Measuring the Properties of Stars (ch. 17)
... Theory tells us that the mass a star is born with determines nearly everything else about its fate. Good example: stellar lifetime = fuel supply/rate at which it is being burned ∝ stellar mass / stellar luminosity ∝ M / M3 ∝ 1/M2 So low mass stars live the longest. Numerically, we find a lifetime of ...
... Theory tells us that the mass a star is born with determines nearly everything else about its fate. Good example: stellar lifetime = fuel supply/rate at which it is being burned ∝ stellar mass / stellar luminosity ∝ M / M3 ∝ 1/M2 So low mass stars live the longest. Numerically, we find a lifetime of ...
Stars I - Astronomy Centre
... Binary Stars • About half of all stars occur in binary systems • Each star feels an equal force towards the other, but the lower mass star will experience a greater acceleration (Newton’s 2nd law) • If the two stars were initially at rest, they would meet at a point closer to the more massive star ...
... Binary Stars • About half of all stars occur in binary systems • Each star feels an equal force towards the other, but the lower mass star will experience a greater acceleration (Newton’s 2nd law) • If the two stars were initially at rest, they would meet at a point closer to the more massive star ...
space - Net Start Class
... wireless networking. Radio waves are used to explore space, such as with radio telescopes. Key Concept 3: Microwaves have shorter wavelengths and more energy than radio waves. Recently, scientists have discovered background microwave radiation left over from the early formation of the universe. This ...
... wireless networking. Radio waves are used to explore space, such as with radio telescopes. Key Concept 3: Microwaves have shorter wavelengths and more energy than radio waves. Recently, scientists have discovered background microwave radiation left over from the early formation of the universe. This ...
Leaving the Main Sequence
... Life of a Sun-like star (cont.) 3. Red giant – Core begins to run out of hydrogen fuel, begins to contract and heats. Remaining hydrogen burns faster in the shell around core and generates extra energy, disrupting hydrostatic equilibrium and causing outer regions to expand and cool. Star turns red. ...
... Life of a Sun-like star (cont.) 3. Red giant – Core begins to run out of hydrogen fuel, begins to contract and heats. Remaining hydrogen burns faster in the shell around core and generates extra energy, disrupting hydrostatic equilibrium and causing outer regions to expand and cool. Star turns red. ...
Astronomical Distance Ladder
... fairly simple using the standard candle approach. Both types of cepheid variable stars are pulsating stars whose period and luminosity are dependent on the mass of the star. Thus at specific periods every cepheid of one type has the same luminosity. The standard candles approach can be used for supe ...
... fairly simple using the standard candle approach. Both types of cepheid variable stars are pulsating stars whose period and luminosity are dependent on the mass of the star. Thus at specific periods every cepheid of one type has the same luminosity. The standard candles approach can be used for supe ...
Determining Distances to Other Galaxies
... differential rotation like the stars and gas, they would have wound up so tightly by now that they would not be visible. The stars and gas have made dozens of revolutions around the center of their galaxy over the age of the Universe so spiral structure should be “smeared out” if caused due to win ...
... differential rotation like the stars and gas, they would have wound up so tightly by now that they would not be visible. The stars and gas have made dozens of revolutions around the center of their galaxy over the age of the Universe so spiral structure should be “smeared out” if caused due to win ...
Lecture 10: Stellar Evolution
... observations • Star clusters are particularly useful because they contain stars of different mass that were born about the same ...
... observations • Star clusters are particularly useful because they contain stars of different mass that were born about the same ...
Spectral Classification
... absorption lines; particular absorption lines can be observed only for a certain range of temperatures because only in that range are the involved atomic energy levels populated. ...
... absorption lines; particular absorption lines can be observed only for a certain range of temperatures because only in that range are the involved atomic energy levels populated. ...
Pp 263-266 - Gravity From The Ground Up
... to somewhere between two and possibly three solar masses. Its actual value is not known: uncertainties in nuclear physics prevent reliable calculations. We have learned that neutron stars can only exist in a rather restricted range of masses, between perhaps 0.1 and two solar masses. In fact, their ...
... to somewhere between two and possibly three solar masses. Its actual value is not known: uncertainties in nuclear physics prevent reliable calculations. We have learned that neutron stars can only exist in a rather restricted range of masses, between perhaps 0.1 and two solar masses. In fact, their ...
Lecture 9
... Supported against gravity by e- degeneracy. Lots of residual heat, no energy source, a white dwarf is like a hot ember. As it radiates energy into space, the white dwarf cools off. There is an upper limit to the mass of a WD set by e-degeneracy. 1.4M☉ is the Chandrasekar Limit. ...
... Supported against gravity by e- degeneracy. Lots of residual heat, no energy source, a white dwarf is like a hot ember. As it radiates energy into space, the white dwarf cools off. There is an upper limit to the mass of a WD set by e-degeneracy. 1.4M☉ is the Chandrasekar Limit. ...
Slide 1
... shows the distribution of stellar masses. The more massive stars are much rarer than the least massive. ...
... shows the distribution of stellar masses. The more massive stars are much rarer than the least massive. ...
17_LectureOutline
... shows the distribution of stellar masses. The more massive stars are much rarer than the least massive. ...
... shows the distribution of stellar masses. The more massive stars are much rarer than the least massive. ...
Chapter 12 Stellar Evolution
... core contracts and heats; the outer atmosphere expands and cools. • Helium begins to fuse in the core, as a helium flash. The star expands into a red giant as the core continues to collapse. The envelope blows ...
... core contracts and heats; the outer atmosphere expands and cools. • Helium begins to fuse in the core, as a helium flash. The star expands into a red giant as the core continues to collapse. The envelope blows ...
A Study of the Spiral Galaxy M101 Elizabeth City State University
... show examples of each type. Galaxies have an enormous range in mass and size as indicated in Table 1. Galaxies are separated by vast gulfs of space. For example, our own Milky Way is over 160,000 light years away from its nearest extragalactic neighbor, the Large Magellanic Cloud. Despite these larg ...
... show examples of each type. Galaxies have an enormous range in mass and size as indicated in Table 1. Galaxies are separated by vast gulfs of space. For example, our own Milky Way is over 160,000 light years away from its nearest extragalactic neighbor, the Large Magellanic Cloud. Despite these larg ...
ppt
... The technology now has a large worldwide group of experts with experience/expertise in constructing and operating massive LS detectors (upto 1 kT so far), for precision low energy (>100 keV ) astro-particle physics Essential questions for a large scale project like this: • What science can be achiev ...
... The technology now has a large worldwide group of experts with experience/expertise in constructing and operating massive LS detectors (upto 1 kT so far), for precision low energy (>100 keV ) astro-particle physics Essential questions for a large scale project like this: • What science can be achiev ...
Evolved Stellar Populations
... kinematics of both the stars and gas. The best laboratories for these studies are galaxies of the Local Group and in particular the Magellanic Clouds (nearby, known distance, low extinction, …interacting irregular galaxies). Distinguish between cluster and field stars. A global picture of any ...
... kinematics of both the stars and gas. The best laboratories for these studies are galaxies of the Local Group and in particular the Magellanic Clouds (nearby, known distance, low extinction, …interacting irregular galaxies). Distinguish between cluster and field stars. A global picture of any ...
Basic Properties of Stars
... cool, but also very bright. Since cool objects don’t emit much light, these stars must be huge. They are red giants. Some stars are faint, but very hot. These must therefore be very small – they are white dwarf stars. ...
... cool, but also very bright. Since cool objects don’t emit much light, these stars must be huge. They are red giants. Some stars are faint, but very hot. These must therefore be very small – they are white dwarf stars. ...
Nucleosynthesis and the death of stars
... Hotter fusion and heavier elements • Could stars in principle live forever simply by contracting gravitationally and increasing their temperature to ignite the next heavier source of nuclear fuel whenever they run out? – No. The strong interaction’s range is smaller than the diameters of all but th ...
... Hotter fusion and heavier elements • Could stars in principle live forever simply by contracting gravitationally and increasing their temperature to ignite the next heavier source of nuclear fuel whenever they run out? – No. The strong interaction’s range is smaller than the diameters of all but th ...
Stars: Their Life and Afterlife
... • The main-sequence lifetime. • The interior structure and dynamics, in particular how heat is transferred within the star, whether by radiation or by convection. • The heaviest elements that can be synthesized by nuclear fusion in the core. • The final state of the star: white dwarf, neutron star, ...
... • The main-sequence lifetime. • The interior structure and dynamics, in particular how heat is transferred within the star, whether by radiation or by convection. • The heaviest elements that can be synthesized by nuclear fusion in the core. • The final state of the star: white dwarf, neutron star, ...
Star Cycle Balloons - Communicating Astronomy With The Public
... 1. Give each group a set of cards and the supplies necessary to complete the activity according to the directions printed on the cards. Have those students with the yellow “stars”(balloons) put a small styrofoam ball inside, those with a white “star” are to put a marble or bead inside, and those wit ...
... 1. Give each group a set of cards and the supplies necessary to complete the activity according to the directions printed on the cards. Have those students with the yellow “stars”(balloons) put a small styrofoam ball inside, those with a white “star” are to put a marble or bead inside, and those wit ...
Life Cycle of Stars Activity
... 1. Give each group a set of cards and the supplies necessary to complete the activity according to the directions printed on the cards. Have those students with the yellow “stars”(balloons) put a small styrofoam ball inside, those with a white “star” are to put a marble or bead inside, and those wit ...
... 1. Give each group a set of cards and the supplies necessary to complete the activity according to the directions printed on the cards. Have those students with the yellow “stars”(balloons) put a small styrofoam ball inside, those with a white “star” are to put a marble or bead inside, and those wit ...