Matariki powerpoint
... “Now listen, you must stay close to these rocks and don’t go adventuring out in the open sea. Today Tataraimaka is going fishing.” Tataraimaka was a giant who loved to fish with a giant black net. He had made the net from the beautiful flax that grew near Spirits Bay. ...
... “Now listen, you must stay close to these rocks and don’t go adventuring out in the open sea. Today Tataraimaka is going fishing.” Tataraimaka was a giant who loved to fish with a giant black net. He had made the net from the beautiful flax that grew near Spirits Bay. ...
Exercise 9
... declination (think of this as a space latitude). The declination runs from -90° (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 ...
... declination (think of this as a space latitude). The declination runs from -90° (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 ...
Stars - Academic Computer Center
... • Since stars are so far away they almost always appear just as points of light. • But as we already know we can learn a lot from light! • Light can tell us about a star’s: ...
... • Since stars are so far away they almost always appear just as points of light. • But as we already know we can learn a lot from light! • Light can tell us about a star’s: ...
Cosmology Fact Sheet
... Possible types of matter that might live in them would be MACHOs (Massive Astrophysical Halo Objects). Obviously, if something gets enough mass, it becomes a star so these would have to be “nearly stars” which never started a fusion reaction or dead stars which have run out of fusion fuel. However, ...
... Possible types of matter that might live in them would be MACHOs (Massive Astrophysical Halo Objects). Obviously, if something gets enough mass, it becomes a star so these would have to be “nearly stars” which never started a fusion reaction or dead stars which have run out of fusion fuel. However, ...
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 correct answers are written in bold, italic and underlined. The
... electromagnetic radiation at precise rates from neutron stars or pulsars in our universe? • The rapid orbiting of a neutron star around a black hole, the intense gravitational field of which periodically focuses emitted electromagnetic radiation from the neutron star toward the Earth • The regular p ...
... electromagnetic radiation at precise rates from neutron stars or pulsars in our universe? • The rapid orbiting of a neutron star around a black hole, the intense gravitational field of which periodically focuses emitted electromagnetic radiation from the neutron star toward the Earth • The regular p ...
nuclear fusion atoms
... 5. By looking deep into space, we can see back in time about __________________ billion years. 6. Many cosmologists say the ________ _________ Theory helps explain why the universe has universal forces and continues to expand today. 7. A ________________ is a huge ball of fiery gas, generally a mill ...
... 5. By looking deep into space, we can see back in time about __________________ billion years. 6. Many cosmologists say the ________ _________ Theory helps explain why the universe has universal forces and continues to expand today. 7. A ________________ is a huge ball of fiery gas, generally a mill ...
CHP 11
... a. the balance between the pressure and force of gravity inside a star. b. the force that binds protons and neutrons together to form a nucleus. c. the force that binds an electron to the nucleus in an atom. d. a measure of the ease with which photons can pass through a gas. e. the temperature and d ...
... a. the balance between the pressure and force of gravity inside a star. b. the force that binds protons and neutrons together to form a nucleus. c. the force that binds an electron to the nucleus in an atom. d. a measure of the ease with which photons can pass through a gas. e. the temperature and d ...
Hydrostatic Equilibrium of Hypothetical Quark Stars
... Department of Physics, Kyoto University Kyoto ...
... Department of Physics, Kyoto University Kyoto ...
Contents ISP 205 Section 2 Study Guide for Test 3 28 March 2007
... o Giants burn hydrogen in a shell, helium, or other elements White dwarfs are earth-sized, dead stars. Main sequence is a mass sequence o O stars are massive o M stars have least mass Hot massive stars live a short life and cool stars live a long time o Lifetime=mass/luminosity o Comparison: If sun ...
... o Giants burn hydrogen in a shell, helium, or other elements White dwarfs are earth-sized, dead stars. Main sequence is a mass sequence o O stars are massive o M stars have least mass Hot massive stars live a short life and cool stars live a long time o Lifetime=mass/luminosity o Comparison: If sun ...
Notes on White Dwarfs and Neutron Stars.
... We are thus led to contemplate a shrinking star where the electrons have been gobbled up by protons and the nuclei have dissolved into a dense neutron gas. What about the stability of such an object? Our first idea is to use the same equations as for the electrons: A degenerate neutron gas. We just ...
... We are thus led to contemplate a shrinking star where the electrons have been gobbled up by protons and the nuclei have dissolved into a dense neutron gas. What about the stability of such an object? Our first idea is to use the same equations as for the electrons: A degenerate neutron gas. We just ...
Lecture 2
... Mass M(r) contained within a star of radius r is determined by the density of the gas ρ( r). Consider a thin shell inside the star with radius r and outer radius r+δr ...
... Mass M(r) contained within a star of radius r is determined by the density of the gas ρ( r). Consider a thin shell inside the star with radius r and outer radius r+δr ...
MSci Astrophysics 210PHY412 - QUB Astrophysics Research Centre
... quantities depend on the distance from the centre of the star alone 1) Equation of hydrostatic equilibrium: at each radius, forces due to pressure differences balance gravity 2) Conservation of mass 3) Conservation of energy : at each radius, the change in the energy flux = local rate of energy rele ...
... quantities depend on the distance from the centre of the star alone 1) Equation of hydrostatic equilibrium: at each radius, forces due to pressure differences balance gravity 2) Conservation of mass 3) Conservation of energy : at each radius, the change in the energy flux = local rate of energy rele ...
The Kunlun Infrared Sky Survey
... SNIa standard candle is more accurate in the NIR (Barone-Nugent et al. 2012). Race is now on to distinguish Einstein vacuum energy from other possible equations of state. Requires accumulation of hundreds of accurate SNIa measurements. SkyMapper (Schmidt et al. 2005) is devoted to this. ...
... SNIa standard candle is more accurate in the NIR (Barone-Nugent et al. 2012). Race is now on to distinguish Einstein vacuum energy from other possible equations of state. Requires accumulation of hundreds of accurate SNIa measurements. SkyMapper (Schmidt et al. 2005) is devoted to this. ...
Herbig Ae/Be Stars
... + The birthline is generally near the D-burning main sequence + Whether the D-burning main sequence defines an exact starting point for for T Tauri stars depends on factors such as how much thermal energy is added during protostellar accretion + The youngest low mass stars are observed near the birt ...
... + The birthline is generally near the D-burning main sequence + Whether the D-burning main sequence defines an exact starting point for for T Tauri stars depends on factors such as how much thermal energy is added during protostellar accretion + The youngest low mass stars are observed near the birt ...
The World Year of Physics is a worldwide celebration of physics
... Can you spot the "new star"? It's supernova 2004dj, which was discovered in the outskirts of NGC 2403, a nearby spiral galaxy, in July of 2004. At about 11 million light-years from Earth, it is the closest such stellar explosion of the past decade, and observations of it continue to reveal clues to ...
... Can you spot the "new star"? It's supernova 2004dj, which was discovered in the outskirts of NGC 2403, a nearby spiral galaxy, in July of 2004. At about 11 million light-years from Earth, it is the closest such stellar explosion of the past decade, and observations of it continue to reveal clues to ...
Lecture 13
... Example of estimating stellar radii The nearby star 'Sirius A' has a surface temperature T~10,000 K and a flux of arriving radiation at Earth (integrated over all wavelengths) of : F = 1.2 x 107 W/m2 From measurement of parallax, the distance is r = 2.64 pc = ...
... Example of estimating stellar radii The nearby star 'Sirius A' has a surface temperature T~10,000 K and a flux of arriving radiation at Earth (integrated over all wavelengths) of : F = 1.2 x 107 W/m2 From measurement of parallax, the distance is r = 2.64 pc = ...
Summation Packet KEY
... the rays of the sun are hitting the earth more directly (greater angle). 56. Explain what causes seasons on Earth. The tilt and rotation of the Earth 57. Describe the difference between Spring Tides and Neap Tides. Be sure to tie the tides to the appropriate lunar phase and how often they occur. Spr ...
... the rays of the sun are hitting the earth more directly (greater angle). 56. Explain what causes seasons on Earth. The tilt and rotation of the Earth 57. Describe the difference between Spring Tides and Neap Tides. Be sure to tie the tides to the appropriate lunar phase and how often they occur. Spr ...
L2 - QUB Astrophysics Research Centre
... These two forces play the principal role in determining stellar structure – they must be (at least almost) in balance Thermal properties of stars – continually radiating into space. If thermal properties are constant, continual energy source must exist Theory must describe - origin of energy and tra ...
... These two forces play the principal role in determining stellar structure – they must be (at least almost) in balance Thermal properties of stars – continually radiating into space. If thermal properties are constant, continual energy source must exist Theory must describe - origin of energy and tra ...
Gravitational waves and neutrino emission from the merger of
... Today’s topic = Coalescence of binary neutron stars ✓Promising source of GWs ✓Theoretical candidate of Short-Gamma-Ray Burst ✓High-end laboratory for Nuclear theory A nuclear theory ⇒ Mass-Radius relation for Neutron Star Image of GRB ...
... Today’s topic = Coalescence of binary neutron stars ✓Promising source of GWs ✓Theoretical candidate of Short-Gamma-Ray Burst ✓High-end laboratory for Nuclear theory A nuclear theory ⇒ Mass-Radius relation for Neutron Star Image of GRB ...
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.