Interstellar clouds
... Planetary Nebula • Planetary nebula may form around low-mass dying stars • Form when the mass ejected by the AGB star piles up in a dense expanding shell. • Planetary nebula are visible for about 50,000 years of so, and can be illuminated by a white dwarf. ...
... Planetary Nebula • Planetary nebula may form around low-mass dying stars • Form when the mass ejected by the AGB star piles up in a dense expanding shell. • Planetary nebula are visible for about 50,000 years of so, and can be illuminated by a white dwarf. ...
Astro-Spectroscpy
... Structure of the Sun: Three Zones Core, Radiative, Convective • Energy is produced in the core via thermonuclear reactions and radiates out through the star • Radiation diffuses through the Radiative zone via lightmatter interactions • Convection occurs in the outermost regions before radiation eme ...
... Structure of the Sun: Three Zones Core, Radiative, Convective • Energy is produced in the core via thermonuclear reactions and radiates out through the star • Radiation diffuses through the Radiative zone via lightmatter interactions • Convection occurs in the outermost regions before radiation eme ...
astr study guide ex 3 s`16
... did it take for the supernova to decrease in brightness by a factor of 100? 27. Where are elements heavier than iron primarily produced? 28. What is The density of a neutron star? 29. The ____________ of a black hole is the radius from a black hole at which the escape velocity is approximately equal ...
... did it take for the supernova to decrease in brightness by a factor of 100? 27. Where are elements heavier than iron primarily produced? 28. What is The density of a neutron star? 29. The ____________ of a black hole is the radius from a black hole at which the escape velocity is approximately equal ...
Life Cycle of Stars
... • These stars can exhaust their fuel in as little as 1 million years. • This large star is one of the most luminous in the universe. • It expands into a red supergiant and ends in a powerful supernova explosion. ...
... • These stars can exhaust their fuel in as little as 1 million years. • This large star is one of the most luminous in the universe. • It expands into a red supergiant and ends in a powerful supernova explosion. ...
Why Is the Sun a Star
... The Sun is the center of our Solar System. It is so massive that its strong gravity attracts all the planets and their moons, comets, asteroids and meteors into orbit around it. Its light provides Earth with 99% of all the energy used on our planet and we see its reflected light on all the planets a ...
... The Sun is the center of our Solar System. It is so massive that its strong gravity attracts all the planets and their moons, comets, asteroids and meteors into orbit around it. Its light provides Earth with 99% of all the energy used on our planet and we see its reflected light on all the planets a ...
ISP 205 Review Questions, Week 10
... from falling to the center. This is what we mean by gas pressure. Gas pressure is proportional to the density (the number of atoms per unit volume), and also to the average speed of the atoms (measured by the gas temperature). 3. Using the Hertzprung-Russell diagram in Figure ...
... from falling to the center. This is what we mean by gas pressure. Gas pressure is proportional to the density (the number of atoms per unit volume), and also to the average speed of the atoms (measured by the gas temperature). 3. Using the Hertzprung-Russell diagram in Figure ...
Lifecycle of a Star
... Super dense core of a star left over after a supernova. Only 5 to 15 MILES in diameter, but have a mass 1.5 – 2 times that of the Sun. ...
... Super dense core of a star left over after a supernova. Only 5 to 15 MILES in diameter, but have a mass 1.5 – 2 times that of the Sun. ...
A-105 Homework 1
... 20. (1 pt.) The Crab Nebula is now 1.35 pc in radius and is expanding at 1,400 km/s. About when did the supernova occur? ...
... 20. (1 pt.) The Crab Nebula is now 1.35 pc in radius and is expanding at 1,400 km/s. About when did the supernova occur? ...
Stars after the Main Sequence. Example: Betelgeuse (Alpha Orionis
... How do we check this result? ...
... How do we check this result? ...
Black holes - Red Hook Central School District
... get no more heat or light from it, but our elliptical orbit would not change. 2. We would not be “sucked in” 3. Spaceships near a black hole would merely go into orbit around it 4. Black Holes are so small it would be hard to “fall in” by accident ...
... get no more heat or light from it, but our elliptical orbit would not change. 2. We would not be “sucked in” 3. Spaceships near a black hole would merely go into orbit around it 4. Black Holes are so small it would be hard to “fall in” by accident ...
RFS_315_answers
... mass of a star the shorter it’s lifetime as it’s fuel is used much faster. Algol B is a dying K giant star but at only .81 solar masses, it is the LESS massive of the two. The dim companion has lost a great deal of mass to it’s closely orbiting partner. 15. Polaris is a variable star – what type of ...
... mass of a star the shorter it’s lifetime as it’s fuel is used much faster. Algol B is a dying K giant star but at only .81 solar masses, it is the LESS massive of the two. The dim companion has lost a great deal of mass to it’s closely orbiting partner. 15. Polaris is a variable star – what type of ...
File - Morgan, Kristen
... How can we find them if we can’t see them? We can’t, for sure. Matter falling into a black hole releases large bursts of X-rays. ...
... How can we find them if we can’t see them? We can’t, for sure. Matter falling into a black hole releases large bursts of X-rays. ...
The Lifecycle of Stars
... White Dwarfs When a star begins to run out of hydrogen it may become a White Dwarf A White Dwarf has no hydrogen left and can no longer generate energy by fusing hydrogen into helium. White Dwarf’s can shine for billions of years before they cool completely. ...
... White Dwarfs When a star begins to run out of hydrogen it may become a White Dwarf A White Dwarf has no hydrogen left and can no longer generate energy by fusing hydrogen into helium. White Dwarf’s can shine for billions of years before they cool completely. ...
Star Track 2 - The Search for a Supermassive Black... Early radio astronomers detected an immensely
... Early radio astronomers detected an immensely powerful source of radio waves towards the center of the Galaxy in the constellation Sagittarius; this mysterious object was designated SgrA*. More recently, infrared astronomers using adaptive optics have imaged individual stars near this object and tra ...
... Early radio astronomers detected an immensely powerful source of radio waves towards the center of the Galaxy in the constellation Sagittarius; this mysterious object was designated SgrA*. More recently, infrared astronomers using adaptive optics have imaged individual stars near this object and tra ...
ASTRONOMY 1 ... You may use this only this study guide for reference... No electronic devises: I pads, lap tops, phones, etc.
... 37. When a single star with a mass equal to the Sun dies, what will it become ? 38. Where are elements heavier than iron can only be created ? 39. When the mass of a star's core becomes greater than 1.4 times the mass of the Sun, degenerate electrons can no longer keep it as a white dwarf. Instead, ...
... 37. When a single star with a mass equal to the Sun dies, what will it become ? 38. Where are elements heavier than iron can only be created ? 39. When the mass of a star's core becomes greater than 1.4 times the mass of the Sun, degenerate electrons can no longer keep it as a white dwarf. Instead, ...
Big Bang, 429
... 37. When a single star with a mass equal to the Sun dies, what will it become ? 38. Where are elements heavier than iron can only be created ? 39. When the mass of a star's core becomes greater than 1.4 times the mass of the Sun, degenerate electrons can no longer keep it as a white dwarf. Instead, ...
... 37. When a single star with a mass equal to the Sun dies, what will it become ? 38. Where are elements heavier than iron can only be created ? 39. When the mass of a star's core becomes greater than 1.4 times the mass of the Sun, degenerate electrons can no longer keep it as a white dwarf. Instead, ...
122final10
... 3) The rate of neutron addition to Iron nuclei during supernova explosions tells us the intrinsic luminosity of the pre-supernovae stars determines the amount of Gold in the Earth ensures the creation of a neutron star depends on the core neutron degeneracy pressure causes the neutron star to collap ...
... 3) The rate of neutron addition to Iron nuclei during supernova explosions tells us the intrinsic luminosity of the pre-supernovae stars determines the amount of Gold in the Earth ensures the creation of a neutron star depends on the core neutron degeneracy pressure causes the neutron star to collap ...
Dead Stars They do exist! The white dwarf stars
... 2.40 solar masses for Sirius A) • Even though it is hotter than Sirius A, it is much fainter (look at difference in absolute magnitudes • The only way to do this is with small WD ...
... 2.40 solar masses for Sirius A) • Even though it is hotter than Sirius A, it is much fainter (look at difference in absolute magnitudes • The only way to do this is with small WD ...
Cygnus X-1
Cygnus X-1 (abbreviated Cyg X-1) is a well-known galactic X-ray source, thought to be a black hole, in the constellation Cygnus. It was discovered in 1964 during a rocket flight and is one of the strongest X-ray sources seen from Earth, producing a peak X-ray flux density of 6977229999999999999♠2.3×10−23 Wm−2 Hz−1 (7003230000000000000♠2.3×103 Jansky). Cygnus X-1 was the first X-ray source widely accepted to be a black hole and it remains among the most studied astronomical objects in its class. The compact object is now estimated to have a mass about 14.8 times the mass of the Sun and has been shown to be too small to be any known kind of normal star, or other likely object besides a black hole. If so, the radius of its event horizon is about 7004440000000000000♠44 km.Cygnus X-1 belongs to a high-mass X-ray binary system about 7019574266339685654♠6070 ly from the Sun that includes a blue supergiant variable star designated HDE 226868 which it orbits at about 0.2 AU, or 20% of the distance from the Earth to the Sun. A stellar wind from the star provides material for an accretion disk around the X-ray source. Matter in the inner disk is heated to millions of degrees, generating the observed X-rays. A pair of jets, arranged perpendicular to the disk, are carrying part of the energy of the infalling material away into interstellar space.This system may belong to a stellar association called Cygnus OB3, which would mean that Cygnus X-1 is about five million years old and formed from a progenitor star that had more than 7001400000000000000♠40 solar masses. The majority of the star's mass was shed, most likely as a stellar wind. If this star had then exploded as a supernova, the resulting force would most likely have ejected the remnant from the system. Hence the star may have instead collapsed directly into a black hole.Cygnus X-1 was the subject of a friendly scientific wager between physicists Stephen Hawking and Kip Thorne in 1975, with Hawking betting that it was not a black hole. He conceded the bet in 1990 after observational data had strengthened the case that there was indeed a black hole in the system. This hypothesis has not been confirmed due to a lack of direct observation but has generally been accepted from indirect evidence.