Astronomy Study Guide #2
... 05. What two parameters does the brightness of a star depend on? 06. What is the stellar spectral classification sequence? 07. What do studies of binary stars help us learn? 08. Solar granulation is evidence for what aspect of energy transport? 09. In traveling from the center of the sun to the top ...
... 05. What two parameters does the brightness of a star depend on? 06. What is the stellar spectral classification sequence? 07. What do studies of binary stars help us learn? 08. Solar granulation is evidence for what aspect of energy transport? 09. In traveling from the center of the sun to the top ...
Intro Lecture: Stars - University of Redlands
... Mizar, 88 light years distant, is the middle star in the handle of the Big Dipper. It was the first binary star system to be imaged with a telescope. Spectroscopic observations show periodic Doppler shifts in the spectra of Mizar A and B, indicating that they are each binary stars. But they were too ...
... Mizar, 88 light years distant, is the middle star in the handle of the Big Dipper. It was the first binary star system to be imaged with a telescope. Spectroscopic observations show periodic Doppler shifts in the spectra of Mizar A and B, indicating that they are each binary stars. But they were too ...
PH507 - University of Kent
... 1. Calculate the luminosity (in units of the solar luminosity) of a blackbody of Saturn’s radius that has a temperature of 1000 K? Explain the steps you take in the derivation. The surface temperature of the Sun is 5780 K. The radii of Saturn and the Sun are 6.00 x 107 m and 6.96 x 108 m, respective ...
... 1. Calculate the luminosity (in units of the solar luminosity) of a blackbody of Saturn’s radius that has a temperature of 1000 K? Explain the steps you take in the derivation. The surface temperature of the Sun is 5780 K. The radii of Saturn and the Sun are 6.00 x 107 m and 6.96 x 108 m, respective ...
matthewchristianstarprodject
... hydrogen atoms into helium. During this stage of the star's lifetime, it is determined by its mass, but also based upon its chemical composition and other factors. All main sequence stars are in hydrostatic equilibrium, where outward thermal pressure from the core is balanced by the inward gravita ...
... hydrogen atoms into helium. During this stage of the star's lifetime, it is determined by its mass, but also based upon its chemical composition and other factors. All main sequence stars are in hydrostatic equilibrium, where outward thermal pressure from the core is balanced by the inward gravita ...
The Hidden Lives of Galaxies NSTA 2001
... How does the sun produce energy? How is fusion different from bonding? Do small stars or large stars burn faster? Do small stars or large stars burn hotter? When does fusion stop in a red ...
... How does the sun produce energy? How is fusion different from bonding? Do small stars or large stars burn faster? Do small stars or large stars burn hotter? When does fusion stop in a red ...
Stars Part Two
... How do we know all this? By observing Globular clusters… 1. Globular clusters are thousands of stars that all formed at more or less the same time. 2. Globular clusters are much smaller than galaxies. 3. Galaxies create stars in an on-going process. 4. The stars in a globular cluster accrete sudde ...
... How do we know all this? By observing Globular clusters… 1. Globular clusters are thousands of stars that all formed at more or less the same time. 2. Globular clusters are much smaller than galaxies. 3. Galaxies create stars in an on-going process. 4. The stars in a globular cluster accrete sudde ...
Due Date: Thursday, November 16, 2006
... fusion will last for about a million years, and the Sun will just very slowly contract. So, we will not see changes on the surface until a million years later. However, we should be able to tell that the hydrogen fusion in the core has stopped by observing the solar neutrinos. The neutrinos do not i ...
... fusion will last for about a million years, and the Sun will just very slowly contract. So, we will not see changes on the surface until a million years later. However, we should be able to tell that the hydrogen fusion in the core has stopped by observing the solar neutrinos. The neutrinos do not i ...
Astrophysics
... By examining the temperature and spectra of nearby stars, astrophysicists found that there were other indicators of temperature Certain spectral lines appeared consistently at certain temperatures and disappeared at others Different lines appear with different degrees of ionisation – which results f ...
... By examining the temperature and spectra of nearby stars, astrophysicists found that there were other indicators of temperature Certain spectral lines appeared consistently at certain temperatures and disappeared at others Different lines appear with different degrees of ionisation – which results f ...
Life Cycle of a Star
... • Once stars are formed they enter the main sequence stage. In this stage they continuously generate energy in the core through nuclear fusion. • Size, structure and composition change very little during this stage. ...
... • Once stars are formed they enter the main sequence stage. In this stage they continuously generate energy in the core through nuclear fusion. • Size, structure and composition change very little during this stage. ...
Slide 1
... 1. A cold cloud of gas and dust starts to contract, pulled together by gravity. It breaks up into several smaller clouds and each continues to contract. 2. Within a contracting cloud, each particle attracts every other particle, so that the cloud collapses towards its centre. It forms a rotating swi ...
... 1. A cold cloud of gas and dust starts to contract, pulled together by gravity. It breaks up into several smaller clouds and each continues to contract. 2. Within a contracting cloud, each particle attracts every other particle, so that the cloud collapses towards its centre. It forms a rotating swi ...
Stars, Galaxies, and the Universe
... Most stars do not exist alone Stars are held together by the force of gravity between them Binary system has 2 stars Multiple system has more than 2 stars ...
... Most stars do not exist alone Stars are held together by the force of gravity between them Binary system has 2 stars Multiple system has more than 2 stars ...
test - Scioly.org
... 14. What type of star is shown on the right side of this illustration? 15. What is the name of the material spiraling around and into the left hand star? 16. Expressed in solar masses, a type 1a supernova will occur when the left hand star reaches what mass? 17. Expressed in kg, and in scientific no ...
... 14. What type of star is shown on the right side of this illustration? 15. What is the name of the material spiraling around and into the left hand star? 16. Expressed in solar masses, a type 1a supernova will occur when the left hand star reaches what mass? 17. Expressed in kg, and in scientific no ...
Stars
... 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 univ ...
... 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 univ ...
The Sizes of Stars
... z Lower temperature means lower gas pressure z The lower gas pressure cannot hold up against gravity – the Sun shrinks z The added compression puts the Sun’s center under greater pressure, so the central temperature increases z The higher temperature produces higher pressure, which fights off gravit ...
... z Lower temperature means lower gas pressure z The lower gas pressure cannot hold up against gravity – the Sun shrinks z The added compression puts the Sun’s center under greater pressure, so the central temperature increases z The higher temperature produces higher pressure, which fights off gravit ...
ASTR-1020 Exam 2 Review Questions
... these two stars are farther from Earth? (Remember that the parallax angle is inversely proportional to the distance.) 4. What is the moving cluster method? Which star cluster is the foundation of the distance indicator method of figuring out the distance to external galaxies? 5. What is the differen ...
... these two stars are farther from Earth? (Remember that the parallax angle is inversely proportional to the distance.) 4. What is the moving cluster method? Which star cluster is the foundation of the distance indicator method of figuring out the distance to external galaxies? 5. What is the differen ...
April 15th
... • Type Ia Supernovas are rich in elements such as carbon, oxygen, silicon, and iron • Magnetic fields in the expanding remnant can accelerate atomic nuclei to speed close to the speed of light, which are called cosmic rays ...
... • Type Ia Supernovas are rich in elements such as carbon, oxygen, silicon, and iron • Magnetic fields in the expanding remnant can accelerate atomic nuclei to speed close to the speed of light, which are called cosmic rays ...
Lecture 22 - Star Formation from Molecular Clouds
... • We understand the physics of these processes (at least partially) • We believe the Sun formed like this. • What characteristic of the solar system can we see that is an indicator of the processes of contraction, jet formation, accretion disk formation, etc? ...
... • We understand the physics of these processes (at least partially) • We believe the Sun formed like this. • What characteristic of the solar system can we see that is an indicator of the processes of contraction, jet formation, accretion disk formation, etc? ...
File - SMIC Physics
... Supergiants and Supernovas • Stars more than 8x massive than Sun → evolution occurs more quickly and more violently • Massive stars → core heats up to higher temps → heavier elements form by fusion (becoz higher temp is needed to fuse bigger elements. Eg : He → C needs higher temp) → star expands i ...
... Supergiants and Supernovas • Stars more than 8x massive than Sun → evolution occurs more quickly and more violently • Massive stars → core heats up to higher temps → heavier elements form by fusion (becoz higher temp is needed to fuse bigger elements. Eg : He → C needs higher temp) → star expands i ...
Lecture 9
... • The Sun generates energy by fusing hydrogen into helium. But, some stars shine by turning heavier elements (like helium) into even heavier elements (possibly oxygen, carbon). Do temperatures need to be higher or lower for the fusion of other elements to occur? Why? • Challenge: Estimate how much h ...
... • The Sun generates energy by fusing hydrogen into helium. But, some stars shine by turning heavier elements (like helium) into even heavier elements (possibly oxygen, carbon). Do temperatures need to be higher or lower for the fusion of other elements to occur? Why? • Challenge: Estimate how much h ...
Main Sequence Lifetime
... • As the degenerate core grows and the shellburning rate increases, the surrounding layers of the star are heated and expand • As the star’s surface expands it becomes more luminous but also cooler • The star becomes a subgiant - luminous but red in colour • The star moves above and to the right of ...
... • As the degenerate core grows and the shellburning rate increases, the surrounding layers of the star are heated and expand • As the star’s surface expands it becomes more luminous but also cooler • The star becomes a subgiant - luminous but red in colour • The star moves above and to the right of ...
Stars and The Universe
... the inner layers come from fusion of the elements in the Why does the “ash” that is created by fusion move to the outer layers. It all starts with center of the sun? hydrogen fusion… When atoms fuse, their product is a heavier, denser The fusion process continues material. Denser materials sink. unt ...
... the inner layers come from fusion of the elements in the Why does the “ash” that is created by fusion move to the outer layers. It all starts with center of the sun? hydrogen fusion… When atoms fuse, their product is a heavier, denser The fusion process continues material. Denser materials sink. unt ...
Astronomy
... exists today. Celestial object: something in space, such as a star or planet. Constellation: stars that appear to be grouped in patterns forming the outlines of people, animals, and physical objects in the sky. Doppler effect: the apparent change in wave frequency as an energy source moves toward or ...
... exists today. Celestial object: something in space, such as a star or planet. Constellation: stars that appear to be grouped in patterns forming the outlines of people, animals, and physical objects in the sky. Doppler effect: the apparent change in wave frequency as an energy source moves toward or ...
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.