jackie822 beanerbutt777 life cycle of a star
... http://solarsystem.nasa.gov/multimedia/gallery/prominence.gif ...
... http://solarsystem.nasa.gov/multimedia/gallery/prominence.gif ...
Name - CLC Charter School
... star’s iron core is massive enough, when it collapses, it will explode in a supernova. Some scientists think that type Ib supernovae are actually type II. The hydrogen was probably blown away by the huge star’s strong stellar winds before the star exploded which explains the lack of hydrogen in its ...
... star’s iron core is massive enough, when it collapses, it will explode in a supernova. Some scientists think that type Ib supernovae are actually type II. The hydrogen was probably blown away by the huge star’s strong stellar winds before the star exploded which explains the lack of hydrogen in its ...
Planetary Nebulae – White dwarfs
... • All heavy elements are created and dispersed through the galaxy by stars • Without high mass stars, no heavy elements • Our atoms were once parts of stars that died ...
... • All heavy elements are created and dispersed through the galaxy by stars • Without high mass stars, no heavy elements • Our atoms were once parts of stars that died ...
common constellations
... In 1054 A.D., Chinese astronomers wrote down that a "guest star" had suddenly appeared in their night skies. At the same time, Native Americans made drawings in at least two places that appear to record the same event. What was somewhat casually noted as a guest star was in fact a giant star that ha ...
... In 1054 A.D., Chinese astronomers wrote down that a "guest star" had suddenly appeared in their night skies. At the same time, Native Americans made drawings in at least two places that appear to record the same event. What was somewhat casually noted as a guest star was in fact a giant star that ha ...
East Valley Astronomy Club
... Their textures are reproduced only if they temperatures > 1575 C, for minutes, then cooled over a matter of hours. ...
... Their textures are reproduced only if they temperatures > 1575 C, for minutes, then cooled over a matter of hours. ...
Endpoints of stellar evolution
... Shock wave hits inner ring of material and creates intense X-ray radiation ...
... Shock wave hits inner ring of material and creates intense X-ray radiation ...
Document
... Very high rotation rates can be reached simply via conservation of angular momentum. This is faster than any known (or possible) neutron star. Mass and angular momentum are lost during the collapse. ...
... Very high rotation rates can be reached simply via conservation of angular momentum. This is faster than any known (or possible) neutron star. Mass and angular momentum are lost during the collapse. ...
Supernovae March 23 − Supernova 1987A
... Sirius A, a main-sequence star Sirius B, an earth-sized white dwarf ...
... Sirius A, a main-sequence star Sirius B, an earth-sized white dwarf ...
Astronomy 102, Spring 2003 Solutions to Review Problems
... 2. Consider a binary system consisting of a main sequence star and a white dwarf companion. Which star is older? Which star started its life with more mass? Given that we’ve talked about how far apart stars are in the galaxy, they almost never run into each other. (It’s a different matter in the cor ...
... 2. Consider a binary system consisting of a main sequence star and a white dwarf companion. Which star is older? Which star started its life with more mass? Given that we’ve talked about how far apart stars are in the galaxy, they almost never run into each other. (It’s a different matter in the cor ...
Neutron Stars
... Neutron Stars • A neutron star forms during the supernova explosion if the mass of the collapsing core exceeds the Chandrasekhar limit of 1.4 Msun • Degenerate neutron pressure count-balances the gravitation • A neutron star is a dense stellar corpse consisting primarily of ...
... Neutron Stars • A neutron star forms during the supernova explosion if the mass of the collapsing core exceeds the Chandrasekhar limit of 1.4 Msun • Degenerate neutron pressure count-balances the gravitation • A neutron star is a dense stellar corpse consisting primarily of ...
Stellar Spire in the Eagle Nebula
... gas that reside in chaotic neighborhoods, where energy from newborn stars sculpts fantasy-like landscapes in the gas. The tower is a giant incubator for these newborn stars. A torrent of ultraviolet light from a band of massive, hot, young stars [off the top of the image] is eroding the pillar. The ...
... gas that reside in chaotic neighborhoods, where energy from newborn stars sculpts fantasy-like landscapes in the gas. The tower is a giant incubator for these newborn stars. A torrent of ultraviolet light from a band of massive, hot, young stars [off the top of the image] is eroding the pillar. The ...
Low Mass
... become electron degenerate – force of electrons around atoms keeps from collapse (no energy is produced). This force originates from the Pauli Exclusion Principle – core temperature never reaches the 600 million K required to burn carbon or oxygen, so core fusion ends. ...
... become electron degenerate – force of electrons around atoms keeps from collapse (no energy is produced). This force originates from the Pauli Exclusion Principle – core temperature never reaches the 600 million K required to burn carbon or oxygen, so core fusion ends. ...
Student Worksheet - Indiana University Astronomy
... young star cluster near its center. The dust lanes appear dark because they obscure visible light, and are thus seen in silhouette against the brighter, glowing, hydrogen gas. Surrounding the red nebula is a blue reflection nebula, especially bright at northern end. The reflection nebula glows by re ...
... young star cluster near its center. The dust lanes appear dark because they obscure visible light, and are thus seen in silhouette against the brighter, glowing, hydrogen gas. Surrounding the red nebula is a blue reflection nebula, especially bright at northern end. The reflection nebula glows by re ...
Supernova - Mid-Pacific Institute
... A white dwarf cannot be more massive than about 1.4 solar masses and remain stable. if the white dwarf's companion star expands to become a red giant, some of its matter may be drawn away and sucked onto the surface of the white dwarf. ...
... A white dwarf cannot be more massive than about 1.4 solar masses and remain stable. if the white dwarf's companion star expands to become a red giant, some of its matter may be drawn away and sucked onto the surface of the white dwarf. ...
Handout from Allaire Star Party
... called a red giant (such as the bright star Arcturus). Then it puffs off its outer layers, leaving a glowing remnant called a white dwarf, which is only the size of the Earth but can contain more mass the Sun. Because of this, white dwarves are very dense; a basketball made of white dwarf material w ...
... called a red giant (such as the bright star Arcturus). Then it puffs off its outer layers, leaving a glowing remnant called a white dwarf, which is only the size of the Earth but can contain more mass the Sun. Because of this, white dwarves are very dense; a basketball made of white dwarf material w ...
Constants and Equations
... a) AM CVn stars are binary systems with an orbital period of less than 65 minutes. b) AM CVn stars may produce a type II supernova after the white dwarf reaches a critical mass. c) AM CVn stars are sources of gravitational waves. d) AM CVn stars are binary systems where a white dwarf accretes mass f ...
... a) AM CVn stars are binary systems with an orbital period of less than 65 minutes. b) AM CVn stars may produce a type II supernova after the white dwarf reaches a critical mass. c) AM CVn stars are sources of gravitational waves. d) AM CVn stars are binary systems where a white dwarf accretes mass f ...
Activity 1 - Mathematical and Scientific Methods
... 1. Theoretically, what is a pulsar? A rapidly spinning neutron star beaming synchrotron radiation towards Earth. 2. Observationally, what is a pulsar? An object whose radiation varies extremely rapidly. 3. What are the characteristics of a neutron star ? Extremely dense, R~10 km, supported by neutro ...
... 1. Theoretically, what is a pulsar? A rapidly spinning neutron star beaming synchrotron radiation towards Earth. 2. Observationally, what is a pulsar? An object whose radiation varies extremely rapidly. 3. What are the characteristics of a neutron star ? Extremely dense, R~10 km, supported by neutro ...
Background Science - Faulkes Telescope Project
... the X-ray, we are looking at the parts of the shell that are much hotter than the areas shining in the optical. The X-rays come from the extremely hot material at around 10 million degrees Kelvin. These high energy rays are emitted from the chemical elements in the gas, for example, from silicon, ir ...
... the X-ray, we are looking at the parts of the shell that are much hotter than the areas shining in the optical. The X-rays come from the extremely hot material at around 10 million degrees Kelvin. These high energy rays are emitted from the chemical elements in the gas, for example, from silicon, ir ...
January 2006
... • nuclei and electrons are crushed together • protons combine with electrons to form neutrons • Ultimately the collapse is halted by neutron pressure – Most of the core is composed of neutrons at this point ...
... • nuclei and electrons are crushed together • protons combine with electrons to form neutrons • Ultimately the collapse is halted by neutron pressure – Most of the core is composed of neutrons at this point ...
Supernovae - Michigan State University
... Shock wave hits inner ring of material and creates intense X-ray radiation ...
... Shock wave hits inner ring of material and creates intense X-ray radiation ...
TAURUS ZODIAC CONSTELLATION In Greek mythology, Taurus
... themselves are represented by large, bright stars; there are also many small The constellation Taurus as it can be brown dwarfs and white dwarfs. The cluster is estimated to dissipate in another seen by the naked eye. The 250 million years. constellation lines have been added In the northern part of ...
... themselves are represented by large, bright stars; there are also many small The constellation Taurus as it can be brown dwarfs and white dwarfs. The cluster is estimated to dissipate in another seen by the naked eye. The 250 million years. constellation lines have been added In the northern part of ...
Stellar Evolution: the Death of Stars
... • Electron combines with proton to form neutrons • During the combining process, it produces neutrinos that carry energy away • The core ends up as all neutron, with nuclear density (1017 km/m3) • The degenerate neutron pressure suddenly halts the core contract • The outer core bounce back and sends ...
... • Electron combines with proton to form neutrons • During the combining process, it produces neutrinos that carry energy away • The core ends up as all neutron, with nuclear density (1017 km/m3) • The degenerate neutron pressure suddenly halts the core contract • The outer core bounce back and sends ...
Crab Nebula
The Crab Nebula (catalogue designations M1, NGC 1952, Taurus A) is a supernova remnant and pulsar wind nebula in the constellation of Taurus. It is not, as its name might suggest, in Cancer. The now-current name is due to William Parsons, 3rd Earl of Rosse, who observed the object in 1840 using a 36-inch telescope and produced a drawing that looked somewhat like a crab. Corresponding to a bright supernova recorded by Chinese astronomers in 1054, the nebula was observed later by English astronomer John Bevis in 1731. The nebula was the first astronomical object identified with a historical supernova explosion.At an apparent magnitude of 8.4, comparable to that of Saturn's moon Titan, it is not visible to the naked eye but can be made out using binoculars under favourable conditions. The nebula lies in the Perseus Arm of the Milky Way galaxy, at a distance of about 2.0 kiloparsecs (6,500 ly) from Earth. It has a diameter of 3.4 parsecs (11 ly), corresponding to an apparent diameter of some 7 arcminutes, and is expanding at a rate of about 1,500 kilometres per second (930 mi/s), or 0.5% c.At the center of the nebula lies the Crab Pulsar, a neutron star 28–30 kilometres (17–19 mi) across with a spin rate of 30.2 times per second, which emits pulses of radiation from gamma rays to radio waves. At X-ray and gamma ray energies above 30 keV, the Crab is generally the strongest persistent source in the sky, with measured flux extending to above 10 TeV. The nebula's radiation allows for the detailed studying of celestial bodies that occult it. In the 1950s and 1960s, the Sun's corona was mapped from observations of the Crab's radio waves passing through it, and in 2003, the thickness of the atmosphere of Saturn's moon Titan was measured as it blocked out X-rays from the nebula.