LAB: Star Classification
... KPD 0005+5106. The team who present these observations show that this white dwarf is among the hottest stars known so far, with a temperature of 200,000º K at its surface. Stars of intermediate mass (1-8 solar masses) terminate their life as an Earth-sized white dwarf after the exhaustion of their n ...
... KPD 0005+5106. The team who present these observations show that this white dwarf is among the hottest stars known so far, with a temperature of 200,000º K at its surface. Stars of intermediate mass (1-8 solar masses) terminate their life as an Earth-sized white dwarf after the exhaustion of their n ...
SAMPLE THIRD MIDTERM
... 35. Stars A and B have the same luminosity. If star B is 5 times farther from you than star A, how much dimmer will star B appear to you? a) 25 times dimmer b) 5 times dimmer c) 5 times dimmer d) it will appear the same as star A ...
... 35. Stars A and B have the same luminosity. If star B is 5 times farther from you than star A, how much dimmer will star B appear to you? a) 25 times dimmer b) 5 times dimmer c) 5 times dimmer d) it will appear the same as star A ...
main-sequence stars
... more luminous and have diameters from 10-100 times greater than our sun. Super giants are giant stars that have diameters more than 100 times greater than our sun. These giant stars (but relatively cool) are very luminous. ...
... more luminous and have diameters from 10-100 times greater than our sun. Super giants are giant stars that have diameters more than 100 times greater than our sun. These giant stars (but relatively cool) are very luminous. ...
Asymptotic Giant Branch
... Thermal Pulses 1. Quiet phase, H shell provides luminosity, T increase in He shell 2. He shell ignition (shell flash), expansion, H shell off 3. Cooling of He shell, reduction of energy production 4. Convective envelope reaches burning layers, third dredge up 5. Recovery of H-burning shell, quiet p ...
... Thermal Pulses 1. Quiet phase, H shell provides luminosity, T increase in He shell 2. He shell ignition (shell flash), expansion, H shell off 3. Cooling of He shell, reduction of energy production 4. Convective envelope reaches burning layers, third dredge up 5. Recovery of H-burning shell, quiet p ...
The Hertzsprung-Russell Diagram
... In general the hotter the star is the brighter it will be. Thus you would expect stars of the same size but different temperatures to form a diagonal line called an equal radius line. Equal Radius lines can be added to an H-R diagram ...
... In general the hotter the star is the brighter it will be. Thus you would expect stars of the same size but different temperatures to form a diagonal line called an equal radius line. Equal Radius lines can be added to an H-R diagram ...
properties of stars 2012
... Variable Stars are those whose luminosity varies. A PULSATING variable is a star that is swelling and shrinking. As it swells, the same energy is spread over a larger area, the star cools and appears dimmer. (also, star cols because less pressure allows energy to escape) As it shrinks, it heats up ...
... Variable Stars are those whose luminosity varies. A PULSATING variable is a star that is swelling and shrinking. As it swells, the same energy is spread over a larger area, the star cools and appears dimmer. (also, star cols because less pressure allows energy to escape) As it shrinks, it heats up ...
Earth Science, 10th edition Chapter 23: Beyond Our Solar System I
... d. Energy is released e. Outward pressure increases f. Outward pressure balanced by gravity pulling in g. Star becomes a stable main-sequence star 3. Main-sequence stage a. Stars age at different rates 1. Massive stars use fuel faster and exist for only a few million year 2. Small stars use fuel slo ...
... d. Energy is released e. Outward pressure increases f. Outward pressure balanced by gravity pulling in g. Star becomes a stable main-sequence star 3. Main-sequence stage a. Stars age at different rates 1. Massive stars use fuel faster and exist for only a few million year 2. Small stars use fuel slo ...
File
... is believed to occur when a massive star in a binary system loses its hydrogen-rich outer layers to its ...
... is believed to occur when a massive star in a binary system loses its hydrogen-rich outer layers to its ...
Space Test Explanations
... 11. As a new star is born, what type of atoms first begin to fuse? Hydrogen 12. Which type of new atoms are created when these first atoms fuse? Helium 13. Why are some stars red giants? In these stars, a lot of hydrogen has already fused. This fusion creates helium, which is more dense than hydroge ...
... 11. As a new star is born, what type of atoms first begin to fuse? Hydrogen 12. Which type of new atoms are created when these first atoms fuse? Helium 13. Why are some stars red giants? In these stars, a lot of hydrogen has already fused. This fusion creates helium, which is more dense than hydroge ...
Document
... object with respect to a distant background is called parallax. As Earth moves in its orbit, astronomers are able to observe stars from two different positions. Astronomers measure the parallax of nearby stars to determine their distance from Earth ...
... object with respect to a distant background is called parallax. As Earth moves in its orbit, astronomers are able to observe stars from two different positions. Astronomers measure the parallax of nearby stars to determine their distance from Earth ...
Today`s Class: Measuring temperatures of stars Astronomer`s
... spectral types of stars is true? a) The spectral type of a star can be used to determine its surface temperature. b) The spectral type of a star can be used to ...
... spectral types of stars is true? a) The spectral type of a star can be used to determine its surface temperature. b) The spectral type of a star can be used to ...
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2-2 wkst - Home [www.petoskeyschools.org]
... ____________ 22. small hot stars that are dimmer than the sun ____________ 23. high-temperature stars that quickly use up their hydrogen ____________ 24. cool stars with high absolute magnitude ...
... ____________ 22. small hot stars that are dimmer than the sun ____________ 23. high-temperature stars that quickly use up their hydrogen ____________ 24. cool stars with high absolute magnitude ...
2. Stellar Physics
... fusion reactions in the stellar interior Other energy sources are dominant during star formation and stellar death: • Star formation - before the interior is hot enough for significant fusion, gravitational potential energy is radiated as the radius of the forming star contracts. Protostellar or pre ...
... fusion reactions in the stellar interior Other energy sources are dominant during star formation and stellar death: • Star formation - before the interior is hot enough for significant fusion, gravitational potential energy is radiated as the radius of the forming star contracts. Protostellar or pre ...
Common Stages 7 to 9
... While on the main sequence, the star is burning hydrogen. It’s luminosity is determined by the stars mass. The most intense fusion is occurring at the center regions of the core (highest pressure and temperature). ...
... While on the main sequence, the star is burning hydrogen. It’s luminosity is determined by the stars mass. The most intense fusion is occurring at the center regions of the core (highest pressure and temperature). ...
HW7-3
... (260)RQ 2: (a) Why is there a lower end to the main sequence? (b) Why is there an upper end? (a) Stars less than 0.08M☉ (8% of M☉) are not hot enough in their cores to run fusion. These are brown dwarfs. (b) Very massive stars have so much fusion that the outward forces overwhelm gravity and they ar ...
... (260)RQ 2: (a) Why is there a lower end to the main sequence? (b) Why is there an upper end? (a) Stars less than 0.08M☉ (8% of M☉) are not hot enough in their cores to run fusion. These are brown dwarfs. (b) Very massive stars have so much fusion that the outward forces overwhelm gravity and they ar ...
monkeyball_lifecycleofastar
... This is the stage when a red giant stops fusing helium and pushes the outer layers of itself outward a shown in the picture. When this happens all that is left is a solid dense core. At this point all life on earth would http://en.wikipedia.org/wik ...
... This is the stage when a red giant stops fusing helium and pushes the outer layers of itself outward a shown in the picture. When this happens all that is left is a solid dense core. At this point all life on earth would http://en.wikipedia.org/wik ...
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.