Sun, Earth and Moon Model
... The strange new world was discovered orbiting a star in a triple star system. That means its parent star orbits alongside two other stars. This makes sunrises and sunsets something special — sometimes one sun rises in the sky, sometimes it’s two or three! But despite this, this planet is not entirel ...
... The strange new world was discovered orbiting a star in a triple star system. That means its parent star orbits alongside two other stars. This makes sunrises and sunsets something special — sometimes one sun rises in the sky, sometimes it’s two or three! But despite this, this planet is not entirel ...
The Sun and Other Stars - Tuslaw Local School District
... Life of a star • How long a star lives depends on its mass *small mass stars use up their fuel more slowly than large mass stars, so they have much longer lives • Medium mass stars like the sun live about 10 by • Small mass stars may live 200 by • A large mass star 15 x’s as massive as the sun may ...
... Life of a star • How long a star lives depends on its mass *small mass stars use up their fuel more slowly than large mass stars, so they have much longer lives • Medium mass stars like the sun live about 10 by • Small mass stars may live 200 by • A large mass star 15 x’s as massive as the sun may ...
Astroparticle physics 1. stellar astrophysics and solar neutrinos
... • Hertzsprung (1905): correlation between spectral type ( colour temperature) and absolute magnitudes ( luminosities). ...
... • Hertzsprung (1905): correlation between spectral type ( colour temperature) and absolute magnitudes ( luminosities). ...
planetary nebulae
... For a star of the Sun’s size, 5 million tonnes start to be converted into energy every second. The protostar detonates into a star. ...
... For a star of the Sun’s size, 5 million tonnes start to be converted into energy every second. The protostar detonates into a star. ...
Review Packet
... 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 ...
The Change in Gravitational Potential Energy of Objects
... objects near stars in stellar metamorphosis changes as the stars evolve. Explanation is provided. In stellar metamorphosis, exoplanets are evolved/evolving and dead stars. They have lost the majority of their mass, and their gravitational fields and radii have diminished considerably, as well as the ...
... objects near stars in stellar metamorphosis changes as the stars evolve. Explanation is provided. In stellar metamorphosis, exoplanets are evolved/evolving and dead stars. They have lost the majority of their mass, and their gravitational fields and radii have diminished considerably, as well as the ...
Review: How does a star`s mass determine its life story?
... less mass gains mass from its companion ...
... less mass gains mass from its companion ...
Life Cycle of Stars
... • The matter inside the star will be compressed so tightly that its atoms are compacted into a dense shell of neutrons. If the remaining mass of the star is more than about three times that of the Sun, it will collapse so completely that it will literally disappear from the universe. What is left be ...
... • The matter inside the star will be compressed so tightly that its atoms are compacted into a dense shell of neutrons. If the remaining mass of the star is more than about three times that of the Sun, it will collapse so completely that it will literally disappear from the universe. What is left be ...
ASTRONOMY: WHAT DO YOU NEED TO KNOW
... Energy flows outward from the outer layers as……………………….. convection What are the four laws of stellar structure? (p. 185) 1) Total mass = sum of the shell masses 2) Total luminosity = the sum of the energy generated in each shell 3) The weight on each layer is balanced by the pressure in the layer 4 ...
... Energy flows outward from the outer layers as……………………….. convection What are the four laws of stellar structure? (p. 185) 1) Total mass = sum of the shell masses 2) Total luminosity = the sum of the energy generated in each shell 3) The weight on each layer is balanced by the pressure in the layer 4 ...
Exploring the Universe
... a. Main sequence: A line or sequence in an H-R diagram where most stars spend 90% of their life. i. A diagonal band running from the bright, hot stars on the upper left to the dim, cool stars on the lower right ii. Example: The Sun lies in the main sequence ...
... a. Main sequence: A line or sequence in an H-R diagram where most stars spend 90% of their life. i. A diagonal band running from the bright, hot stars on the upper left to the dim, cool stars on the lower right ii. Example: The Sun lies in the main sequence ...
Handout Life of Stars
... inward pressure of its gravity (known as hydrostatic equilibrium). This is the period known as the main sequence of the star. Already about 4.5 - 5 billion years old, when the Sun’s hydrogen fuel starts to run out (in an estimated further 5 billion years or so), its main sequence comes to an end, an ...
... inward pressure of its gravity (known as hydrostatic equilibrium). This is the period known as the main sequence of the star. Already about 4.5 - 5 billion years old, when the Sun’s hydrogen fuel starts to run out (in an estimated further 5 billion years or so), its main sequence comes to an end, an ...
Time From the Perspective of a Particle Physicist
... • Usually leaves neutron star For high mass stars • fusion continues beyond C,O to Iron • if Mass(core) > 1.4 M(Sun) core collapses in SUPERNOVA (II) • leaves either Neutron Star or Black Hole • Most SN are this type PHYS 162 ...
... • Usually leaves neutron star For high mass stars • fusion continues beyond C,O to Iron • if Mass(core) > 1.4 M(Sun) core collapses in SUPERNOVA (II) • leaves either Neutron Star or Black Hole • Most SN are this type PHYS 162 ...
1. The distances to the most remote galaxies can be
... 27. A supernova is produced when: a) any star reaches the carbon fusion limit. b) the collapse of a star’s iron nucleus causes a shock wave that “blows off” the envelope of the star. c) an O and B main sequence star evolves explosively to the red supergiant stage. d) an intermediate mass star reache ...
... 27. A supernova is produced when: a) any star reaches the carbon fusion limit. b) the collapse of a star’s iron nucleus causes a shock wave that “blows off” the envelope of the star. c) an O and B main sequence star evolves explosively to the red supergiant stage. d) an intermediate mass star reache ...
Stellar Interiors - Hydrostatic Equilibrium and Ignition on the Main
... Solve for condition that ideal gas pressure and degeneracy pressure are equal at 107 K. ...
... Solve for condition that ideal gas pressure and degeneracy pressure are equal at 107 K. ...
Elemental Abundances
... odd:even and shell effects in nuclei which affect their binding energy. • From successive stages in stellar evolution: exhaustion of one fuel is followed by contraction, heating, alpha=He capture fusion. • Onset of Ca burning leads to Mg and nearby elements; accompanied by neutrino emission (ever fa ...
... odd:even and shell effects in nuclei which affect their binding energy. • From successive stages in stellar evolution: exhaustion of one fuel is followed by contraction, heating, alpha=He capture fusion. • Onset of Ca burning leads to Mg and nearby elements; accompanied by neutrino emission (ever fa ...
The Life Cycle of Stars Webquest
... Task #4: Types of Stars Continue to read on to the section “Types of Stars” on the same webpage http://www.seasky.org/cosmic/sky7a01.html and answer the following questions: 1. What does the main ...
... Task #4: Types of Stars Continue to read on to the section “Types of Stars” on the same webpage http://www.seasky.org/cosmic/sky7a01.html and answer the following questions: 1. What does the main ...
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.