Note Taking Guide #2: Characteristics of Stars Welcome back! As
... sun versus Alpha Centauri; the sun appears to give off much more light, even though the two stars are actually very similar in size and temperature. A star’s absolute magnitude is how much light a star would actually give off if it were a standard distance from Erath. Think of it this way: two simil ...
... sun versus Alpha Centauri; the sun appears to give off much more light, even though the two stars are actually very similar in size and temperature. A star’s absolute magnitude is how much light a star would actually give off if it were a standard distance from Erath. Think of it this way: two simil ...
Chapter 14
... wave that causes particles to move closer together into a growing cluster and as the mass increases the gravitational attraction of the particles for each other increases. • Eventually you end up with a protostar, an accumulation of gases that will form a star. ...
... wave that causes particles to move closer together into a growing cluster and as the mass increases the gravitational attraction of the particles for each other increases. • Eventually you end up with a protostar, an accumulation of gases that will form a star. ...
The Population of Stars
... • Most brown dwarfs are in even cooler spectral classes called L and T • Unlike true stars, brown dwarfs are too small to sustain thermonuclear fusion ...
... • Most brown dwarfs are in even cooler spectral classes called L and T • Unlike true stars, brown dwarfs are too small to sustain thermonuclear fusion ...
THE BIG BANG - Dublin City Schools
... • They use radioactive dating of uranium isotopes! • we know that the oldest isotopes were created (through nuclear reactions in supernovae) about 10 billion years ago. ...
... • They use radioactive dating of uranium isotopes! • we know that the oldest isotopes were created (through nuclear reactions in supernovae) about 10 billion years ago. ...
Slayt 1
... particles goes up and the protons get closer before repelling one another. If the proton get very close, the short-range nuclear force fuses them together. ...
... particles goes up and the protons get closer before repelling one another. If the proton get very close, the short-range nuclear force fuses them together. ...
What is a Red Shift?
... humans. Describe some situations where the sun helps us as humans, with our community, and our way of living. ...
... humans. Describe some situations where the sun helps us as humans, with our community, and our way of living. ...
Observational properties of stars
... So theoretically a high mass star goes straight and a low mass star gets curved over into the degenerate regions as they evolve. The temperature-density plot shows us some limits for masses such as 1. There is a lower limit for fusion to occur 2. Highest mass possible for a stable star. Any higher, ...
... So theoretically a high mass star goes straight and a low mass star gets curved over into the degenerate regions as they evolve. The temperature-density plot shows us some limits for masses such as 1. There is a lower limit for fusion to occur 2. Highest mass possible for a stable star. Any higher, ...
Starlight (conclusion)
... Types of stars, important terms Main Sequence Giants Supergiants White dwarfs What does it all mean? ...
... Types of stars, important terms Main Sequence Giants Supergiants White dwarfs What does it all mean? ...
Stellar and Atomic Spectra
... the orbits that the electron had before and after. • Because only certain energies are allowed for the electron orbits, only certain energies of photons can be produced. We call these the spectral lines. ...
... the orbits that the electron had before and after. • Because only certain energies are allowed for the electron orbits, only certain energies of photons can be produced. We call these the spectral lines. ...
M WHITE DWAR F The WhiTe-hoT Core
... pairs of stars orbiting each other, are fairly common. As many as half the stars in the Milky Way might be binary stars! ...
... pairs of stars orbiting each other, are fairly common. As many as half the stars in the Milky Way might be binary stars! ...
Timescales of stellar evolution 1. Dynamical time scale Measure of
... Virial theorem: the thermal energy U is roughly equal to the gravitational potential energy ...
... Virial theorem: the thermal energy U is roughly equal to the gravitational potential energy ...
Characteristics of stars powerpoint
... Distances to the Stars: •Distances are so large that kilometers are not very practical •Instead astronomers use a unit called a light-year ...
... Distances to the Stars: •Distances are so large that kilometers are not very practical •Instead astronomers use a unit called a light-year ...
8.3 Stars
... diagram (pg. 704)! Draw your own HR Diagram using the chart on page 704 as an example!! You have 20 minutes…work smart! ...
... diagram (pg. 704)! Draw your own HR Diagram using the chart on page 704 as an example!! You have 20 minutes…work smart! ...
I`m using this stupid huge font
... Generation of energy via Hawking radiation Every galaxy contributes one supermassive and about one million stellar black holes Black hole lifetime is mass dependent: One solar mass: Million solar mass: Galactic mass: Horizon mass: ...
... Generation of energy via Hawking radiation Every galaxy contributes one supermassive and about one million stellar black holes Black hole lifetime is mass dependent: One solar mass: Million solar mass: Galactic mass: Horizon mass: ...
www.astro.utu.fi
... stars burn H to He, He to heavier elements stars like the Sun are now middle aged low mass stars will burn for much longer, 1013 years about half of all stars are “low mass” stars ...
... stars burn H to He, He to heavier elements stars like the Sun are now middle aged low mass stars will burn for much longer, 1013 years about half of all stars are “low mass” stars ...
GEARS Workshop Monday - Georgia Southern University
... camera radius (from geometry and knowing distance) to get temperature of the sun as blackbody • We used Wien’s Law model for peak wavelength of blackbody emitter using the temperature ...
... camera radius (from geometry and knowing distance) to get temperature of the sun as blackbody • We used Wien’s Law model for peak wavelength of blackbody emitter using the temperature ...
Test 3 Review
... • Get plenty of rest the night before • Bring at least 2 pencils, UNM student ID, and a calculator 2) During the Test: • Write out and bubble your last name, space, first name and Exam color in the name space of the scantron form. Write out and bubble your Banner ID in the ID space. • Draw simple sk ...
... • Get plenty of rest the night before • Bring at least 2 pencils, UNM student ID, and a calculator 2) During the Test: • Write out and bubble your last name, space, first name and Exam color in the name space of the scantron form. Write out and bubble your Banner ID in the ID space. • Draw simple sk ...
WHERE DO WE SEARCH FOR LIFE IN THE UNIVERSE?
... Elimination of Low Mass Stars If we eliminate all stars that have a luminosity that is less than 1% of the Sun’s, then we eliminate nearly 75% of all stars in the Milky Way! ...
... Elimination of Low Mass Stars If we eliminate all stars that have a luminosity that is less than 1% of the Sun’s, then we eliminate nearly 75% of all stars in the Milky Way! ...
Lecture 5
... • Main sequence stars are same as Sun>thermonuclear reactions • Greater the Mass, greater the pressure and temperature at the Core->FASTER thermonuclear reaction->more LUMINOUS • Models of Main-Sequence Stars: for the stars to maintain equilibrium, more massive->larger radius, higher surface T (look ...
... • Main sequence stars are same as Sun>thermonuclear reactions • Greater the Mass, greater the pressure and temperature at the Core->FASTER thermonuclear reaction->more LUMINOUS • Models of Main-Sequence Stars: for the stars to maintain equilibrium, more massive->larger radius, higher surface T (look ...
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.