X Ray Astronomy
... Sources of X Rays:• X ray emmission is expected from astronomical objects that contain extremely hot gases at temperatures from about a million kelvin (K) to hundreds of millions of kelvin (MK). • Gravity also contributes in productional of X Rays . • Infalling gas and dust is heated by the strong ...
... Sources of X Rays:• X ray emmission is expected from astronomical objects that contain extremely hot gases at temperatures from about a million kelvin (K) to hundreds of millions of kelvin (MK). • Gravity also contributes in productional of X Rays . • Infalling gas and dust is heated by the strong ...
Life Cycle of a Star
... behind. • There is so much mass its gravity prevents even light from leaving it • Black holes can suck in nearby stars and solar systems. ...
... behind. • There is so much mass its gravity prevents even light from leaving it • Black holes can suck in nearby stars and solar systems. ...
Lives and Deaths of Stars (middle school)
... Isolated neutron stars are extremely hard to observe ...
... Isolated neutron stars are extremely hard to observe ...
Life Cycle of Star Flipbook
... 6. What is going to happen to our Sun’s magnitude and temperature when it goes to its next stage? 7. What is the final stage of our Sun’s life? 8. What will happen to our Sun’s magnitude and temperature when it goes to its final stage? 9. What determines which star will go supernova? 10. What two fo ...
... 6. What is going to happen to our Sun’s magnitude and temperature when it goes to its next stage? 7. What is the final stage of our Sun’s life? 8. What will happen to our Sun’s magnitude and temperature when it goes to its final stage? 9. What determines which star will go supernova? 10. What two fo ...
How the univ works
... 17. A __________ ________ ______ was mistaken for a Russian nuclear bomb test. ...
... 17. A __________ ________ ______ was mistaken for a Russian nuclear bomb test. ...
Unit 1
... electrons merge into neutrons, taking energy away from the core • The core collapses, and the layers above fall rapidly toward the center, where they collide with the core material and “bounce” • The “bounced material collides with the remaining infalling gas, raising temperatures high enough to set ...
... electrons merge into neutrons, taking energy away from the core • The core collapses, and the layers above fall rapidly toward the center, where they collide with the core material and “bounce” • The “bounced material collides with the remaining infalling gas, raising temperatures high enough to set ...
Stages in the Formation of Stars
... 3. Name the process that causes a star to begin producing vast amounts of energy. _____________________________________________ 4. What two processes balance each other to make a star stable? ...
... 3. Name the process that causes a star to begin producing vast amounts of energy. _____________________________________________ 4. What two processes balance each other to make a star stable? ...
Protostar A nebula is a region of gas and dust in space. Over time
... - Region of gas and dust create a nebula - Gravity causes the gas and dust to condense creating a protostar - The prefix “proto” means first or original - A protostar is the original form of a star ...
... - Region of gas and dust create a nebula - Gravity causes the gas and dust to condense creating a protostar - The prefix “proto” means first or original - A protostar is the original form of a star ...
The Pulsar “Lighthouse”
... • Degenerate pressure of neutrons can support stars only up to 3M • For M > 3M: Further collapse Î black hole • Mass is so concentrated that light cannot escape. • One way to think about it: – vescape = 2GM/R becomes greater than speed of light. – So photons can’t escape. ...
... • Degenerate pressure of neutrons can support stars only up to 3M • For M > 3M: Further collapse Î black hole • Mass is so concentrated that light cannot escape. • One way to think about it: – vescape = 2GM/R becomes greater than speed of light. – So photons can’t escape. ...
Chapter 11 - USD Home Pages
... 10,000 times as luminous as our sun will have a mass of about 10 M . Chap 12 will show that explains its short life of only 10 million years. b. A star with a mass of 10−1 M will have a luminosity of about 10−3 L . That’s why its life will be 1000 billion years. 44. What if? The Sun were a B-type ...
... 10,000 times as luminous as our sun will have a mass of about 10 M . Chap 12 will show that explains its short life of only 10 million years. b. A star with a mass of 10−1 M will have a luminosity of about 10−3 L . That’s why its life will be 1000 billion years. 44. What if? The Sun were a B-type ...
PowerPoint - Chandra X
... Robotic Optical Monitoring and Polarimetry Telescopes (PROMPT) and the Two Micron All Sky Survey (2MASS). ...
... Robotic Optical Monitoring and Polarimetry Telescopes (PROMPT) and the Two Micron All Sky Survey (2MASS). ...
Star Life Cycle Poster
... Star Life Cycle Poster You need to investigate the life cycle of stars and other objects in the universe. All work must be typed. You may work alone or with a partner and turn in one assignment. 1. Give a description or definition, in YOUR OWN WORDS, for the following terms. (1 pt. each) Black hole ...
... Star Life Cycle Poster You need to investigate the life cycle of stars and other objects in the universe. All work must be typed. You may work alone or with a partner and turn in one assignment. 1. Give a description or definition, in YOUR OWN WORDS, for the following terms. (1 pt. each) Black hole ...
AST 443
... 5. The Sun will reside on the main sequence for 1010 years. If the luminosity of a main-sequence star is proportional to the fourth power of the star’s mass, what mass star is just now leaving the main sequence in a cluster that formed (a) ...
... 5. The Sun will reside on the main sequence for 1010 years. If the luminosity of a main-sequence star is proportional to the fourth power of the star’s mass, what mass star is just now leaving the main sequence in a cluster that formed (a) ...
Lecture 22 - Star Formation from Molecular Clouds
... • We understand the physics of these processes (at least partially) • We believe the Sun formed like this. • What characteristic of the solar system can we see that is an indicator of the processes of contraction, jet formation, accretion disk formation, etc? ...
... • We understand the physics of these processes (at least partially) • We believe the Sun formed like this. • What characteristic of the solar system can we see that is an indicator of the processes of contraction, jet formation, accretion disk formation, etc? ...
Section 3-3(rev04) 2
... near it will be pulled so strongly that it will spin rapidly around the black hole. This will cause the gas to give off x-rays that we can detect. • We can also detect black holes from the effect they have on the gravity of nearby stars. ...
... near it will be pulled so strongly that it will spin rapidly around the black hole. This will cause the gas to give off x-rays that we can detect. • We can also detect black holes from the effect they have on the gravity of nearby stars. ...
Protostar, Initial mass, Main Sequence
... Red dwarf stars with less than half a solar mass do not achieve red giant status they begin to fade as soon as their hydrogen fuel is exhausted. White dwarfs, planetary nebulae Our Sun, and any star with similar mass, will fuse to carbon and, possibly, oxygen and neon before shrinking to become a wh ...
... Red dwarf stars with less than half a solar mass do not achieve red giant status they begin to fade as soon as their hydrogen fuel is exhausted. White dwarfs, planetary nebulae Our Sun, and any star with similar mass, will fuse to carbon and, possibly, oxygen and neon before shrinking to become a wh ...
ASTR2050 Spring 2005 • In this class we will ...
... MBol (!) − MBol (!) = 2.5 log10 [L(!)/L(!)] ...
... MBol (!) − MBol (!) = 2.5 log10 [L(!)/L(!)] ...
life and death of a high mass star 2
... AFTER THAT, THEY LOSE THEIR MASS AND HEAT AND BEGIN TO DIE. THIS PROCESS TAKES BILLIONS AND BILLIONS OF YEARS. ...
... AFTER THAT, THEY LOSE THEIR MASS AND HEAT AND BEGIN TO DIE. THIS PROCESS TAKES BILLIONS AND BILLIONS OF YEARS. ...
Chapter 5 Mid-term Study Guide
... ______ The star continues to give off the same amount of energy for billions of years. ______ The star swells to a red giant or supergiant. ______ It collapses, causing increased fusion and energy. ______ The star uses up its hydrogen. ______ Material in the cloud, or nebula, begins to give off ener ...
... ______ The star continues to give off the same amount of energy for billions of years. ______ The star swells to a red giant or supergiant. ______ It collapses, causing increased fusion and energy. ______ The star uses up its hydrogen. ______ Material in the cloud, or nebula, begins to give off ener ...
Today`s Powerpoint
... Gravity is so strong that nothing can escape, not even light => black hole. Schwarzschild radius for Earth is 1 cm. For a 3 MSun object, it’s 9 km. ...
... Gravity is so strong that nothing can escape, not even light => black hole. Schwarzschild radius for Earth is 1 cm. For a 3 MSun object, it’s 9 km. ...
SHORT ANSWER. Answer the questions, showingh your work for
... a. If there were no air resistance, so that the mass falls with the acceleration of gravity ge=10 m/s2, about how fast (in m/s) would it be going when it hit the ground? ...
... a. If there were no air resistance, so that the mass falls with the acceleration of gravity ge=10 m/s2, about how fast (in m/s) would it be going when it hit the ground? ...
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.