![Notes 4, p. 1-3](http://s1.studyres.com/store/data/002897003_1-317440a10175c03a1e98153ce72b587e-300x300.png)
Notes 4, p. 1-3
... How does that energy get out? It is transported, and that transport has great bearing on the structure of the star • Early on, you learned there were three energy trnasport mechanisms: conduction, convection and radiation. We will state without proof that conduction is generally not important in sta ...
... How does that energy get out? It is transported, and that transport has great bearing on the structure of the star • Early on, you learned there were three energy trnasport mechanisms: conduction, convection and radiation. We will state without proof that conduction is generally not important in sta ...
Hot Stars With Cool Companions
... The multiplicity of A- and B-type stars can also help constrain the binary star formation mechanism and the relevant physics involved during and after the formation of the secondary. The dominant mode of binary star formation is thought to be molecular core fragmentation (Boss & Bodenheimer 1979; Bo ...
... The multiplicity of A- and B-type stars can also help constrain the binary star formation mechanism and the relevant physics involved during and after the formation of the secondary. The dominant mode of binary star formation is thought to be molecular core fragmentation (Boss & Bodenheimer 1979; Bo ...
Chapter 20 Review of Stars` Lifetime Review
... main sequence, they tend to move horizontally along the giants branch instead of vertically • They “burn” successively heavier elements ...
... main sequence, they tend to move horizontally along the giants branch instead of vertically • They “burn” successively heavier elements ...
Stellar Evolution
... • The description of stars’ birth and death can be tested by looking at star clusters, whose stars are all the same age but have different masses. • Stars in binary systems can evolve quite differently due to interactions with each other. ...
... • The description of stars’ birth and death can be tested by looking at star clusters, whose stars are all the same age but have different masses. • Stars in binary systems can evolve quite differently due to interactions with each other. ...
bringing pulsating stars into the physics classroom
... exposed to any aspect of theoretical astrophysics. This is doubly unfortunate because students then miss the opportunity to integrate their knowledge of several disciplines and apply it to interesting astrophysical phenomena. Students find pulsating stars inherently interesting, even more so when th ...
... exposed to any aspect of theoretical astrophysics. This is doubly unfortunate because students then miss the opportunity to integrate their knowledge of several disciplines and apply it to interesting astrophysical phenomena. Students find pulsating stars inherently interesting, even more so when th ...
Lec10_2D
... stellar remnant. In the remnant, the electrons of atoms are crushed into their nucleus. The star becomes one gigantic atomic nucleus made up only of neutrons – a neutron star. ...
... stellar remnant. In the remnant, the electrons of atoms are crushed into their nucleus. The star becomes one gigantic atomic nucleus made up only of neutrons – a neutron star. ...
No Slide Title
... If its companion is a main sequence or Red giant star then it can gain mass from its companion. Clump of mass has some small angular velocity. Law of conservation of angular momentummeans it moves faster and faster as it falls in. The infalling matter forms an accretion disc – a whirlpool like di ...
... If its companion is a main sequence or Red giant star then it can gain mass from its companion. Clump of mass has some small angular velocity. Law of conservation of angular momentummeans it moves faster and faster as it falls in. The infalling matter forms an accretion disc – a whirlpool like di ...
Relation Between the Luminosity of the Star at Different
... decrease in the luminosity and then an increase. This may be explained by the fact that in the Naked Helium stage, the star loses much of its outer surface to the stellar winds. The mass decreases as only the helium core is left behind. And since mass is directly proportional to the luminosity hence ...
... decrease in the luminosity and then an increase. This may be explained by the fact that in the Naked Helium stage, the star loses much of its outer surface to the stellar winds. The mass decreases as only the helium core is left behind. And since mass is directly proportional to the luminosity hence ...
Stellar Evolution 1
... Gets denser Converts gravitational PE -> KE Gets hotter • Conserves Angular Momentum Spins faster Flattens into a disk (rotation prevents contraction perpendicular to spin axis) ...
... Gets denser Converts gravitational PE -> KE Gets hotter • Conserves Angular Momentum Spins faster Flattens into a disk (rotation prevents contraction perpendicular to spin axis) ...
–1– 1. Polytropes – Derivation and Solutions of the Lane
... rigorous solutions of all the equations of stellar structure. But the price of this simplicity is assuming a power law relationship between pressure and density which must hold (including a fixed constant) throughout the star. We begin with the equations of mass continuity and of hydrostatic equilib ...
... rigorous solutions of all the equations of stellar structure. But the price of this simplicity is assuming a power law relationship between pressure and density which must hold (including a fixed constant) throughout the star. We begin with the equations of mass continuity and of hydrostatic equilib ...
PROBLEM SET #6 AST142 Due in class Tuesday Mar 17, 2015 First
... of stars in a mass bin dM equal to N (M ) where M is the stellar mass. A power law, N (M ) = AM −α with constant A and index α is an approximate description for the initial mass function. Recent work has used more complex functions to describe it and found that the initial mass function may vary wit ...
... of stars in a mass bin dM equal to N (M ) where M is the stellar mass. A power law, N (M ) = AM −α with constant A and index α is an approximate description for the initial mass function. Recent work has used more complex functions to describe it and found that the initial mass function may vary wit ...
Your Star: _____________________ d = 1 / p
... Winter Stars – The brightest and most spectacular stars in the sky belong to the winter. Betelgeuse, the ridiculously huge supergiant mentioned in lecture; Meissa, a rare superhot O star in Orion's belt; and dog star Sirius: the brightest of all stars are all winter stars. These stars are already vi ...
... Winter Stars – The brightest and most spectacular stars in the sky belong to the winter. Betelgeuse, the ridiculously huge supergiant mentioned in lecture; Meissa, a rare superhot O star in Orion's belt; and dog star Sirius: the brightest of all stars are all winter stars. These stars are already vi ...
VY Canis Majoris: The Astrophysical Basis of Its Luminosity
... photosphere or its surface directly. It has been known for some time that VY CMa’s absorption spectrum is significantly redshifted with respect to its systemic velocity (Humphreys 1975, Wallerstein 1977) due to scattering by dust (Herbig 1970, Kwok 1976, Van Blerkom & Van Blerkom 1978). Indeed, most ...
... photosphere or its surface directly. It has been known for some time that VY CMa’s absorption spectrum is significantly redshifted with respect to its systemic velocity (Humphreys 1975, Wallerstein 1977) due to scattering by dust (Herbig 1970, Kwok 1976, Van Blerkom & Van Blerkom 1978). Indeed, most ...
Life Cycle of stars
... fusion happens in the nebula's core. The nebula will start to glow brightly and become smaller due to the nebula starting to contract and shrink. Then after the nebula contracts the core of the nebula becomes docile and more stable. This phase changes the protostar into a main sequence star. Main se ...
... fusion happens in the nebula's core. The nebula will start to glow brightly and become smaller due to the nebula starting to contract and shrink. Then after the nebula contracts the core of the nebula becomes docile and more stable. This phase changes the protostar into a main sequence star. Main se ...
Astronomy Exam #2 for the 10
... 23) Star γ and star δ have equal radii and equal temperatures. Star δ is 33 ly distant from the Sun and has an apparent magnitude of -1. What is the apparent magnitude of star γ if it is 330 ly from the Sun? Since star δ has an apparent magnitude of -1 at a distance of 33 ly (i.e. about 1 pc), it mu ...
... 23) Star γ and star δ have equal radii and equal temperatures. Star δ is 33 ly distant from the Sun and has an apparent magnitude of -1. What is the apparent magnitude of star γ if it is 330 ly from the Sun? Since star δ has an apparent magnitude of -1 at a distance of 33 ly (i.e. about 1 pc), it mu ...
poll_questions
... The sequence ‘OBAFGKMLT’ for main sequence stars is ordered by decreasing ___________, whereas the letters are ordered alphabetically by ...
... The sequence ‘OBAFGKMLT’ for main sequence stars is ordered by decreasing ___________, whereas the letters are ordered alphabetically by ...
Star G has an apparent magnitude of +5.0 and an absolute
... with filters gives temperatures of stars is • Hotter stars lie further away from us • More luminous stars lie further away from us • If you compare any two stars, the colder one is ...
... with filters gives temperatures of stars is • Hotter stars lie further away from us • More luminous stars lie further away from us • If you compare any two stars, the colder one is ...
ASTR2050 Spring 2005 •
... from stars. We see that it is connected to temperature and we approximate it by “blackbody radiation”. However, there is also “discrete radiation” obvious in stellar spectra. These “spectral lines” give clues to the elements which make up the star. Historically, this is how astronomers came to class ...
... from stars. We see that it is connected to temperature and we approximate it by “blackbody radiation”. However, there is also “discrete radiation” obvious in stellar spectra. These “spectral lines” give clues to the elements which make up the star. Historically, this is how astronomers came to class ...
Stellar Temperatures
... There is a great variety of stellar absorption lines; the strength of any individual line is determined by the star’s • Temperature (most important) • Gravity • Abundance Historically, stellar spectral types have been classified using letters; the temperature sequence is (hot-to-cool) O-B-A-F-G-K ...
... There is a great variety of stellar absorption lines; the strength of any individual line is determined by the star’s • Temperature (most important) • Gravity • Abundance Historically, stellar spectral types have been classified using letters; the temperature sequence is (hot-to-cool) O-B-A-F-G-K ...
Gold could have come from colliding stars - Horizon Magazine
... The question, according to Dr Bauswein, is whether this picture can be confirmed by observations. Fortunately, the simulations predict that every merger should generate a characteristic ‘gravitational wave’ – a ripple in the very fabric of space–time. The observation of the right kind of gravitation ...
... The question, according to Dr Bauswein, is whether this picture can be confirmed by observations. Fortunately, the simulations predict that every merger should generate a characteristic ‘gravitational wave’ – a ripple in the very fabric of space–time. The observation of the right kind of gravitation ...
13.5 The HR Diagram By the early 1900s, astronomers had learned
... and 27% helium, with a trace of the heavier elements. Most have surface temperatures between about 3000 and 30,000 K and masses between about 0.1 and 30 M⊙. The HR diagram offers a simple, pictorial way to summarize stellar properties. Most stars lie along the main sequence, with hotter stars being ...
... and 27% helium, with a trace of the heavier elements. Most have surface temperatures between about 3000 and 30,000 K and masses between about 0.1 and 30 M⊙. The HR diagram offers a simple, pictorial way to summarize stellar properties. Most stars lie along the main sequence, with hotter stars being ...
10.2 Galaxies
... • If the nebula cloud is massive enough, gravity within the cloud will be large enough to shrink it and to raise its temperature above 10 000 000 degrees celsius, a temperature at which atomic fusion happens, releasing huge amounts of energy in the form of all kinds of electromagnetic radiation (gam ...
... • If the nebula cloud is massive enough, gravity within the cloud will be large enough to shrink it and to raise its temperature above 10 000 000 degrees celsius, a temperature at which atomic fusion happens, releasing huge amounts of energy in the form of all kinds of electromagnetic radiation (gam ...
Cooling of Compact Stars
... The Astrophysical Journal V 749 N1 Chris L. Fryer et al. 2012 ApJ 749 91 ...
... The Astrophysical Journal V 749 N1 Chris L. Fryer et al. 2012 ApJ 749 91 ...