THE HISTORY OF THE UNIVERSE IN ONE EASY LESSON
... “Astronomy is more than the study of stars and planets. It is the study of the universe in which we humans exist. You and I live on a small planet circling a small sun drifting through the universe, but astronomy can take us beyond these boundaries and help us not only see where we are in the univer ...
... “Astronomy is more than the study of stars and planets. It is the study of the universe in which we humans exist. You and I live on a small planet circling a small sun drifting through the universe, but astronomy can take us beyond these boundaries and help us not only see where we are in the univer ...
Chapter 07
... If a star is moving toward Earth, the lines in its spectrum are shifted slightly toward shorter wavelength (higher frequency). This shifts the absorption lines toward the blue end of the spectrum, so it’s called a blue shift. If a star is moving away from Earth, the lines in its spectrum are shifted ...
... If a star is moving toward Earth, the lines in its spectrum are shifted slightly toward shorter wavelength (higher frequency). This shifts the absorption lines toward the blue end of the spectrum, so it’s called a blue shift. If a star is moving away from Earth, the lines in its spectrum are shifted ...
Powerpoint
... through the surface of the star. A brief, hard ultra-violet (or even soft x-ray) transient ensues as a small amount of mass expands and cools very rapidly. The transient is brighter and longer for larger progenitors but hotter for smaller ones ...
... through the surface of the star. A brief, hard ultra-violet (or even soft x-ray) transient ensues as a small amount of mass expands and cools very rapidly. The transient is brighter and longer for larger progenitors but hotter for smaller ones ...
Globular Clusters Dynamic Lives The
... roughly like those between molecules in a uniform-temperature gas. The stars are not physically colliding in this celestial pinball game, just deflecting each other gravitationally. This energy exchange eventually leads to thermal equilibrium. In a typical cluster this takes about a hundred million ...
... roughly like those between molecules in a uniform-temperature gas. The stars are not physically colliding in this celestial pinball game, just deflecting each other gravitationally. This energy exchange eventually leads to thermal equilibrium. In a typical cluster this takes about a hundred million ...
6-8 question answers
... Stars are forming in the Solar System as you read this. TRUE. Stars are continually being formed and destroyed. Stars are formed, or born, in clouds of gas and dust in the interstellar medium. Gravity squeezes the mass of these “star nurseries” so that the centers become incredibly dense and hot. T ...
... Stars are forming in the Solar System as you read this. TRUE. Stars are continually being formed and destroyed. Stars are formed, or born, in clouds of gas and dust in the interstellar medium. Gravity squeezes the mass of these “star nurseries” so that the centers become incredibly dense and hot. T ...
Picture: Alnitak is the left-hand star in Orion`s Belt. Image: NASA
... times that of the Sun. Often they are found together with O stars in OB associations since, being massive, they are short-lived and therefore do not survive long enough to move far from the place where they were formed. Their brief main sequence careers, measured in tens of millions of years, probab ...
... times that of the Sun. Often they are found together with O stars in OB associations since, being massive, they are short-lived and therefore do not survive long enough to move far from the place where they were formed. Their brief main sequence careers, measured in tens of millions of years, probab ...
Brown_Dwarfs
... Molecular clouds with density greater than the Jeans Density will begin to collapse under their own gravity in the same way we learned how stars are formed in class. As the cloud contracts, its gravitational energy is converted to thermal energy, and thus the cloud begins to heat up. ...
... Molecular clouds with density greater than the Jeans Density will begin to collapse under their own gravity in the same way we learned how stars are formed in class. As the cloud contracts, its gravitational energy is converted to thermal energy, and thus the cloud begins to heat up. ...
Sample Answer Sheet for The 10 Tourist Wonders of the
... As much as 90% of the star’s material can be thrown off during the explosion and, in the process, new (heavier) elements are made, and then distributed at high speed into the Galaxy. In many ways, life on Earth owes its existence to supernovae and the fact that they “recycle” the material of early g ...
... As much as 90% of the star’s material can be thrown off during the explosion and, in the process, new (heavier) elements are made, and then distributed at high speed into the Galaxy. In many ways, life on Earth owes its existence to supernovae and the fact that they “recycle” the material of early g ...
Chapter 10 Hertzsprung-Russel Diagrams and Distance to Stars
... to the stars were unknown, one could not determine the intrinsic brightness of a star, but only its apparent brightness. As we’ve already said, a bright star that’s very far away would appear much fainter than a dim star that’s much closer. To overcome this problem, scientists began to look at stars ...
... to the stars were unknown, one could not determine the intrinsic brightness of a star, but only its apparent brightness. As we’ve already said, a bright star that’s very far away would appear much fainter than a dim star that’s much closer. To overcome this problem, scientists began to look at stars ...
Stars and Constellations Power Point
... Stars are born when there is a large amount of gas and dust in a small area that becomes so hot that nuclear fusion starts. The gas continues to burn until it runs out. More burning gas = a bigger and brighter star! ...
... Stars are born when there is a large amount of gas and dust in a small area that becomes so hot that nuclear fusion starts. The gas continues to burn until it runs out. More burning gas = a bigger and brighter star! ...
here
... each other. One of these stars Proxima Centauri is the closest star to Earth next to our sun. There are many kinds of stars, big and small, close and far, bright and dim, some even change in brightness in a matter of hours (these are called pulsating stars). When most stars get old they bloat and be ...
... each other. One of these stars Proxima Centauri is the closest star to Earth next to our sun. There are many kinds of stars, big and small, close and far, bright and dim, some even change in brightness in a matter of hours (these are called pulsating stars). When most stars get old they bloat and be ...
PowerPoint - Chandra X
... Chandra Science Highlights IC 443: A Supernova Remnant with a Newly Discovered Neutron Star 5,000 light years from Earth This Chandra image shows a point-like source of X-rays inside a cloud of high energy particles which is embedded in the supernova remnant IC443. Using this image, along with radio ...
... Chandra Science Highlights IC 443: A Supernova Remnant with a Newly Discovered Neutron Star 5,000 light years from Earth This Chandra image shows a point-like source of X-rays inside a cloud of high energy particles which is embedded in the supernova remnant IC443. Using this image, along with radio ...
Nebulas - WLWV Staff Blogs
... together to create larger masses, which then gather other material until they become big enough to be known as stars. ...
... together to create larger masses, which then gather other material until they become big enough to be known as stars. ...
N-Body Simulations of Star Clusters with IMBH
... Observations indicate that there might be a connection between ULX and star clusters. Matsumoto et al. (2001) for example found a bright X-ray source at the center of the starburst galaxy M82 with an Eddington luminosity corresponding to a black hole of several hundred ...
... Observations indicate that there might be a connection between ULX and star clusters. Matsumoto et al. (2001) for example found a bright X-ray source at the center of the starburst galaxy M82 with an Eddington luminosity corresponding to a black hole of several hundred ...
Hierarchical galaxy formation
... Nuclear reactions in the stellar core support a star against the inward force of its own gravity. When the star’s nuclear fuel runs out it should begin to collapse… ...
... Nuclear reactions in the stellar core support a star against the inward force of its own gravity. When the star’s nuclear fuel runs out it should begin to collapse… ...
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.