Northam Sky July 2009
... able to see the bright Globular Cluster “M4” or Messier 4 ( pictured below with Antares). M4 is made up of about a million stars similar to but older than our sun packed tightly together. Named after the french comet hunter, Messier from the 1800's who cataloged most of the bright fuzzy objects that ...
... able to see the bright Globular Cluster “M4” or Messier 4 ( pictured below with Antares). M4 is made up of about a million stars similar to but older than our sun packed tightly together. Named after the french comet hunter, Messier from the 1800's who cataloged most of the bright fuzzy objects that ...
Astronomy 15 - Problem Set Number 7
... incompressible) you would have to assemble to make a black hole. How does your number compare to the actual upper mass limit for neutron stars (about 2.5 M )? Why any discrepancy? (c) Suppose you were given an indefinitely large supply of magic, incompressible water (density = 1 gm cm−3 ). Show tha ...
... incompressible) you would have to assemble to make a black hole. How does your number compare to the actual upper mass limit for neutron stars (about 2.5 M )? Why any discrepancy? (c) Suppose you were given an indefinitely large supply of magic, incompressible water (density = 1 gm cm−3 ). Show tha ...
We Are All Stardust: Nuclear Physics in the Cosmos
... one another due to electromagnetic force If they get close enough together, the dominant strong nuclear force can be felt Probability of a reaction depends very strongly on temperature Only at very high temperatures of a few million K or higher can fusion occur, for typical pressures ...
... one another due to electromagnetic force If they get close enough together, the dominant strong nuclear force can be felt Probability of a reaction depends very strongly on temperature Only at very high temperatures of a few million K or higher can fusion occur, for typical pressures ...
declarative interrogative imperative
... The nearest star to Earth is the sun. © www.thecurriculumcorner.com ...
... The nearest star to Earth is the sun. © www.thecurriculumcorner.com ...
The Sun`s Size, Heat, and Structure
... size of a milk-bottle cap (about 3 centimeters), then the diameter of the largest star known, Epsilon Aurigae, would be the size of a football field. ...
... size of a milk-bottle cap (about 3 centimeters), then the diameter of the largest star known, Epsilon Aurigae, would be the size of a football field. ...
Coords
... radial distance respectively. Any object can be mapped using this system, including stars. The reference point is our sun, and distances to stars (Z axis) are measured radially outward in light years. The celestial latitude (Y axis) is measured in degrees north (positive) and south (negative) of the ...
... radial distance respectively. Any object can be mapped using this system, including stars. The reference point is our sun, and distances to stars (Z axis) are measured radially outward in light years. The celestial latitude (Y axis) is measured in degrees north (positive) and south (negative) of the ...
Nuclear Fusion – when two H atoms combine to form one atom thus
... Nebula – Stars are formed or “born” in a nebula. Massive cosmic cloud of matter from which stars are created. Light Year – distance light travels in one year. 186,000 miles/sec – speed of light Life Cycle of a Star Stars start off as a nebula until a nuclear explosion causes the star to shine. The n ...
... Nebula – Stars are formed or “born” in a nebula. Massive cosmic cloud of matter from which stars are created. Light Year – distance light travels in one year. 186,000 miles/sec – speed of light Life Cycle of a Star Stars start off as a nebula until a nuclear explosion causes the star to shine. The n ...
1: The scientific name for my field is astronomy
... 1: The scientific name for my field is Astronomy. 2: Chapters 20-22 in Earth Science deal with my field. 3: None of the chapters in the Science Interactions brown book are based on Astronomy. 4: Chapters 19-20 in the Science Interactions blue book are based on Astronomy. 5: Astronomers study anythin ...
... 1: The scientific name for my field is Astronomy. 2: Chapters 20-22 in Earth Science deal with my field. 3: None of the chapters in the Science Interactions brown book are based on Astronomy. 4: Chapters 19-20 in the Science Interactions blue book are based on Astronomy. 5: Astronomers study anythin ...
Observation
... Blue represents regions of low mass concentration, red and yellow are denser . Note the blue and red striations behind the head of the jet. These are bounded by internal shocks. ...
... Blue represents regions of low mass concentration, red and yellow are denser . Note the blue and red striations behind the head of the jet. These are bounded by internal shocks. ...
M - IMAG2E
... • Four fundamental observables used to parameterise stars and compare with models M, R, L, Te • M and R can be measured directly in small numbers of stars (will cover more of this later) • Age and chemical composition also dictate the position of stars in the HR diagram • Stellar clusters very usefu ...
... • Four fundamental observables used to parameterise stars and compare with models M, R, L, Te • M and R can be measured directly in small numbers of stars (will cover more of this later) • Age and chemical composition also dictate the position of stars in the HR diagram • Stellar clusters very usefu ...
PROBLEM SET #6 AST142 Due in class Tuesday Mar 17, 2015 First
... called the initial mass function (IMF). Consider the initial mass function with number of stars in a mass bin dM equal to N (M ) where M is the stellar mass. A power law, N (M ) = AM −α with constant A and index α is an approximate description for the initial mass function. Recent work has used more ...
... called the initial mass function (IMF). Consider the initial mass function with number of stars in a mass bin dM equal to N (M ) where M is the stellar mass. A power law, N (M ) = AM −α with constant A and index α is an approximate description for the initial mass function. Recent work has used more ...
The Great Bear and the Little Bear
... • Most of the gas in the inside of a star is hydrogen and its temperature is over 20 million degrees Fahrenheit. There is also helium, a gas that is formed when the hydrogen molecules join together. • The energy released by a star is equal to millions of hydrogen bombs exploding all at once. ...
... • Most of the gas in the inside of a star is hydrogen and its temperature is over 20 million degrees Fahrenheit. There is also helium, a gas that is formed when the hydrogen molecules join together. • The energy released by a star is equal to millions of hydrogen bombs exploding all at once. ...
Nova & SuperNova - Heart of the Valley Astronomers
... dwarfs. This maximum mass for a white dwarf is called the Chandrasekhar limit. • As the star contracts, all the lowest electron energy levels are filled and the electrons are forced into higher and higher energy levels, filling the lowest unoccupied energy levels. This creates an effective pressure ...
... dwarfs. This maximum mass for a white dwarf is called the Chandrasekhar limit. • As the star contracts, all the lowest electron energy levels are filled and the electrons are forced into higher and higher energy levels, filling the lowest unoccupied energy levels. This creates an effective pressure ...
HNRS 227 Lecture #2 Chapters 2 and 3
... Solar Flux = Lum (Sun) / 4 x distance2 Flux emitted = constant x T4 [Stefan-Boltzmann] Concluding from above yields ...
... Solar Flux = Lum (Sun) / 4 x distance2 Flux emitted = constant x T4 [Stefan-Boltzmann] Concluding from above yields ...
Die Sonne im Röntgenlicht - ST-ECF
... • Only observable from the space • Excellent imaging stability • Little background due to the Earth’s warm atmosphere Wang et al. 2009 ...
... • Only observable from the space • Excellent imaging stability • Little background due to the Earth’s warm atmosphere Wang et al. 2009 ...
HAYASHI LIMIT
... We can derive the SC critical mass by using the Virial theorem with the core boundary pressure retained and assuming an ideal gas, finding the maximum surface pressure the core can sustain (calculated in terms of core quantities), calculating the surface pressure due to the weight of the overlying e ...
... We can derive the SC critical mass by using the Virial theorem with the core boundary pressure retained and assuming an ideal gas, finding the maximum surface pressure the core can sustain (calculated in terms of core quantities), calculating the surface pressure due to the weight of the overlying e ...
Support worksheet – Topic 3 Questions
... Explain what the comparison of the density of the universe to the critical density allows us to determine. ...
... Explain what the comparison of the density of the universe to the critical density allows us to determine. ...
The life-cycle of stars - Young Scientists Journal
... just 20 kilometers, yet masses three times that of the Sun [Figure 6].[3] Some neutron stars emit radio waves. These neutron stars are called pulsars. The waves seem to flash on and off, but this is only the case due to the beam of radio waves rotating around the poles of the stars, while the Earth ...
... just 20 kilometers, yet masses three times that of the Sun [Figure 6].[3] Some neutron stars emit radio waves. These neutron stars are called pulsars. The waves seem to flash on and off, but this is only the case due to the beam of radio waves rotating around the poles of the stars, while the Earth ...
Stellar Evolution
... In which order will a single star of one solar mass progress through the various stages of stellar evolution? 1. Planetary nebula, main-sequence star, white dwarf, black hole 2. Proto-star, main-sequence star, planetary nebula, white dwarf 3. Proto-star, red giant, supernova, planetary nebula 4. Pr ...
... In which order will a single star of one solar mass progress through the various stages of stellar evolution? 1. Planetary nebula, main-sequence star, white dwarf, black hole 2. Proto-star, main-sequence star, planetary nebula, white dwarf 3. Proto-star, red giant, supernova, planetary nebula 4. Pr ...
30-1
... a. devices that separate light into different colors b. devices that separate light into different gases c. graphs that separate light into different spectra d. devices that gather light into different spectra _____ 4. What does a star’s dark-line spectrum reveal? a. the star’s distance and size b. ...
... a. devices that separate light into different colors b. devices that separate light into different gases c. graphs that separate light into different spectra d. devices that gather light into different spectra _____ 4. What does a star’s dark-line spectrum reveal? a. the star’s distance and size b. ...
Stellar Evolution Game (PDF: 112k)
... information to answer the questions during the game. 2. Students will also need to be knowledgeable about basic stellar evolution pathways for stars based on their masses. 3. Copy a set of the game cards on matching colored paper for each group. Use a different color for each group. Place game cards ...
... information to answer the questions during the game. 2. Students will also need to be knowledgeable about basic stellar evolution pathways for stars based on their masses. 3. Copy a set of the game cards on matching colored paper for each group. Use a different color for each group. Place game cards ...
kaekae14 dae dae15 lifecycleofastar
... Brown dwarfs are often thought of as "stillborn" stars. They have masses that range from twice the mass of Jupiter and ...
... Brown dwarfs are often thought of as "stillborn" stars. They have masses that range from twice the mass of Jupiter and ...
Characteristics of Stars
... distance from Earth and how bright the star actually is. The brightness of a star can be described in two different ways: apparent brightness and absolute brightness. A star’s apparent brightness is its brightness as seen from Earth. Astronomers can measure apparent brightness fairly easily using el ...
... distance from Earth and how bright the star actually is. The brightness of a star can be described in two different ways: apparent brightness and absolute brightness. A star’s apparent brightness is its brightness as seen from Earth. Astronomers can measure apparent brightness fairly easily using el ...
Gravity simplest fusion
... • They do not glow– no nuclear reaction occurs • Some neutron stars do emit radiation, in the form of x-rays and radio waves ...
... • They do not glow– no nuclear reaction occurs • Some neutron stars do emit radiation, in the form of x-rays and radio waves ...
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.