoint format) - Flash
... brightness of a star. Two stars of the same intrinsic brightness at two different distances will have two different magnitudes. If one also knows the distance to the star (not always the case!), then one can correct for the distance and obtain an intrinsic magnitude. By convention this is chosen t ...
... brightness of a star. Two stars of the same intrinsic brightness at two different distances will have two different magnitudes. If one also knows the distance to the star (not always the case!), then one can correct for the distance and obtain an intrinsic magnitude. By convention this is chosen t ...
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.