the formation of the earth
... gases began to contract under its own gravitational influence. Gradually the atoms pulled closer and closer together and the cloud became smaller and smaller. It then developed some component of rotational motion, rotating faster and faster as it contracted, forming a disk-like shape.The greatest co ...
... gases began to contract under its own gravitational influence. Gradually the atoms pulled closer and closer together and the cloud became smaller and smaller. It then developed some component of rotational motion, rotating faster and faster as it contracted, forming a disk-like shape.The greatest co ...
Star Types - College of Engineering and Computer Science
... While the exterior layers expand, the helium core continues to contract, while growing in mass, and eventually becomes hot enough (100 million Kelvin) for helium to begin to fuse into carbon Carbon ash is deposited in core and eventually a helium-burning shell develops. This shell is itself surround ...
... While the exterior layers expand, the helium core continues to contract, while growing in mass, and eventually becomes hot enough (100 million Kelvin) for helium to begin to fuse into carbon Carbon ash is deposited in core and eventually a helium-burning shell develops. This shell is itself surround ...
Origin of the Universe
... more massive than our Sun. Such explosions distribute all the common elements such as Oxygen, Carbon, Nitrogen, Calcium and Iron into interstellar space where they enrich clouds of Hydrogen and Helium that are about to form new stars. They also create the heavier elements (such as gold, silver, lead ...
... more massive than our Sun. Such explosions distribute all the common elements such as Oxygen, Carbon, Nitrogen, Calcium and Iron into interstellar space where they enrich clouds of Hydrogen and Helium that are about to form new stars. They also create the heavier elements (such as gold, silver, lead ...
Hot-plate model of stars Test 2 & grades • Public viewing sessions
... Goal is to discover the model for • flux, the amount of energy we on Earth receive per second per area of telescope. ...
... Goal is to discover the model for • flux, the amount of energy we on Earth receive per second per area of telescope. ...
Poster - Arkansas Center for Space and Planetary Sciences
... other nearly edge-on from an observer’s viewpoint, the object’s variability results from the stars eclipsing each other and blocking some of the light. GX Gem belongs to a category of binary stars called close binaries since the two stars cannot be individually resolved in a telescope. By studying t ...
... other nearly edge-on from an observer’s viewpoint, the object’s variability results from the stars eclipsing each other and blocking some of the light. GX Gem belongs to a category of binary stars called close binaries since the two stars cannot be individually resolved in a telescope. By studying t ...
Lecture 11: Stars, HR diagram.
... There is a very tight relationship between luminosity and temperature We see that the Sun is in this sequence... Then there is something in common between the Sun and the rest of the stars in the main sequence.... They are all burning H into He in their cores More luminous = hotter = more massive! L ...
... There is a very tight relationship between luminosity and temperature We see that the Sun is in this sequence... Then there is something in common between the Sun and the rest of the stars in the main sequence.... They are all burning H into He in their cores More luminous = hotter = more massive! L ...
Abundances - Michigan State University
... to best reproduce all spectral features, incl. all absorption lines (can be 100’s or more) . Example for a r-process star (Sneden et al. ApJ 572 (2002) 861) ...
... to best reproduce all spectral features, incl. all absorption lines (can be 100’s or more) . Example for a r-process star (Sneden et al. ApJ 572 (2002) 861) ...
AST 105: Introduction to the Solar System HOMEWORK # 3
... photon of red light contain more or less energy than a photon of blue light? Red light has a longer wavelength, a smaller frequency, and thus a photon energy which is smaller than blue light. 4. In the movie Contact, Jodi Foster is shown listening on headphones to signals from space. Why is this fan ...
... photon of red light contain more or less energy than a photon of blue light? Red light has a longer wavelength, a smaller frequency, and thus a photon energy which is smaller than blue light. 4. In the movie Contact, Jodi Foster is shown listening on headphones to signals from space. Why is this fan ...
Light as a Wave (1) Distances to Stars
... The flux received from the light is proportional to its intrinsic brightness or luminosity (L) and inversely proportional to the square of the distance (d): ...
... The flux received from the light is proportional to its intrinsic brightness or luminosity (L) and inversely proportional to the square of the distance (d): ...
Sample Final - IUPUI Physics
... B) The Drake Equation C) The Tully-Fisher Relationship D) Parallax 86) In order to be able to determine if there might be life on an Earth sized planet what do we have to be able to do? A) Use a space based interferometer B) Block out the light from the star the planet is orbiting C) Take a spectrum ...
... B) The Drake Equation C) The Tully-Fisher Relationship D) Parallax 86) In order to be able to determine if there might be life on an Earth sized planet what do we have to be able to do? A) Use a space based interferometer B) Block out the light from the star the planet is orbiting C) Take a spectrum ...
Stellar Evolution Simulation
... 8. Compare and contrast the evolution of a sun like star to the evolution of a star smaller than the sun. You should include a comparison of their lifetimes, how they began, how they end, and their characteristics in the main sequence (radii, temperature, luminosity) ...
... 8. Compare and contrast the evolution of a sun like star to the evolution of a star smaller than the sun. You should include a comparison of their lifetimes, how they began, how they end, and their characteristics in the main sequence (radii, temperature, luminosity) ...
Astronomy Final Study Guide – Name: **This will be the biggest test
... 22. How does the atmosphere protect us from dangerous forms of radiation? Which forms does it protect us from? Be able to draw a diagram explaining how this happens. ...
... 22. How does the atmosphere protect us from dangerous forms of radiation? Which forms does it protect us from? Be able to draw a diagram explaining how this happens. ...
nucleosynthesis_oct28
... These bodies are composed of 4 elements and contain opposite qualities (hot, cold), (wet, dry). Bodies in the celestial region are composed of a special element, quintessence, or celestial matter. Celestial matter is eternal and unchangeable. There is a very close connection between the nature of th ...
... These bodies are composed of 4 elements and contain opposite qualities (hot, cold), (wet, dry). Bodies in the celestial region are composed of a special element, quintessence, or celestial matter. Celestial matter is eternal and unchangeable. There is a very close connection between the nature of th ...
Probing the first stars through the abundance of metal poor stars
... Chemical abundances of metal poor stars Probing the first stars – Stellar archeology Looking for the fossil records of early star formation and Galaxy evolution In metal poor systems of Milky way and its satellite galaxies. Complementary to high redshift observations (IGM, GRB, SNs) Nature of Fir ...
... Chemical abundances of metal poor stars Probing the first stars – Stellar archeology Looking for the fossil records of early star formation and Galaxy evolution In metal poor systems of Milky way and its satellite galaxies. Complementary to high redshift observations (IGM, GRB, SNs) Nature of Fir ...
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.