GLY 1001 Earth Science Name:__Answers
... Red giant – A large, cool star of high luminosity, a star occupying the upper-right portion of the Hertzsprung-Russell Diagram. Reflection nebula – A relatively dense dust cloud in interstellar space that is illuminated by starlight. Spiral galaxy – A flattened, rotating galaxy with pinwheel-like ar ...
... Red giant – A large, cool star of high luminosity, a star occupying the upper-right portion of the Hertzsprung-Russell Diagram. Reflection nebula – A relatively dense dust cloud in interstellar space that is illuminated by starlight. Spiral galaxy – A flattened, rotating galaxy with pinwheel-like ar ...
v3 Long theoretical questions Instructions 1. You will receive in your
... 500 nm is adequately approximated by the formula: Lλ (λ) λ4 (i.e., the spectral density of the object's luminosity, known also as the monochromatic luminosity, is proportional to λ4.) ...
... 500 nm is adequately approximated by the formula: Lλ (λ) λ4 (i.e., the spectral density of the object's luminosity, known also as the monochromatic luminosity, is proportional to λ4.) ...
Chapter 30 Graphing skills worksheet
... Line Graphs and the Surface Temperature of Stars Astronomers can determine the temperature of individual stars based on their color. The temperature of the star is higher as you move across the spectrum from red to blue. The data that shows this is found in the table below. Surface Temperature of St ...
... Line Graphs and the Surface Temperature of Stars Astronomers can determine the temperature of individual stars based on their color. The temperature of the star is higher as you move across the spectrum from red to blue. The data that shows this is found in the table below. Surface Temperature of St ...
AS2001
... • Q2: What changes to the particle content of the expanding Universe occur at the following epochs: • Annihilation: particles and anti-particles annihilate, producing photons. Small excess of particles (~1 per 109 photons) • Baryogenesis: free quarks confined by strong force in (colourless) groups ...
... • Q2: What changes to the particle content of the expanding Universe occur at the following epochs: • Annihilation: particles and anti-particles annihilate, producing photons. Small excess of particles (~1 per 109 photons) • Baryogenesis: free quarks confined by strong force in (colourless) groups ...
Nuclear Fusion Nuclear Physics Mass Number Structure of Matter
... Detection of Neutrinos – Difficult since they interact so weakly with matter – Takes very large detectors – Several have been built to detect different types of neutrinos from inside the sun ...
... Detection of Neutrinos – Difficult since they interact so weakly with matter – Takes very large detectors – Several have been built to detect different types of neutrinos from inside the sun ...
Unit 5 - Stars
... Use this temperature and pressure to fuse together Hydrogen nuclei (protons) into Helium nuclei For each helium atom created, place one bead next to it Continue this until all your Hydrogen supply is gone Write down how many Helium atoms there are Leave the 7 beads in the Helium quadrant. At this po ...
... Use this temperature and pressure to fuse together Hydrogen nuclei (protons) into Helium nuclei For each helium atom created, place one bead next to it Continue this until all your Hydrogen supply is gone Write down how many Helium atoms there are Leave the 7 beads in the Helium quadrant. At this po ...
South Pasadena • Chemistry Name 8 • Nuclear Chemistry Period
... 1. What chemical element is the primary constituent of a young star? 2. Name the astrophysicist who first advanced the idea that the chemical elements originated from hydrogen in stars. 3. Name the stellar process in which the fusion of hydrogen produces other elements. 4. Why is iron the heaviest e ...
... 1. What chemical element is the primary constituent of a young star? 2. Name the astrophysicist who first advanced the idea that the chemical elements originated from hydrogen in stars. 3. Name the stellar process in which the fusion of hydrogen produces other elements. 4. Why is iron the heaviest e ...
Introduction:
... Fontaine and his colleagues made two assumptions about the state of the star that they would then go on to verify. Firstly they assumed that the star was a slow rotator. This would mean that the pulsation periods of the star would be much smaller than its rotation period. To validate this assumptio ...
... Fontaine and his colleagues made two assumptions about the state of the star that they would then go on to verify. Firstly they assumed that the star was a slow rotator. This would mean that the pulsation periods of the star would be much smaller than its rotation period. To validate this assumptio ...
pptx
... Main sequence stars fuse hydrogen to helium in core Red giants (and subgiants) fuse hydrogen to helium in shell outside helium core Stars have nearly constant ...
... Main sequence stars fuse hydrogen to helium in core Red giants (and subgiants) fuse hydrogen to helium in shell outside helium core Stars have nearly constant ...
The “Tuning Fork” Diagram Galaxy Properties 1 “Early”
... • Maximum rotation velocity-Luminosity relation [FIG 25.10] • Tully-Fisher relation ...
... • Maximum rotation velocity-Luminosity relation [FIG 25.10] • Tully-Fisher relation ...
9 - WordPress.com
... describe the key features of stellar spectra and describe how these are used to classify stars describe how spectra can provide information on surface temperature, rotational and translational velocity, density and chemical composition of stars ...
... describe the key features of stellar spectra and describe how these are used to classify stars describe how spectra can provide information on surface temperature, rotational and translational velocity, density and chemical composition of stars ...
Chapter 14
... High Mass Stars – Less than 100 M on Main Sequence – Become Neutron Stars (1.4M < M < 3M) » Neutron Degeneracy Pressure ...
... High Mass Stars – Less than 100 M on Main Sequence – Become Neutron Stars (1.4M < M < 3M) » Neutron Degeneracy Pressure ...
death_high_mass_2b
... • When a high mass star runs out of hydrogen in its core, the core begins to shrink. The outside of the star expands and the star moves right on the H-R diagram. • The temperature is cooling and the radius is growing, but the luminosity is virtually constant. • Since L = σT4(4πR2); T4 must be chang ...
... • When a high mass star runs out of hydrogen in its core, the core begins to shrink. The outside of the star expands and the star moves right on the H-R diagram. • The temperature is cooling and the radius is growing, but the luminosity is virtually constant. • Since L = σT4(4πR2); T4 must be chang ...
Astronomy 100 Name(s):
... (celestial south pole) to +90° (celestial north pole). Both of these coordinates are laminated to the metal pole bases. In addition, the stars have been colored according to their spectral classes; blue balls represent O, B and A type stars; yellow represent F and G type; orange represents K type an ...
... (celestial south pole) to +90° (celestial north pole). Both of these coordinates are laminated to the metal pole bases. In addition, the stars have been colored according to their spectral classes; blue balls represent O, B and A type stars; yellow represent F and G type; orange represents K type an ...
The light curves for a nova look like the following.
... The s-process works as long as the decay time for unstable isotopes is longer than the capture time. Up to the element bismuth (atomic number 83), the s-process works, but above this point the more massive nuclei that can be built from bismuth are unstable. 2) r-process (r means rapid) In this proce ...
... The s-process works as long as the decay time for unstable isotopes is longer than the capture time. Up to the element bismuth (atomic number 83), the s-process works, but above this point the more massive nuclei that can be built from bismuth are unstable. 2) r-process (r means rapid) In this proce ...
Balloon Model of the Life Cycle of Stars
... Throw most of the confetti into the air. When there is enough, or if it is compressed by other nearby events, gravity pulls the gas together into a dense ball. Gravity increases the heat and pressure so much that hydrogen in the gas begins to fuse into helium. A star is born. (We ignore planetary fo ...
... Throw most of the confetti into the air. When there is enough, or if it is compressed by other nearby events, gravity pulls the gas together into a dense ball. Gravity increases the heat and pressure so much that hydrogen in the gas begins to fuse into helium. A star is born. (We ignore planetary fo ...
Different types of YSOs
... • YSO has not yet ignited H; it follows Hayashi track in luminosity & ...
... • YSO has not yet ignited H; it follows Hayashi track in luminosity & ...
Nuclear Nomenclature
... Neutron Stars and Black Holes • If matter is forced to even higher densities than in a white dwarf, 106 times that of water, it collapses but could stabilize to form a neutron star with aid of additional pressure from nucleon degeneracy and the strong nuclear force. ...
... Neutron Stars and Black Holes • If matter is forced to even higher densities than in a white dwarf, 106 times that of water, it collapses but could stabilize to form a neutron star with aid of additional pressure from nucleon degeneracy and the strong nuclear force. ...
Section 14
... A star can live billions of years this way; the Sun is believed to be approximately halfway through its estimated 10 billion-year life. However, it's lifetime is determined by its size at the outset--the larger the star, the shorter its life. However, the larger the star, the brighter it is. The Sun ...
... A star can live billions of years this way; the Sun is believed to be approximately halfway through its estimated 10 billion-year life. However, it's lifetime is determined by its size at the outset--the larger the star, the shorter its life. However, the larger the star, the brighter it is. The Sun ...
Astrophysics and Chemistry Review Guide
... What is the difference between apparent magnitude and absolute magnitude? What are 5 ways mass influences a star? About how far away is the sun? What is the chorus to the sun song? “The sun is a mass…” Why do Hubble images of stars have 4 points? Describe a super high mass stars life cycle? Describe ...
... What is the difference between apparent magnitude and absolute magnitude? What are 5 ways mass influences a star? About how far away is the sun? What is the chorus to the sun song? “The sun is a mass…” Why do Hubble images of stars have 4 points? Describe a super high mass stars life cycle? Describe ...
Asteroseismology of white dwarf stars provides important constraints
... stellar pulsations to probe the physics of convection through nonlinear light curve fitting. We have chosen R808 (mv=14.2) as our second target for XCOV26 for its importance to both asteroseismology and our understanding of convection across the DAV instability strip. R808 was discovered to be a pul ...
... stellar pulsations to probe the physics of convection through nonlinear light curve fitting. We have chosen R808 (mv=14.2) as our second target for XCOV26 for its importance to both asteroseismology and our understanding of convection across the DAV instability strip. R808 was discovered to be a pul ...
The Mass-Radius Relation for Polytropes The mass within any point
... In other words, the radius of a polytropic star is related to its mass by (1−n)/(3−n) R ∝ MT Note what this means: for a polytropic index of 3/2 (the γ = 5/3 case), R ∝ M−1/3 . Thus, for a set of stars with the same K and n (i.e., white dwarfs, or a fully convective star that is undergoing mass tra ...
... In other words, the radius of a polytropic star is related to its mass by (1−n)/(3−n) R ∝ MT Note what this means: for a polytropic index of 3/2 (the γ = 5/3 case), R ∝ M−1/3 . Thus, for a set of stars with the same K and n (i.e., white dwarfs, or a fully convective star that is undergoing mass tra ...
Formation of the Universe
... to and it becomes a white dwarf. After it cools, which takes billions of years, a white dwarf becomes a black dwarf. In larger stars, when fuel runs out and the material contracts a huge explosion occurs. Depending on the size of the star, this explosion is called a nova or supernova. These explosio ...
... to and it becomes a white dwarf. After it cools, which takes billions of years, a white dwarf becomes a black dwarf. In larger stars, when fuel runs out and the material contracts a huge explosion occurs. Depending on the size of the star, this explosion is called a nova or supernova. These explosio ...
The Fourth Day (January 5, 2014)
... afterthought. “He made the stars also.” According to National Geographic, there are likely more than 100 billion galaxies with each galaxy containing more than 100 billion stars. If you and I had been in charge of creation it might have taken us at least two days to accomplish that small feat, don’t ...
... afterthought. “He made the stars also.” According to National Geographic, there are likely more than 100 billion galaxies with each galaxy containing more than 100 billion stars. If you and I had been in charge of creation it might have taken us at least two days to accomplish that small feat, don’t ...
Main sequence
In astronomy, the main sequence is a continuous and distinctive band of stars that appears on plots of stellar color versus brightness. These color-magnitude plots are known as Hertzsprung–Russell diagrams after their co-developers, Ejnar Hertzsprung and Henry Norris Russell. Stars on this band are known as main-sequence stars or ""dwarf"" stars.After a star has formed, it generates thermal energy in the dense core region through the nuclear fusion of hydrogen atoms into helium. During this stage of the star's lifetime, it is located along the main sequence at a position determined primarily 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 hot core is balanced by the inward pressure of gravitational collapse from the overlying layers. The strong dependence of the rate of energy generation in the core on the temperature and pressure helps to sustain this balance. Energy generated at the core makes its way to the surface and is radiated away at the photosphere. The energy is carried by either radiation or convection, with the latter occurring in regions with steeper temperature gradients, higher opacity or both.The main sequence is sometimes divided into upper and lower parts, based on the dominant process that a star uses to generate energy. Stars below about 1.5 times the mass of the Sun (or 1.5 solar masses (M☉)) primarily fuse hydrogen atoms together in a series of stages to form helium, a sequence called the proton–proton chain. Above this mass, in the upper main sequence, the nuclear fusion process mainly uses atoms of carbon, nitrogen and oxygen as intermediaries in the CNO cycle that produces helium from hydrogen atoms. Main-sequence stars with more than two solar masses undergo convection in their core regions, which acts to stir up the newly created helium and maintain the proportion of fuel needed for fusion to occur. Below this mass, stars have cores that are entirely radiative with convective zones near the surface. With decreasing stellar mass, the proportion of the star forming a convective envelope steadily increases, whereas main-sequence stars below 0.4 M☉ undergo convection throughout their mass. When core convection does not occur, a helium-rich core develops surrounded by an outer layer of hydrogen.In general, the more massive a star is, the shorter its lifespan on the main sequence. After the hydrogen fuel at the core has been consumed, the star evolves away from the main sequence on the HR diagram. The behavior of a star now depends on its mass, with stars below 0.23 M☉ becoming white dwarfs directly, whereas stars with up to ten solar masses pass through a red giant stage. More massive stars can explode as a supernova, or collapse directly into a black hole.