Life of stars, formation of elements
... • Many more similar starformation regions buried deep inside cloud. ...
... • Many more similar starformation regions buried deep inside cloud. ...
Document
... Model calculations predict the strength of various molecular lines, which can be compared to observations. The models are adjusted until agreement is found. The model is then used to predict the results of new observations and the process continues ...
... Model calculations predict the strength of various molecular lines, which can be compared to observations. The models are adjusted until agreement is found. The model is then used to predict the results of new observations and the process continues ...
This chapter has a brief overview of astronomical topics that we will
... not understand the moment of creation, but current physics can extrapolate back to a tiny fraction of a second after this event. All of space and time was created in this "Big Bang". There was nothing before (as there was no time) and it was not an explosion in space (since space was created here). ...
... not understand the moment of creation, but current physics can extrapolate back to a tiny fraction of a second after this event. All of space and time was created in this "Big Bang". There was nothing before (as there was no time) and it was not an explosion in space (since space was created here). ...
Chapter 30 Study Notes
... A star with the sun’s mass would stay on the main sequence of the H-R diagram for about _____ 10 billion years. ...
... A star with the sun’s mass would stay on the main sequence of the H-R diagram for about _____ 10 billion years. ...
Stellar Formation 1) Solar Wind/Sunspots 2) Interstellar Medium 3) Protostars
... cooler (~100 K) and denser (100x) than hot interstellar gas surrounding dust absorbs energetic light atoms and molecules can form 100s to 1000s of lightyears across 4,000 of them in our Galaxy ...
... cooler (~100 K) and denser (100x) than hot interstellar gas surrounding dust absorbs energetic light atoms and molecules can form 100s to 1000s of lightyears across 4,000 of them in our Galaxy ...
The ISM and Stellar Birth
... Reflection Nebulae: • Light reflected (scattered) by dust/gas much like the moon reflects the Sun’s light – so doesn’t generate its own light • Scatter light from cooler stars • Mostly scatters blue light (like our atmosphere) – so they appear blue. • Dust grains must have sizes ranging from 0.01mm ...
... Reflection Nebulae: • Light reflected (scattered) by dust/gas much like the moon reflects the Sun’s light – so doesn’t generate its own light • Scatter light from cooler stars • Mostly scatters blue light (like our atmosphere) – so they appear blue. • Dust grains must have sizes ranging from 0.01mm ...
SNC1PL The Life Cycle of Stars
... quickly. This spinning creates highfrequency radio waves, which have been detected by astronomers on Earth. ...
... quickly. This spinning creates highfrequency radio waves, which have been detected by astronomers on Earth. ...
main sequence star
... • This is the 4th and 5th stages of small mass stars. • Small mass stars will collapse into white dwarfs after being red giants. • The outer gases are lost, which allows us to see the core of the star. The white dwarf is very dense and hot. The emit (release) less light than they did when they were ...
... • This is the 4th and 5th stages of small mass stars. • Small mass stars will collapse into white dwarfs after being red giants. • The outer gases are lost, which allows us to see the core of the star. The white dwarf is very dense and hot. The emit (release) less light than they did when they were ...
mass of star
... Remember, takes energetic UV photons to ionize H. Hot, massive stars produce huge amounts of these. Such short-lived stars spend all their lives in the stellar nursery of their birth, so emission nebulae mark sites of ongoing star formation. Many stars of lower mass are forming too, but make few UV ...
... Remember, takes energetic UV photons to ionize H. Hot, massive stars produce huge amounts of these. Such short-lived stars spend all their lives in the stellar nursery of their birth, so emission nebulae mark sites of ongoing star formation. Many stars of lower mass are forming too, but make few UV ...
astronomy 2 review sheet - Hicksville Public Schools
... 9. What are eclipsing binary stars? A STAR SYSTEM WHERE ONE STAR BLOCKS THE LIGHT OF THE OTHER STAR AT REGULAR INTERVALS. 10. What are the different types of galaxies? SPIRAL. ELLIPTICAL, IRREGULAR. 11. What type of galaxy is the Milky Way? SPIRAL 12. What is the name of the theory that describes th ...
... 9. What are eclipsing binary stars? A STAR SYSTEM WHERE ONE STAR BLOCKS THE LIGHT OF THE OTHER STAR AT REGULAR INTERVALS. 10. What are the different types of galaxies? SPIRAL. ELLIPTICAL, IRREGULAR. 11. What type of galaxy is the Milky Way? SPIRAL 12. What is the name of the theory that describes th ...
3. Stellar Formation and Evolution
... • Eventually the outer layers of the star will be shed, creating a planetary nebula, with only a white dwarf left behind. ...
... • Eventually the outer layers of the star will be shed, creating a planetary nebula, with only a white dwarf left behind. ...
Final Exam Study Guide
... The escape velocity of a neutron star (speed you need to escape it) is about ________. A planetary nebula is typically formed at the same time as a(n) _______________. The process in which many stars form from a single interstellar cloud is called _______. Interstellar clouds cause stars behind them ...
... The escape velocity of a neutron star (speed you need to escape it) is about ________. A planetary nebula is typically formed at the same time as a(n) _______________. The process in which many stars form from a single interstellar cloud is called _______. Interstellar clouds cause stars behind them ...
SES4U Life Cycle of a Star
... Stars will spend the majority of their lives fusing H into He When H fuel is gone, He is fused into C Massive stars are able to fuse C into heavier elements Stars slowly contract as they release energy during their life, yet their internal temperatures, densities and pressures continue to increase i ...
... Stars will spend the majority of their lives fusing H into He When H fuel is gone, He is fused into C Massive stars are able to fuse C into heavier elements Stars slowly contract as they release energy during their life, yet their internal temperatures, densities and pressures continue to increase i ...
Foundation 1 - Discovering Astronomy
... As the temperature in the interior rises, nuclear reactions produce outward force and balances the inward force of gravity hydrostatic equilibrium = star becomes stable and contraction stopsmain-sequence star ...
... As the temperature in the interior rises, nuclear reactions produce outward force and balances the inward force of gravity hydrostatic equilibrium = star becomes stable and contraction stopsmain-sequence star ...
The Evolution of Massive Stars
... • Pulse of neutrinos as core collapses • “Pollution” of the interstellar medium as explosion blows off the outer stellar core • Birth of the “neutron star” ...
... • Pulse of neutrinos as core collapses • “Pollution” of the interstellar medium as explosion blows off the outer stellar core • Birth of the “neutron star” ...
Pre-Main Sequence Evolution
... collapse releases energy, which goes into further H2 disassociation (rather than heating the gas). Very quickly, all the molecular hydrogen is destroyed, and the protostar settles into a new hydrostatic equilibrium. Similar episodes occur when the temperature becomes hot enough to ionize hydrogen an ...
... collapse releases energy, which goes into further H2 disassociation (rather than heating the gas). Very quickly, all the molecular hydrogen is destroyed, and the protostar settles into a new hydrostatic equilibrium. Similar episodes occur when the temperature becomes hot enough to ionize hydrogen an ...
Stellar evolution, I
... If interstellar gas is cold enough and dense enough, it will collapse under its own gravitational power to form stars. The “free fall” time of a spherical cloud is given by: Tff = [3/(32 G )]1/2 , where G is Newton's gravitational constant and is the initial density of the cloud. If the densi ...
... If interstellar gas is cold enough and dense enough, it will collapse under its own gravitational power to form stars. The “free fall” time of a spherical cloud is given by: Tff = [3/(32 G )]1/2 , where G is Newton's gravitational constant and is the initial density of the cloud. If the densi ...
14 The Interstellar Medium and Star Formation
... temperature rises because it is becoming more compact. At stage 6, the core reaches 106 K, and nuclear fusion begins. The protostar has become a star, but it is not in equilibrium. The star continues to contract and increase in temperature until it is in equilibrium. This is stage 7: The star has re ...
... temperature rises because it is becoming more compact. At stage 6, the core reaches 106 K, and nuclear fusion begins. The protostar has become a star, but it is not in equilibrium. The star continues to contract and increase in temperature until it is in equilibrium. This is stage 7: The star has re ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.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.