The Family of Stars
... shell around the core. He core + H-burning shell produce more energy than needed for pressure support Expansion and cooling of the outer layers of the star ...
... shell around the core. He core + H-burning shell produce more energy than needed for pressure support Expansion and cooling of the outer layers of the star ...
Unit 1
... – Radiation carries away energy in regions where the photons are not readily absorbed by stellar gas – Close to the cores of massive stars, there is enough material to impede the flow of energy through radiation ...
... – Radiation carries away energy in regions where the photons are not readily absorbed by stellar gas – Close to the cores of massive stars, there is enough material to impede the flow of energy through radiation ...
PS 224, Fall 2014 HW 4
... e: Pre-main-sequence star: Between 3–50 million years after birth, the star has formed planets. It is still contracting.While most of the disk has dissipated, a small debris disk remains. f: Young stellar systems: After 50 million years, the star is burning hydrogen and is settling into its adult li ...
... e: Pre-main-sequence star: Between 3–50 million years after birth, the star has formed planets. It is still contracting.While most of the disk has dissipated, a small debris disk remains. f: Young stellar systems: After 50 million years, the star is burning hydrogen and is settling into its adult li ...
Stars - MrCrabtreesScience
... If remaining core is >3 times the mass of the sun it forms a Black Hole • All the matter is squeezed into a space smaller ...
... If remaining core is >3 times the mass of the sun it forms a Black Hole • All the matter is squeezed into a space smaller ...
Class II Supernova
... •Class II can be divided, because of their emission spectra •Unlike a Type I supernova, the mass and brightness can vary •Type 2P has a Very wide wavelength, •A type PL has a somewhat small wavelength, •A rare Type 2N has an extremely narrow wavelength, (thus the “n”) ...
... •Class II can be divided, because of their emission spectra •Unlike a Type I supernova, the mass and brightness can vary •Type 2P has a Very wide wavelength, •A type PL has a somewhat small wavelength, •A rare Type 2N has an extremely narrow wavelength, (thus the “n”) ...
dtu7ech13 - Fort Thomas Independent Schools
... Will the Sun someday cease to exist? If so, how? The Sun will shed matter as a planetary nebula in about 6 billion years and then cease nuclear fusion. Its remnant white dwarf will dim over the succeeding billions of years. What is a nova? A nova is a relatively gentle explosion of hydrogen gas on t ...
... Will the Sun someday cease to exist? If so, how? The Sun will shed matter as a planetary nebula in about 6 billion years and then cease nuclear fusion. Its remnant white dwarf will dim over the succeeding billions of years. What is a nova? A nova is a relatively gentle explosion of hydrogen gas on t ...
I have heard people call Jupiter a "failed star" that just did not get big
... of rotation, these clouds form flattened disks that surround the central, growing stars. After the star has nearly reached its final mass, by accreting gas from the disk, the leftover matter in the disk is free to form planets. "Jupiter is generally believed to have formed in a two-step process. Fir ...
... of rotation, these clouds form flattened disks that surround the central, growing stars. After the star has nearly reached its final mass, by accreting gas from the disk, the leftover matter in the disk is free to form planets. "Jupiter is generally believed to have formed in a two-step process. Fir ...
Quiz #4 – The Electromagnetic Spectrum and Stars
... The ___________________ will determine the evolutionary course a star will take. ...
... The ___________________ will determine the evolutionary course a star will take. ...
Chapter 2 Cosmic tombstones
... Since the magnetic axis and the rotation axis are not aligned, the pulsar operates like a lighthouse an observer sees periodic pulses of radio emission According to the leading theory, this emission is produced by fast particles propagating along the magnetic field lines Particles are extracted fr ...
... Since the magnetic axis and the rotation axis are not aligned, the pulsar operates like a lighthouse an observer sees periodic pulses of radio emission According to the leading theory, this emission is produced by fast particles propagating along the magnetic field lines Particles are extracted fr ...
Star Formation
... *Luminosity is how much energy the star emits *Absolute Magnitude is how bright the star would be if it was 10 parsecs away *B-V is a color metric, the difference in magnitude between the blue astronomical filter and the visible light filter *see The Brightness of Stars ppt. ...
... *Luminosity is how much energy the star emits *Absolute Magnitude is how bright the star would be if it was 10 parsecs away *B-V is a color metric, the difference in magnitude between the blue astronomical filter and the visible light filter *see The Brightness of Stars ppt. ...
Lecture 13
... cores are no longer on the main sequence. • They may be fusing He to Carbon in their core or fusing H to He in shell outside the core … but there is no H to He fusion in the core. • All stars become larger and redder after exhausting their core hydrogen fuel: giants and supergiants. • Most stars end ...
... cores are no longer on the main sequence. • They may be fusing He to Carbon in their core or fusing H to He in shell outside the core … but there is no H to He fusion in the core. • All stars become larger and redder after exhausting their core hydrogen fuel: giants and supergiants. • Most stars end ...
History of the Universe and Solar System
... Main sequence: hydrogen burns (nuclear fusion) to form helium Red Giant: helium burns (nuclear fusion) to form carbon, carbon burns to form oxygen, oxygen burns to form iron. All elements lighter than and including iron (56) formed this way. ...
... Main sequence: hydrogen burns (nuclear fusion) to form helium Red Giant: helium burns (nuclear fusion) to form carbon, carbon burns to form oxygen, oxygen burns to form iron. All elements lighter than and including iron (56) formed this way. ...
Instructor Notes
... an asymptotic giant branch (AGB) star when the helium in the core is exhausted and shell helium fusion begins ...
... an asymptotic giant branch (AGB) star when the helium in the core is exhausted and shell helium fusion begins ...
30.2 PowerPoint Stellar Evolution
... The nebula begins to contract and gravitational attraction increases It continues shrinking and starts to spin. Eventually it forms a flat disk with a PROTOSTAR in the middle ...
... The nebula begins to contract and gravitational attraction increases It continues shrinking and starts to spin. Eventually it forms a flat disk with a PROTOSTAR in the middle ...
Star Classification
... 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 ...
Name
... 13. Star A has an apparent magnitude of .15 and is 1600 lya. Star B has an apparent magnitude of .86 and is 14 lya. If Star B is a white giant, what might be true about Star A? Star ...
... 13. Star A has an apparent magnitude of .15 and is 1600 lya. Star B has an apparent magnitude of .86 and is 14 lya. If Star B is a white giant, what might be true about Star A? Star ...
BIO 10 Lecture 2
... • They might have had gaseous planets like our own outer planets (Jupiter, Saturn, Uranus, and Neptune) ...
... • They might have had gaseous planets like our own outer planets (Jupiter, Saturn, Uranus, and Neptune) ...
Consequences of Neutrino Emission from a Phase
... In our study we did not consider the detail formation process from normal matter to quark matter. We simply assume that a neutron star suddenly undergoes a phase-transition. We use a 3D Newtonian hydrodynamic code to study the consequences of phase-transitioninduced collapse. This code solves a set ...
... In our study we did not consider the detail formation process from normal matter to quark matter. We simply assume that a neutron star suddenly undergoes a phase-transition. We use a 3D Newtonian hydrodynamic code to study the consequences of phase-transitioninduced collapse. This code solves a set ...
Sample exam 2
... sentence/paragraph format or a drawing, depending on what is asked. 11. The Sun started off its trajectory on the Hertzsprung-Russell diagram by initially moving down and to the left as it organized into a protostar. Explain this behavior in terms of temperature and luminosity, and give a reason for ...
... sentence/paragraph format or a drawing, depending on what is asked. 11. The Sun started off its trajectory on the Hertzsprung-Russell diagram by initially moving down and to the left as it organized into a protostar. Explain this behavior in terms of temperature and luminosity, and give a reason for ...
The Life Cycle of a Star Webquest:
... 3. How long can a star stay a protostar? ____________________________ 4. Explain nuclear fusion. ____________________________________________________________ ______________________________________________________________________________________ 5. How long does a star live before it begins to die? _ ...
... 3. How long can a star stay a protostar? ____________________________ 4. Explain nuclear fusion. ____________________________________________________________ ______________________________________________________________________________________ 5. How long does a star live before it begins to die? _ ...
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.