Stars part 1
... 2. Luminosity – the total amount of energy a star radiates each second. Luminosity of all visible stars range from 1/1,000,000 the luminosity of the sun to 1,000,000 time the luminosity of the sun. 90% of the stars are not as bright as the sun. ...
... 2. Luminosity – the total amount of energy a star radiates each second. Luminosity of all visible stars range from 1/1,000,000 the luminosity of the sun to 1,000,000 time the luminosity of the sun. 90% of the stars are not as bright as the sun. ...
Stellar Evolution of a Star like the Sun
... central core. The central temperature need to be hotter and hotter each time a new nuclear fuel is used. Burning H to He requires tens of millions of degrees Kelvin. Burning Helium requires a higher temperature because the repulsion between the He-nuclei is larger (twice as much) than that of the Hn ...
... central core. The central temperature need to be hotter and hotter each time a new nuclear fuel is used. Burning H to He requires tens of millions of degrees Kelvin. Burning Helium requires a higher temperature because the repulsion between the He-nuclei is larger (twice as much) than that of the Hn ...
Thermal Equilibrium
... central core. The central temperature need to be hotter and hotter each time a new nuclear fuel is used. Burning H to He requires tens of millions of degrees Kelvin. Burning Helium requires a higher temperature because the repulsion between the He-nuclei is larger (twice as much) than that of the Hn ...
... central core. The central temperature need to be hotter and hotter each time a new nuclear fuel is used. Burning H to He requires tens of millions of degrees Kelvin. Burning Helium requires a higher temperature because the repulsion between the He-nuclei is larger (twice as much) than that of the Hn ...
Lecture 13 - Star Formation
... • The interstellar medium (ISM) consists of gas and dust. • Gas is mainly hydrogen, but also contains other elements and molecules. • Density is typically around 1 atom per cubic centimeter. ...
... • The interstellar medium (ISM) consists of gas and dust. • Gas is mainly hydrogen, but also contains other elements and molecules. • Density is typically around 1 atom per cubic centimeter. ...
Galaxies - Indiana University Astronomy
... exploding white dwarfs, and Type II supernovae, which are explosions of massive stars that run out of nuclear fuel. The light curves of supernovae of Type Ia and Type II are compared in the figure below. Type Ia supernova rise to maximum and then fall steadily in brightness, fading in just a few wee ...
... exploding white dwarfs, and Type II supernovae, which are explosions of massive stars that run out of nuclear fuel. The light curves of supernovae of Type Ia and Type II are compared in the figure below. Type Ia supernova rise to maximum and then fall steadily in brightness, fading in just a few wee ...
Luminosity
... In binary stars, the orbital period depends on the masses of the stars and the sizes of the orbits. Why is this so valuable to know? 1. We can predict how long an orbit will take 2. This is the main way we determine the masses of stars 3. This lets us know if two stars that look close together in t ...
... In binary stars, the orbital period depends on the masses of the stars and the sizes of the orbits. Why is this so valuable to know? 1. We can predict how long an orbit will take 2. This is the main way we determine the masses of stars 3. This lets us know if two stars that look close together in t ...
91KB - NZQA
... • blue / white giant • supernova • black hole. The birth stage is explained: A very large GMC condenses under gravity to become dense. As it condenses, the particles become hotter (due to friction) and eventually become hot enough to become a protostar. Rigel birth explained with associated energy c ...
... • blue / white giant • supernova • black hole. The birth stage is explained: A very large GMC condenses under gravity to become dense. As it condenses, the particles become hotter (due to friction) and eventually become hot enough to become a protostar. Rigel birth explained with associated energy c ...
145KB - NZQA
... • blue / white giant • supernova • black hole. The birth stage is explained: A very large GMC condenses under gravity to become dense. As it condenses, the particles become hotter (due to friction) and eventually become hot enough to become a protostar. Rigel birth explained with associated energy c ...
... • blue / white giant • supernova • black hole. The birth stage is explained: A very large GMC condenses under gravity to become dense. As it condenses, the particles become hotter (due to friction) and eventually become hot enough to become a protostar. Rigel birth explained with associated energy c ...
Life Cycle of Stars
... Facts: Protostar: a large mass that forms by contraction out of the gas of a giant molecular cloud. The energy source of Protostars is gravitational contraction (as opposed to hydrogen burning in main-sequence stars). Accretion: Growth of massive objects by gravitationally attracting more matter, ty ...
... Facts: Protostar: a large mass that forms by contraction out of the gas of a giant molecular cloud. The energy source of Protostars is gravitational contraction (as opposed to hydrogen burning in main-sequence stars). Accretion: Growth of massive objects by gravitationally attracting more matter, ty ...
Name - CLC Charter School
... different kind of star left. This star is called a spinning neutron star. Neutron stars produce radio waves in a steady stream or in random bursts. But if a star is massive enough, it can leave behind something more. For this to happen though, the star must be at least I0 times the size of the sun. ...
... different kind of star left. This star is called a spinning neutron star. Neutron stars produce radio waves in a steady stream or in random bursts. But if a star is massive enough, it can leave behind something more. For this to happen though, the star must be at least I0 times the size of the sun. ...
File
... of hot gas with atomic nuclei and electrons whizzing around. • Nuclei collide and sometimes they “stick” together to form a heavier nucleus (and heavier element). • Fusion- the process by which two atomic nuclei fuse together ...
... of hot gas with atomic nuclei and electrons whizzing around. • Nuclei collide and sometimes they “stick” together to form a heavier nucleus (and heavier element). • Fusion- the process by which two atomic nuclei fuse together ...
What are the Spectral Lines? - University of Texas Astronomy Home
... - real knowledge only due to hard facts, e.g., laboratory science, measurements • claimed ...
... - real knowledge only due to hard facts, e.g., laboratory science, measurements • claimed ...
Searching for Dwarf Galaxies and Population III Star
... at early times are volumes that have been ionized by flux from nearby, bright galaxies or proto-clusters of galaxies. This project is a search for tiny, star-forming dwarf galaxies in regions around very luminous star-forming galaxies at z~7.7 discovered by the James Webb Space Telescope. The projec ...
... at early times are volumes that have been ionized by flux from nearby, bright galaxies or proto-clusters of galaxies. This project is a search for tiny, star-forming dwarf galaxies in regions around very luminous star-forming galaxies at z~7.7 discovered by the James Webb Space Telescope. The projec ...
An introduce of the spectrograph of the GALEX
... assumptions and corrections that together affect the SFH normalization to test their accuracy, both in this redshift range and beyond. As lower limits on this normalization, we consider the evolution in stellar and metal mass densities, and supernova rate density, finding it unlikely that the SFH no ...
... assumptions and corrections that together affect the SFH normalization to test their accuracy, both in this redshift range and beyond. As lower limits on this normalization, we consider the evolution in stellar and metal mass densities, and supernova rate density, finding it unlikely that the SFH no ...
Astronomy Exam #2 for the 10
... luminosity of between 16 and 10,000 solar luminosities. These stars will have a short main sequence lifetime compared to the Sun’s lifetime. Some as short as a few million years. The giant stars appear to be mostly G and K spectral types with luminosities over 100 solar luminosities. These giant sta ...
... luminosity of between 16 and 10,000 solar luminosities. These stars will have a short main sequence lifetime compared to the Sun’s lifetime. Some as short as a few million years. The giant stars appear to be mostly G and K spectral types with luminosities over 100 solar luminosities. These giant sta ...
UNIVERSITY OF BRISTOL
... appropriate? How does the Sersic profile differ from this? (b) (12 marks) The bulge and disc components of a certain galaxy are observed to have half light (effective) radii of 3 arcsec and 15 arcsec, and surface brightnesses at these radii of 22 and 23 B magnitudes per square arcsec, respectively. ...
... appropriate? How does the Sersic profile differ from this? (b) (12 marks) The bulge and disc components of a certain galaxy are observed to have half light (effective) radii of 3 arcsec and 15 arcsec, and surface brightnesses at these radii of 22 and 23 B magnitudes per square arcsec, respectively. ...
Evolution of a Star
... Once the red giant’s core uses its supply of helium, it contracts even more. As the core runs out of fuel, the outer layers escape into space. This leaves behind the hot dense core. The core contracts under the force of gravity. At this stage in a star’s evolution, it is a white dwarf. A white dwarf ...
... Once the red giant’s core uses its supply of helium, it contracts even more. As the core runs out of fuel, the outer layers escape into space. This leaves behind the hot dense core. The core contracts under the force of gravity. At this stage in a star’s evolution, it is a white dwarf. A white dwarf ...
The Cosmic Microwave Background
... density Ωbh2 make the first acoustic peak much larger than the second. The more baryons the more the second peak is relatively suppressed. Baryons constitute about 5% of the critical density today, in agreement with the number derived from studies of light element synthesis in the infant universe. A ...
... density Ωbh2 make the first acoustic peak much larger than the second. The more baryons the more the second peak is relatively suppressed. Baryons constitute about 5% of the critical density today, in agreement with the number derived from studies of light element synthesis in the infant universe. A ...
Stars and Light
... C) Electrons can jump between energy levels in an atom only if they receive or give up an amount of energy equal to the difference in energy between the energy levels. D) An electron has a negative electrical charge. E) Electrons have very little mass compared to protons or neutrons. ...
... C) Electrons can jump between energy levels in an atom only if they receive or give up an amount of energy equal to the difference in energy between the energy levels. D) An electron has a negative electrical charge. E) Electrons have very little mass compared to protons or neutrons. ...
The Vital Force: Proton Power and the Origins of Life An Introduction
... energy that the sun every second. This sounds improbable, to put it mildly, so let’s consider the numbers. The sun’s luminosity is about 4 x 1026 watts and its total mass is 2 x 1030 kg. Over its projected lifetime, about 10 billion years, each gram of solar material will produce about 60 million ki ...
... energy that the sun every second. This sounds improbable, to put it mildly, so let’s consider the numbers. The sun’s luminosity is about 4 x 1026 watts and its total mass is 2 x 1030 kg. Over its projected lifetime, about 10 billion years, each gram of solar material will produce about 60 million ki ...
Radial Stellar Pulsations
... produced by nuclear reactions. In equilibrium, heat production in the core is exactly balanced by heat loss from the surface, i.e., by the stellar luminosity. Stellar pulsation disturbs this balance by (i) modulating the nuclear reaction rate in the core (epsilon mechanism); and more importantly, (i ...
... produced by nuclear reactions. In equilibrium, heat production in the core is exactly balanced by heat loss from the surface, i.e., by the stellar luminosity. Stellar pulsation disturbs this balance by (i) modulating the nuclear reaction rate in the core (epsilon mechanism); and more importantly, (i ...