File - greenscapes4you
... Most stars fall along the main sequence – upper left to lower right. These stars fuse hydrogen into helium in their cores and have a wide range of life spans, which depend on their mass. Higher mass stars on main sequence have shorter life spans. A star has a limited supply of core hydrogen and ther ...
... Most stars fall along the main sequence – upper left to lower right. These stars fuse hydrogen into helium in their cores and have a wide range of life spans, which depend on their mass. Higher mass stars on main sequence have shorter life spans. A star has a limited supply of core hydrogen and ther ...
Forming Planets
... How long does it take to make a solar system? A. 1 million years. B. 10 million years. C. 100 million years. D. 1 billion years. ...
... How long does it take to make a solar system? A. 1 million years. B. 10 million years. C. 100 million years. D. 1 billion years. ...
Stellar Properties
... what would be the distance to the star? A)1/5, b)1. c)5, d)25 pc 2. Star A and B have same luminosity. If star A is 4 times closer to Earth then star B, then _____ to earthly viewer.: a=A is 4 x brighter, b=B is 4x brighter, c=A is 16 times brighter d=B is 16 times brighter, e=A is 64x brighter 3. A ...
... what would be the distance to the star? A)1/5, b)1. c)5, d)25 pc 2. Star A and B have same luminosity. If star A is 4 times closer to Earth then star B, then _____ to earthly viewer.: a=A is 4 x brighter, b=B is 4x brighter, c=A is 16 times brighter d=B is 16 times brighter, e=A is 64x brighter 3. A ...
Stats talk - Harvard University
... Probing the evolution of stellar systems Andreas Zezas Harvard-Smithsonian Center for Astrophysics ...
... Probing the evolution of stellar systems Andreas Zezas Harvard-Smithsonian Center for Astrophysics ...
Assignment 4 Solutions
... White dwarfs, neutron stars and black holes are similar in that they are all final “death” states of stars which have come to the end of their evolutionary cycles. Specifically, at the end of the “red giant” stage, when fusion of carbon into iron begins to dominate in the core, all stars commence th ...
... White dwarfs, neutron stars and black holes are similar in that they are all final “death” states of stars which have come to the end of their evolutionary cycles. Specifically, at the end of the “red giant” stage, when fusion of carbon into iron begins to dominate in the core, all stars commence th ...
Barium Stars Observed with the Coude Echelle Spectrometer
... factor of four, and strontium even more, butthe other observable heavy elements are virtually unchanged (Fig. 2). Interestingly, there seems to be a connection to normal giants. In recent years five bright red giants and a supergiant - all 01 spectral type K - have been analysed at Kiel on the basis ...
... factor of four, and strontium even more, butthe other observable heavy elements are virtually unchanged (Fig. 2). Interestingly, there seems to be a connection to normal giants. In recent years five bright red giants and a supergiant - all 01 spectral type K - have been analysed at Kiel on the basis ...
binary star
... • Hydrogen burning migrates outward. The star’s outer envelope expands. • Its surface cools and becomes red. • The core collapses as helium is converted to carbon. Eventually all nuclear fuel is used and gravity squeezes the star. ...
... • Hydrogen burning migrates outward. The star’s outer envelope expands. • Its surface cools and becomes red. • The core collapses as helium is converted to carbon. Eventually all nuclear fuel is used and gravity squeezes the star. ...
ď - Google Sites
... 3. Shade other color bands as follows: Stars up to 5,000 °C are orange-red, up to 6,000 °C yellowwhite, up to 7,500 °C blue-white, and up to 40,000 °C blue. 4. Label the main sequence, the red supergiants, and the white dwarfs. Conclusions: 1. Based on our results, we conclude that ...
... 3. Shade other color bands as follows: Stars up to 5,000 °C are orange-red, up to 6,000 °C yellowwhite, up to 7,500 °C blue-white, and up to 40,000 °C blue. 4. Label the main sequence, the red supergiants, and the white dwarfs. Conclusions: 1. Based on our results, we conclude that ...
Siriusposter
... The ROSAT all-sky x-ray and extreme ultraviolet (EUV) surveys discovered many new hot white dwarfs. At these energies, white dwarfs are far brighter than most normal stars, and with ROSAT’s help we have been able to identify over 20 of these degenerate objects in binaries with bright, normal compani ...
... The ROSAT all-sky x-ray and extreme ultraviolet (EUV) surveys discovered many new hot white dwarfs. At these energies, white dwarfs are far brighter than most normal stars, and with ROSAT’s help we have been able to identify over 20 of these degenerate objects in binaries with bright, normal compani ...
slides - Walter Burke Institute for Theoretical Physics
... Lars Bildsten Kavli Institute for Theoretical ...
... Lars Bildsten Kavli Institute for Theoretical ...
The Family of Stars
... b) Any binary system with a combination of period P and separation a that obeys Kepler’s 3rd Law must have a total mass of 1 solar mass. ...
... b) Any binary system with a combination of period P and separation a that obeys Kepler’s 3rd Law must have a total mass of 1 solar mass. ...
Spectroscopy – the study of the colors of light (the spectrum) given
... Titanium lines are common because they easily lose their electrons. ...
... Titanium lines are common because they easily lose their electrons. ...
Lecture 19 The Milky Way Galaxy
... • Previously, astronomers had thought that galaxy was much smaller and that we were near the center because they did not take into account the dimming of light from stars ...
... • Previously, astronomers had thought that galaxy was much smaller and that we were near the center because they did not take into account the dimming of light from stars ...
Star Life Cycle Review 1. What is the first stage of star creation? A
... 12. What are the two variables that are incorporated in the Hertzsprung-Russell diagram? A. a star's luminosity (brightness) and its distance from earth B. a star's age and its distance from earth C. a star's age and its surface temperature D. a star's luminosity (brightness) and its surface temper ...
... 12. What are the two variables that are incorporated in the Hertzsprung-Russell diagram? A. a star's luminosity (brightness) and its distance from earth B. a star's age and its distance from earth C. a star's age and its surface temperature D. a star's luminosity (brightness) and its surface temper ...
Stars
... Nebulas – large clouds of gas and dust As particles in the nebula contract they increase in temperature until the reach 10 million K. This is when fusion begins. Energy given off from the fusion process powers the star ...
... Nebulas – large clouds of gas and dust As particles in the nebula contract they increase in temperature until the reach 10 million K. This is when fusion begins. Energy given off from the fusion process powers the star ...
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.