STAR TYPES
... Most stars, including the sun, are "main sequence stars," fueled by nuclear fusion converting hydrogen into helium. For these stars, the hotter they are, the brighter. These stars are in the most stable part of their existence; this stage generally lasts for about 5 billion years. As stars begin to ...
... Most stars, including the sun, are "main sequence stars," fueled by nuclear fusion converting hydrogen into helium. For these stars, the hotter they are, the brighter. These stars are in the most stable part of their existence; this stage generally lasts for about 5 billion years. As stars begin to ...
Lecture 4a - University of Rochester
... energy with its surrounding and a steady state is reached where there is no net energy flow. • To maintain a steady state the body must emit radiation at the same rate that it is absorbed. • A black body is an object that absorbs equally well radiation at all wavelengths. • A black body is described ...
... energy with its surrounding and a steady state is reached where there is no net energy flow. • To maintain a steady state the body must emit radiation at the same rate that it is absorbed. • A black body is an object that absorbs equally well radiation at all wavelengths. • A black body is described ...
SUMMARY White dwarfs, neutron stars, and black holes are the
... A neutron star forms when a massive star's iron core collapses and triggers a supernova explosion. The collapse compresses the core's protons and electrons together to make neutrons, forming a ball of neutrons with a radius of a mere 10 kilometers that may contain up to about 2 to 3 solar masses. Co ...
... A neutron star forms when a massive star's iron core collapses and triggers a supernova explosion. The collapse compresses the core's protons and electrons together to make neutrons, forming a ball of neutrons with a radius of a mere 10 kilometers that may contain up to about 2 to 3 solar masses. Co ...
Interstellar Medium (ISM) Star Formation Formation of Planetary Systems
... Typical values for the molecular gas: € • ρ ~ 10-19 g cm-3 • T ~ 10 K Use these numbers in the Jeans mass formula, and take µ = 2 for molecular hydrogen: ...
... Typical values for the molecular gas: € • ρ ~ 10-19 g cm-3 • T ~ 10 K Use these numbers in the Jeans mass formula, and take µ = 2 for molecular hydrogen: ...
Powerpoint Presentation (large file)
... • A high-mass star dies in a violent cataclysm in which its core collapses and most of its matter is ejected into space at high speeds • The luminosity of the star increases suddenly by a factor of around 108 during this explosion, producing a supernova • The matter ejected from the supernova, movin ...
... • A high-mass star dies in a violent cataclysm in which its core collapses and most of its matter is ejected into space at high speeds • The luminosity of the star increases suddenly by a factor of around 108 during this explosion, producing a supernova • The matter ejected from the supernova, movin ...
Life Cycle of a Star - Intervention Worksheet
... _____ 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 nebula _____ What happens next depends on the mass of the star. _____ Heat and pressure ...
... _____ 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 nebula _____ What happens next depends on the mass of the star. _____ Heat and pressure ...
Killer Skies
... Unlike medium-mass stars, massive stars finally can get hot enough to ignite carbon fusion at a temperature of about 1 billion Kelvin. This pattern of core ignition and shell ignition continues with a series of heavier nuclei as fusion fuel. At higher temperatures than carbon fusion, nuclei of oxyge ...
... Unlike medium-mass stars, massive stars finally can get hot enough to ignite carbon fusion at a temperature of about 1 billion Kelvin. This pattern of core ignition and shell ignition continues with a series of heavier nuclei as fusion fuel. At higher temperatures than carbon fusion, nuclei of oxyge ...
Fate of Stars
... White Dwarves Mass vs Radius • In WD, gravity is balanced by pressure due to degenerate electrons • A heavier WD will have smaller radius • if Mass(WD) > 1.4 M(Sun) electrons can not resist gravity ! called Chandrasekhar limit and no WD has a mass greater than this • If WD can acquire mass from ...
... White Dwarves Mass vs Radius • In WD, gravity is balanced by pressure due to degenerate electrons • A heavier WD will have smaller radius • if Mass(WD) > 1.4 M(Sun) electrons can not resist gravity ! called Chandrasekhar limit and no WD has a mass greater than this • If WD can acquire mass from ...
32Brightness
... higher energy levels and spontaneously fall to lower levels, emitting light in the process • Absorption from cooler gases in front of continuum source, where discrete colors are absorbed by atoms – From emission and absorption lines, get composition of objects and also their temperature ...
... higher energy levels and spontaneously fall to lower levels, emitting light in the process • Absorption from cooler gases in front of continuum source, where discrete colors are absorbed by atoms – From emission and absorption lines, get composition of objects and also their temperature ...
English Summary
... TARS are born, live and die similarly to any human being in the Universe. This thesis deals with the final stages of evolution (life) experienced by stars like our Sun prior to their death, the so-called Planetary Nebula phase. In 5 billion years our Sun also will experience this phase and will beco ...
... TARS are born, live and die similarly to any human being in the Universe. This thesis deals with the final stages of evolution (life) experienced by stars like our Sun prior to their death, the so-called Planetary Nebula phase. In 5 billion years our Sun also will experience this phase and will beco ...
StarIntro_sb12
... The enormous pressure and heat in a star’s core convert matter into energy. Stars consist of controlled atomic reactions called nuclear fusion in which hydrogen (nuclei) atoms fuse to form helium (nuclei) atoms. During each step of the process, mass is lost and energy is released. ...
... The enormous pressure and heat in a star’s core convert matter into energy. Stars consist of controlled atomic reactions called nuclear fusion in which hydrogen (nuclei) atoms fuse to form helium (nuclei) atoms. During each step of the process, mass is lost and energy is released. ...
Starlight & Stars - Wayne State University Physics and Astronomy
... Ionized helium and metals; hydrogen very weak Neutral helium, ionized metals; hydrogen stronger Hydrogen strongest; singly-ionized metals ...
... Ionized helium and metals; hydrogen very weak Neutral helium, ionized metals; hydrogen stronger Hydrogen strongest; singly-ionized metals ...
key - Scioly.org
... The CNO cycle is a fusion reaction (1 point) that mainly stars of greater than 1.3 solar masses (1 point) use to convert hydrogen into helium. Proton-proton chain reactions are more important in stars with less mass (1 point). The cycle involves carbon, nitrogen, and oxygen acting as catalysts for f ...
... The CNO cycle is a fusion reaction (1 point) that mainly stars of greater than 1.3 solar masses (1 point) use to convert hydrogen into helium. Proton-proton chain reactions are more important in stars with less mass (1 point). The cycle involves carbon, nitrogen, and oxygen acting as catalysts for f ...
The mystery of cosmic oceans and dunes Earth
... Tokyo, February 17, 2015: Simulations by researchers at Tokyo Institute of Technology and Tsinghua University indicate that Earth-like planets are more likely to be found orbiting Sun-like stars rather than lower-mass stars that are currently targeted, in terms of water contents of planets. The sear ...
... Tokyo, February 17, 2015: Simulations by researchers at Tokyo Institute of Technology and Tsinghua University indicate that Earth-like planets are more likely to be found orbiting Sun-like stars rather than lower-mass stars that are currently targeted, in terms of water contents of planets. The sear ...
PPT 15MB - HubbleSOURCE
... Amazing network of long, straight filaments seen in great detail for first time in ionized gas; some of them follow magnetic field lines; New compact nebulae discovered with young massive stars, ranging from early to late stages of star formation Many candidate massive stars identified by brig ...
... Amazing network of long, straight filaments seen in great detail for first time in ionized gas; some of them follow magnetic field lines; New compact nebulae discovered with young massive stars, ranging from early to late stages of star formation Many candidate massive stars identified by brig ...
M104: The Sombrero Galaxy
... This photogenic galaxy looks like a broad-brimmed Mexican hat floating in space. Appropriately called the Sombrero Galaxy, its catalogue name is Messier 104 (M104). Thick dust lanes make up the brim of the galaxy. The brim winds into the brilliant white crown, made up of a central bulge of older sta ...
... This photogenic galaxy looks like a broad-brimmed Mexican hat floating in space. Appropriately called the Sombrero Galaxy, its catalogue name is Messier 104 (M104). Thick dust lanes make up the brim of the galaxy. The brim winds into the brilliant white crown, made up of a central bulge of older sta ...
Smiley Radio Telescope Lab 1 What`s Between the Stars?
... So how does hydrogen gas emit radio waves? Here’s the science: A neutral hydrogen atom consists of a proton surrounded by an electron. One property that both an electron and a proton have is something called spin (Figure 2). Through a crude analogy, spin can be thought of as a spinning earth orbitin ...
... So how does hydrogen gas emit radio waves? Here’s the science: A neutral hydrogen atom consists of a proton surrounded by an electron. One property that both an electron and a proton have is something called spin (Figure 2). Through a crude analogy, spin can be thought of as a spinning earth orbitin ...