Nuclear Physics - fission, fusion, and the stars
... huge variety of interconnected chain reactions. For it to proceed the different nuclei must be at high T. A simple fusion process- a proton fuses with C-12 The radiation emitted during the to make N-13, with emission of a photon. fusion keeps T high. Slowly the heavier elements up to Fe (whose nucle ...
... huge variety of interconnected chain reactions. For it to proceed the different nuclei must be at high T. A simple fusion process- a proton fuses with C-12 The radiation emitted during the to make N-13, with emission of a photon. fusion keeps T high. Slowly the heavier elements up to Fe (whose nucle ...
AY 12 Homework #4 Solutions Winter 2016 Longer Problems 1. a
... e) Stars less than 8 M are “low-mass stars” that end their lives as white dwarfs (and planetary nebulae). Stars above 8 M (“high-mass stars”) end their lives as core-collapse supernovae. These stars are able to burn heavier elements for fuel, e.g., carbon, oxygen, and silicon. f) A star cannot bec ...
... e) Stars less than 8 M are “low-mass stars” that end their lives as white dwarfs (and planetary nebulae). Stars above 8 M (“high-mass stars”) end their lives as core-collapse supernovae. These stars are able to burn heavier elements for fuel, e.g., carbon, oxygen, and silicon. f) A star cannot bec ...
Life Cycle of a Star - Intervention Worksheet
... The stages below are not in the right order. Number the stages in the correct order. _____ The star begins to run out of fuel and expands into a red giant or red super giant. _____ Stars start out as diffused clouds of gas and dust drifting through space. A single one of these clouds is called a neb ...
... The stages below are not in the right order. Number the stages in the correct order. _____ The star begins to run out of fuel and expands into a red giant or red super giant. _____ Stars start out as diffused clouds of gas and dust drifting through space. A single one of these clouds is called a neb ...
Ch18 Life - UCF Physics
... – Ne = The number of Earth-like planets (planets with liquid water) within each planetary system (we are learning about this now…..expect an answer in 3-5 years) – Fl = The fraction of Earth-like planets where life develops (we could have some idea in 20 years) – Fi = The fraction of life sites wher ...
... – Ne = The number of Earth-like planets (planets with liquid water) within each planetary system (we are learning about this now…..expect an answer in 3-5 years) – Fl = The fraction of Earth-like planets where life develops (we could have some idea in 20 years) – Fi = The fraction of life sites wher ...
Star Factories: Nuclear Fusion and the Creation of the Elements
... The R-Process When the supernova explodes, large numbers of neutrons are shot out of the interior of the star at high velocities. Think of these like pellets in a shot gun shell that has been fired. These neutrons pass through the outer regions of the star, colliding with the atoms already there (m ...
... The R-Process When the supernova explodes, large numbers of neutrons are shot out of the interior of the star at high velocities. Think of these like pellets in a shot gun shell that has been fired. These neutrons pass through the outer regions of the star, colliding with the atoms already there (m ...
Classification of magnetized star-planet interactions: dynamics and
... planetary magnetospheres similar to those of our solar system, such outflows are expected to be magnetized. On the other hand, the environment of short period orbits consists of the sweeping stellar wind plasma that is known to attain super-sonic velocities. This framework suggests the manifestation ...
... planetary magnetospheres similar to those of our solar system, such outflows are expected to be magnetized. On the other hand, the environment of short period orbits consists of the sweeping stellar wind plasma that is known to attain super-sonic velocities. This framework suggests the manifestation ...
2.5.2 development of a star
... star spends ~80% of its lifetime on the main sequence. During this time it is stable as the gravitational forces that enable hydrogen burning balance and pull the star in, balance with the gas pressure pushing out. This is much like the gas pressure inside a balloon balancing with the tension in ...
... star spends ~80% of its lifetime on the main sequence. During this time it is stable as the gravitational forces that enable hydrogen burning balance and pull the star in, balance with the gas pressure pushing out. This is much like the gas pressure inside a balloon balancing with the tension in ...
Activity: Stellar Spectra
... 5. Using the spectra given try to identify the mystery star at the bottom of the page. Click on the boxes for the elements you think are present then click ‘Did I get it Right?’ 6. If you got it right record the elements present in your observations table, then click on ‘Give me another star’ and tr ...
... 5. Using the spectra given try to identify the mystery star at the bottom of the page. Click on the boxes for the elements you think are present then click ‘Did I get it Right?’ 6. If you got it right record the elements present in your observations table, then click on ‘Give me another star’ and tr ...
The Life Cycles of Stars
... blown away to form a ring around the core. This ring is called a planetary nebula. When the last of the helium atoms in the core are fused into carbon atoms, the medium size star begins to die. Gravity causes the last of the star’s matter to collapse inward and compact. This is the white dwarf stage ...
... blown away to form a ring around the core. This ring is called a planetary nebula. When the last of the helium atoms in the core are fused into carbon atoms, the medium size star begins to die. Gravity causes the last of the star’s matter to collapse inward and compact. This is the white dwarf stage ...
Chemical Composition of Planetary Nebulae: The Galaxy and the
... the SMC does not favour the formation of the higher mass progenitors that give rise to Type I bipolar (or asymmetric) PN. Recently, Marigo et al. [15] have presented abundances of Galactic PN for which ISO and IUE spectra are available, so that their abundances are presumably well determined, as all ...
... the SMC does not favour the formation of the higher mass progenitors that give rise to Type I bipolar (or asymmetric) PN. Recently, Marigo et al. [15] have presented abundances of Galactic PN for which ISO and IUE spectra are available, so that their abundances are presumably well determined, as all ...
Astronomy 102, Spring 2003 Solutions to Review Problems
... Spiral galaxies, like our own, have a lot of cool gas (including both atomic and molecular galaxy). There is another type of large galaxy known as an Elliptical galaxy. Such galaxies usually do not have much cool gas. How would you expect the colors of stars seen in an elliptical galaxy to differ fr ...
... Spiral galaxies, like our own, have a lot of cool gas (including both atomic and molecular galaxy). There is another type of large galaxy known as an Elliptical galaxy. Such galaxies usually do not have much cool gas. How would you expect the colors of stars seen in an elliptical galaxy to differ fr ...
Mark scheme for Support Worksheet – Topic E, Worksheet 1
... A constellation is a collection of stars usually in a recognisable pattern that are not necessarily physically close to each other; whereas a stellar cluster consists of stars that are close to each other and attract each other gravitationally. ...
... A constellation is a collection of stars usually in a recognisable pattern that are not necessarily physically close to each other; whereas a stellar cluster consists of stars that are close to each other and attract each other gravitationally. ...
How stars form slide show File
... drawn together over millions of years by gravity. •As the gas compresses it changes its gravitational potential energy changes into kinetic energy. •The KE changes into heat and the protostar becomes hotter and hotter as it becomes smaller. •Eventually the protostar becomes hot enough for nuclear fu ...
... drawn together over millions of years by gravity. •As the gas compresses it changes its gravitational potential energy changes into kinetic energy. •The KE changes into heat and the protostar becomes hotter and hotter as it becomes smaller. •Eventually the protostar becomes hot enough for nuclear fu ...
Untitled
... The night sky is illed with the remains of supernovas. They are colorful clouds of dust and gas left over from the explosions. No two are exactly alike. One of the most beautiful such clouds is the Crab Nebula. Through a telescope, it looks like a lacy burst of multicolored strands. The Crab Nebula ...
... The night sky is illed with the remains of supernovas. They are colorful clouds of dust and gas left over from the explosions. No two are exactly alike. One of the most beautiful such clouds is the Crab Nebula. Through a telescope, it looks like a lacy burst of multicolored strands. The Crab Nebula ...
Using exoplanet systems with highly elliptical orbits to search for star
... their host star by studying a sample of planetary systems known to contain massive planets on short period, highly elliptical orbits. While recent studies in the optical, UV, and X-Ray have shown enhanced chromospheric activity for stars hosting exoplanets with orbital semi-major axes less than 0.1 ...
... their host star by studying a sample of planetary systems known to contain massive planets on short period, highly elliptical orbits. While recent studies in the optical, UV, and X-Ray have shown enhanced chromospheric activity for stars hosting exoplanets with orbital semi-major axes less than 0.1 ...
Document
... on the vertical axis & surface temperature (spectral type) on the horizontal axis • We can use spectroscopy to determine the spectral type & luminosity of a star • Main Sequence (MS): Prominent line of points running from the upper left to lower right on an HR Diagram; these stars shine by fusing hy ...
... on the vertical axis & surface temperature (spectral type) on the horizontal axis • We can use spectroscopy to determine the spectral type & luminosity of a star • Main Sequence (MS): Prominent line of points running from the upper left to lower right on an HR Diagram; these stars shine by fusing hy ...
obafgkm - Piscataway High School
... earth. Determine what information about stars can be revealed using the following methods: Parallax effect ...
... earth. Determine what information about stars can be revealed using the following methods: Parallax effect ...
introduction to planetary science: the geological perspective1
... compounds in the nebula are described as having high melting temperatures rather than condensing at high temperatures from gas to solid form. Despite its strong points, and there are many, the readers of Elements may share some of my concerns. Contrary to the book’s subtitle, its geologic perspectiv ...
... compounds in the nebula are described as having high melting temperatures rather than condensing at high temperatures from gas to solid form. Despite its strong points, and there are many, the readers of Elements may share some of my concerns. Contrary to the book’s subtitle, its geologic perspectiv ...
29.3-stellar-evolution
... The density and temp in a star increase toward the center, where energy is generated by nuclear fusion. Stellar Evolution As long as a star is changing hydrogen into helium, nuclear fusion, it will be a main sequence star. Star formation The formation of a star begins with a cloud of dust and ...
... The density and temp in a star increase toward the center, where energy is generated by nuclear fusion. Stellar Evolution As long as a star is changing hydrogen into helium, nuclear fusion, it will be a main sequence star. Star formation The formation of a star begins with a cloud of dust and ...
The Life Cycles of Stars MEDIUM STARS MASSIVE STARS
... called a planetary nebula. When the last of the helium atoms in the core are fused into carbon atoms, the medium size star begins to die. Gravity causes the last of the star's matter to collapse inward and compact. This is the white dwarf stage. At this stage, the star's matter is extremely dense. W ...
... called a planetary nebula. When the last of the helium atoms in the core are fused into carbon atoms, the medium size star begins to die. Gravity causes the last of the star's matter to collapse inward and compact. This is the white dwarf stage. At this stage, the star's matter is extremely dense. W ...
Ch.21 Stars, Galaxies, and the Universe Section 3: Lives of Stars
... High-mass stars quickly evolve into brilliant supergiants When a supergiant runs out of fuel, it can explode suddenly The supernovas can become part of a nebula This nebula can then contract to form a new, partly recycled star o Neutron Stars: are the remains of high-mass stars They are ev ...
... High-mass stars quickly evolve into brilliant supergiants When a supergiant runs out of fuel, it can explode suddenly The supernovas can become part of a nebula This nebula can then contract to form a new, partly recycled star o Neutron Stars: are the remains of high-mass stars They are ev ...
Lecture 18
... Summary of Galactic Recycling • Stars make new elements by fusion. • Dying stars expel gas and new elements, producing hot bubbles (~106 K). • Hot gas cools, allowing atomic hydrogen clouds to form ...
... Summary of Galactic Recycling • Stars make new elements by fusion. • Dying stars expel gas and new elements, producing hot bubbles (~106 K). • Hot gas cools, allowing atomic hydrogen clouds to form ...
Planetary nebula
A planetary nebula, often abbreviated as PN or plural PNe, is a kind of emission nebula consisting of an expanding glowing shell of ionized gas ejected from old red giant stars late in their lives. The word ""nebula"" is Latin for mist or cloud and the term ""planetary nebula"" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years.A mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energises the shell of nebulous gas around the central star, appearing as a bright coloured planetary nebula at several discrete visible wavelengths.Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances.In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. About one-fifth are roughly spherical, but the majority are not spherically symmetric. The mechanisms which produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may play a role.