What Does an Astronomer Do?
... actually be studying a star that no longer exists. Stars go through life cycles just like many living things. Stars are "born" in "nurseries" in nebulae. Huge clouds of dust and gas collapse under gravitational forces, forming protostars. These young stars undergo further collapse, forming main sequ ...
... actually be studying a star that no longer exists. Stars go through life cycles just like many living things. Stars are "born" in "nurseries" in nebulae. Huge clouds of dust and gas collapse under gravitational forces, forming protostars. These young stars undergo further collapse, forming main sequ ...
Combining Practices with Core Ideas in the NGSS
... distances from Earth?” You could just ask them! Their achievement of the performance expectation would be measured by the extent to which their responses showed they understood the three lines of evidence from the lesson: 1) A large, bright object can appear small and dim if it is far away. 2) It is ...
... distances from Earth?” You could just ask them! Their achievement of the performance expectation would be measured by the extent to which their responses showed they understood the three lines of evidence from the lesson: 1) A large, bright object can appear small and dim if it is far away. 2) It is ...
Unit 1
... • Dust particles do not absorb light the same way that gas atoms do, but using similar methods tells us that the dust is made of silicates ...
... • Dust particles do not absorb light the same way that gas atoms do, but using similar methods tells us that the dust is made of silicates ...
Star Life Cycle Web Activity
... From this point on you may click on the Yellow Right Arrow at the bottom of each page. Or Click on Equilibrium of a Star. Read the web page and the summary of a typical cycle of stars given here. Stars repeat a cycle of reaching equilibrium and then losing it after burning out one fuel source…then ...
... From this point on you may click on the Yellow Right Arrow at the bottom of each page. Or Click on Equilibrium of a Star. Read the web page and the summary of a typical cycle of stars given here. Stars repeat a cycle of reaching equilibrium and then losing it after burning out one fuel source…then ...
proper motion
... had determined the distances to roughly 200 stars. The Danish astronomer Hertzsprung and the American astronomer Russell noted that a majority of stars had absolute magnitudes that correlated with their spectral types. In a plot of MV vs. spectral type most stars traced out a band from the upper lef ...
... had determined the distances to roughly 200 stars. The Danish astronomer Hertzsprung and the American astronomer Russell noted that a majority of stars had absolute magnitudes that correlated with their spectral types. In a plot of MV vs. spectral type most stars traced out a band from the upper lef ...
PHY299B Poster-Justin Hudson-v2
... • If everything would have gone as planned, we would have produced a light curve as seen to the bottom picture. • What this light curve shows is that the deepest dips in brightness during the phase is when the brightest star is blocked by the other creating the eclipsing effect like when Earth exper ...
... • If everything would have gone as planned, we would have produced a light curve as seen to the bottom picture. • What this light curve shows is that the deepest dips in brightness during the phase is when the brightest star is blocked by the other creating the eclipsing effect like when Earth exper ...
Teacher`s Guide The Solar Empire: A Star is Born
... or printed sources, PowerPoint presentation, or some other format of the students’ own choosing. 7. After each team’s report, have team members lead a whole-class discussion on what could be inferred about earlier and later stages of the star’s development based on information about the star at the ...
... or printed sources, PowerPoint presentation, or some other format of the students’ own choosing. 7. After each team’s report, have team members lead a whole-class discussion on what could be inferred about earlier and later stages of the star’s development based on information about the star at the ...
The Brightness of Stars
... The surface area of a star is another factor in the brightness of a star Two stars of the same temperature will have different magnitudes, depending on their size A red supergiant can emit vastly more light than a red dwarf ...
... The surface area of a star is another factor in the brightness of a star Two stars of the same temperature will have different magnitudes, depending on their size A red supergiant can emit vastly more light than a red dwarf ...
HR Diagram
... This part uses tables 10.1, 10.2 and 10.3 of an earlier HR Diagram Lab. To find tables go to http://www.auburn.edu/academic/cosam/departments/physics/intro-courses/ugradlab/physics1150/index.htm. Go down page to #18 HR Diagram and look in background material. 1. Which type of star is most common? Ch ...
... This part uses tables 10.1, 10.2 and 10.3 of an earlier HR Diagram Lab. To find tables go to http://www.auburn.edu/academic/cosam/departments/physics/intro-courses/ugradlab/physics1150/index.htm. Go down page to #18 HR Diagram and look in background material. 1. Which type of star is most common? Ch ...
1117 Discussion Notes
... course… but let’s take another look at Newton’s version of Kepler’s third law, slightly rewritten. ...
... course… but let’s take another look at Newton’s version of Kepler’s third law, slightly rewritten. ...
Virtual HR Diagram Lab
... 8. Uncheck show luminosity classes and check show instability strip. Note that this region of the HR Diagram indicates where pulsating stars are found such as RR Lyrae stars and Cepheid variable stars. These stars vary in brightness because they are pulsating-alternately growing bigger and smaller- ...
... 8. Uncheck show luminosity classes and check show instability strip. Note that this region of the HR Diagram indicates where pulsating stars are found such as RR Lyrae stars and Cepheid variable stars. These stars vary in brightness because they are pulsating-alternately growing bigger and smaller- ...
Sections F and G
... These are almost certainly too massive to be neutron stars so are presumably black holes surrounded by accretion discs. In General Relativity, around any mass M there is an ‘event horizon’ from within which no matter or radiation can escape. This has the Schwarzschild radius Rs= (2GM)/c2 (In a simpl ...
... These are almost certainly too massive to be neutron stars so are presumably black holes surrounded by accretion discs. In General Relativity, around any mass M there is an ‘event horizon’ from within which no matter or radiation can escape. This has the Schwarzschild radius Rs= (2GM)/c2 (In a simpl ...
The Life and Times of a Neutron Star
... Exotic neutron stars may not be so rare. • Highly magnetized neutron stars may be as common as standard radio pulsars, but they don’t radio out their locations so they are harder to find. ...
... Exotic neutron stars may not be so rare. • Highly magnetized neutron stars may be as common as standard radio pulsars, but they don’t radio out their locations so they are harder to find. ...
17_LectureOutline
... must be measured. Once this is done, Kepler’s third law gives the sum of the masses of the two stars. Then the relative speeds of the two stars can be measured using the Doppler effect; the speed will be inversely proportional to the mass. This allows us to calculate the mass of each star. ...
... must be measured. Once this is done, Kepler’s third law gives the sum of the masses of the two stars. Then the relative speeds of the two stars can be measured using the Doppler effect; the speed will be inversely proportional to the mass. This allows us to calculate the mass of each star. ...
Slide 1
... must be measured. Once this is done, Kepler’s third law gives the sum of the masses of the two stars. Then the relative speeds of the two stars can be measured using the Doppler effect; the speed will be inversely proportional to the mass. This allows us to calculate the mass of each star. ...
... must be measured. Once this is done, Kepler’s third law gives the sum of the masses of the two stars. Then the relative speeds of the two stars can be measured using the Doppler effect; the speed will be inversely proportional to the mass. This allows us to calculate the mass of each star. ...
Apparent Magnitude
... Types of Stars White dwarfs A red giant at the end stage of its evolution will throw off mass and leave behind a very small size (the size of the Earth), very dense star in which no nuclear reactions take place. It is very hot but its small size gives it a very small luminosity. As white dwarfs h ...
... Types of Stars White dwarfs A red giant at the end stage of its evolution will throw off mass and leave behind a very small size (the size of the Earth), very dense star in which no nuclear reactions take place. It is very hot but its small size gives it a very small luminosity. As white dwarfs h ...
Earth and Beyond - We can`t sign you in
... matter from the star will spiral into the black hole and as it does so the matter emits X ray radiation which can be detected. ...
... matter from the star will spiral into the black hole and as it does so the matter emits X ray radiation which can be detected. ...
Binary star formation
... Mechanisms for binary star formation Although very common, not obvious how to form binary stars: • Never observed the process happening • Wide range of scales involved in different binaries Possible mechanisms that have been suggested: • Fission - one star splits into two • Capture - one star captu ...
... Mechanisms for binary star formation Although very common, not obvious how to form binary stars: • Never observed the process happening • Wide range of scales involved in different binaries Possible mechanisms that have been suggested: • Fission - one star splits into two • Capture - one star captu ...
Stellar evolution
Stellar evolution is the process by which a star changes during its lifetime. Depending on the mass of the star, this lifetime ranges from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe. The table shows the lifetimes of stars as a function of their masses. All stars are born from collapsing clouds of gas and dust, often called nebulae or molecular clouds. Over the course of millions of years, these protostars settle down into a state of equilibrium, becoming what is known as a main-sequence star.Nuclear fusion powers a star for most of its life. Initially the energy is generated by the fusion of hydrogen atoms at the core of the main-sequence star. Later, as the preponderance of atoms at the core becomes helium, stars like the Sun begin to fuse hydrogen along a spherical shell surrounding the core. This process causes the star to gradually grow in size, passing through the subgiant stage until it reaches the red giant phase. Stars with at least half the mass of the Sun can also begin to generate energy through the fusion of helium at their core, whereas more-massive stars can fuse heavier elements along a series of concentric shells. Once a star like the Sun has exhausted its nuclear fuel, its core collapses into a dense white dwarf and the outer layers are expelled as a planetary nebula. Stars with around ten or more times the mass of the Sun can explode in a supernova as their inert iron cores collapse into an extremely dense neutron star or black hole. Although the universe is not old enough for any of the smallest red dwarfs to have reached the end of their lives, stellar models suggest they will slowly become brighter and hotter before running out of hydrogen fuel and becoming low-mass white dwarfs.Stellar evolution is not studied by observing the life of a single star, as most stellar changes occur too slowly to be detected, even over many centuries. Instead, astrophysicists come to understand how stars evolve by observing numerous stars at various points in their lifetime, and by simulating stellar structure using computer models.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.