![Lectures 10 & 11 powerpoint (stellar formation) [movie below]](http://s1.studyres.com/store/data/008083226_1-fec717da713794a7feea61d4eec0ceb1-300x300.png)
Lectures 10 & 11 powerpoint (stellar formation) [movie below]
... in the star. This is why we find stable stars on such a narrow strip (main sequence) in the Hertzsprung-Russell diagram. Pressure-temperature thermostat Q: How does the P-T thermostat control the reactions in stars? ...
... in the star. This is why we find stable stars on such a narrow strip (main sequence) in the Hertzsprung-Russell diagram. Pressure-temperature thermostat Q: How does the P-T thermostat control the reactions in stars? ...
Space Test Explanations
... 8. How does nuclear fusion produce energy? When atoms fuse, the new atoms that are created have less mass than the atoms that fused. This means mass is “lost.” That “lost” mass is converted to energy. 9. Nuclear fusion can only occur in the center of the solar system. Why is that? In order to fuse, ...
... 8. How does nuclear fusion produce energy? When atoms fuse, the new atoms that are created have less mass than the atoms that fused. This means mass is “lost.” That “lost” mass is converted to energy. 9. Nuclear fusion can only occur in the center of the solar system. Why is that? In order to fuse, ...
Stars & Galaxies
... The most massive stars- those having more than 40 times the mass of sun- become black holes when they die. ...
... The most massive stars- those having more than 40 times the mass of sun- become black holes when they die. ...
5Stars_Part_Two
... in England was studying the scintillation of radio sources due to the solar wind. 2. A graduate student named Jocelyn Bell Burnell discovered a strong night time source of “twinkling”. 3. Its location was fixed with respect to the stars. From Jay Pasachoff’s “Contemporary Astronomy” ...
... in England was studying the scintillation of radio sources due to the solar wind. 2. A graduate student named Jocelyn Bell Burnell discovered a strong night time source of “twinkling”. 3. Its location was fixed with respect to the stars. From Jay Pasachoff’s “Contemporary Astronomy” ...
How do stars form as a function of stellar mass
... How do stars form as a function of stellar mass? What are the effects of the immediate circumstellar environment? These are 2 fundamental questions that our study of companions to intermediate-mass pre-main sequence stars seeks to address. Herbig Ae/Be stars span the mass range from roughly 1.5 to 1 ...
... How do stars form as a function of stellar mass? What are the effects of the immediate circumstellar environment? These are 2 fundamental questions that our study of companions to intermediate-mass pre-main sequence stars seeks to address. Herbig Ae/Be stars span the mass range from roughly 1.5 to 1 ...
calculated using stefan`s law
... • Time taken by a photon to defuse from the center of the star to its surface. - In a star energy generated at the core. - Energy spread in the form of photons - While moving towards the surface it faces a large number of frequent collision - Energy and direction of travel of the photon changes. • I ...
... • Time taken by a photon to defuse from the center of the star to its surface. - In a star energy generated at the core. - Energy spread in the form of photons - While moving towards the surface it faces a large number of frequent collision - Energy and direction of travel of the photon changes. • I ...
Structure
... The human body requires 109 ergs/sec to live. 1 gram of hydrogen nuclei fused into helium nuclei will release enough energy to power a human for 200 years. ...
... The human body requires 109 ergs/sec to live. 1 gram of hydrogen nuclei fused into helium nuclei will release enough energy to power a human for 200 years. ...
NASA`s Chandra Sees Brightest Supernova Ever
... might help explain the unusually slow speed of only about 4000 km s−1 indicated by the H line, and might provide a natural explanation for the long duration and rise time of the SN because of time needed for energy to diffuse out of the massive envelope. However, Instead of 70 d, the observed peak ...
... might help explain the unusually slow speed of only about 4000 km s−1 indicated by the H line, and might provide a natural explanation for the long duration and rise time of the SN because of time needed for energy to diffuse out of the massive envelope. However, Instead of 70 d, the observed peak ...
The Galactic Super Star Cluster Westerlund 1
... times the mass of Orion. Therefore, we would have expected diffuse emission with L x = 3x10 35 erg s-1, which is five times more flux than we observe. We suggest that the IMF is nonstandard, as is often claimed for young, massive star clusters. ...
... times the mass of Orion. Therefore, we would have expected diffuse emission with L x = 3x10 35 erg s-1, which is five times more flux than we observe. We suggest that the IMF is nonstandard, as is often claimed for young, massive star clusters. ...
SIMBOL-X The
... • participate to the baffling against diffuse X-ray sky, • formation flying control with respect to the mirror s/c Mission scenario : • High elliptical orbit : 7 days period, and at launch : perigee : 44,000 km apogee : 253,000 km inclination : 5 degrees • Pointing perpendicular ± 20 deg to Sun - S/ ...
... • participate to the baffling against diffuse X-ray sky, • formation flying control with respect to the mirror s/c Mission scenario : • High elliptical orbit : 7 days period, and at launch : perigee : 44,000 km apogee : 253,000 km inclination : 5 degrees • Pointing perpendicular ± 20 deg to Sun - S/ ...
The Death of High Mass Stars
... hundred light years across) in our Galaxy (the Interstellar Medium stuff between the stars). The atoms and molecules in these clouds are moving with speeds according to the temperature of the cloud. If the cloud is cold enough, the particles will begin to come together due to the attractive force of ...
... hundred light years across) in our Galaxy (the Interstellar Medium stuff between the stars). The atoms and molecules in these clouds are moving with speeds according to the temperature of the cloud. If the cloud is cold enough, the particles will begin to come together due to the attractive force of ...
Unit 1 - UW Madison Astronomy Department
... Exploding white dwarfs (supernovae type Ia) provide good standard candle as ...
... Exploding white dwarfs (supernovae type Ia) provide good standard candle as ...
Death of Low Mass Stars 8 Solar Masses or less
... away, the core is exposed, the White Dwarf. • Extremely small, dense and hot. About the size of Earth with a density of 1010 kg/m3 (an object with the volume of 1 grape would have a mass of 1 ton… that’s like the mass of an elephant!!!). • Shines from stored heat, no fusion occurs in the core… the s ...
... away, the core is exposed, the White Dwarf. • Extremely small, dense and hot. About the size of Earth with a density of 1010 kg/m3 (an object with the volume of 1 grape would have a mass of 1 ton… that’s like the mass of an elephant!!!). • Shines from stored heat, no fusion occurs in the core… the s ...
Compact Extragalactic Star Formation
... the luminosity function of SSCs, and the mass function of their star formation? • Is optical/IR modeling of star formation in SSCs consistent with radio observations? • How do supernovae evolve in dense environments? ...
... the luminosity function of SSCs, and the mass function of their star formation? • Is optical/IR modeling of star formation in SSCs consistent with radio observations? • How do supernovae evolve in dense environments? ...
Brock physics - Brock University
... (c) a very small mass. (d) a very small radius. 23. Stars with masses in excess of 50 solar masses are very common. (a) True. (b) False. 24. The spectroscopic binaries are detected (a) as separate stars in telescopic view. (b) using spectroscopic parallax. (c) based on oscillating Doppler shifts of ...
... (c) a very small mass. (d) a very small radius. 23. Stars with masses in excess of 50 solar masses are very common. (a) True. (b) False. 24. The spectroscopic binaries are detected (a) as separate stars in telescopic view. (b) using spectroscopic parallax. (c) based on oscillating Doppler shifts of ...
Lecture 9 - Angular Momentum Transport o
... o Particles lost from the star also carry away angular momentum. Given an initial mass, rotation rate, and radius, we can thus calculate the rate of AM loss. ...
... o Particles lost from the star also carry away angular momentum. Given an initial mass, rotation rate, and radius, we can thus calculate the rate of AM loss. ...
Lecture 13 - BH Disks, Planet Formation
... Tv 3r 3 r r • Gap opened if Tt > Tv which means ...
... Tv 3r 3 r r • Gap opened if Tt > Tv which means ...
Life of a star - bahringcarthnoians
... enough to swallow the inner planets, up to Earth. But don’t panic, because this won’t happen for about 4.5 billion years. ...
... enough to swallow the inner planets, up to Earth. But don’t panic, because this won’t happen for about 4.5 billion years. ...
Life Cycle of Stars - Lab Science Schedule
... The iron atoms in a massive star begin to absorb energy rather than release energy – after nuclear fusion stops. This energy is released in an explosion called a supernova. This explosion can appear as bright as a million suns. During the explosion, the heat is so tremendous that iron atoms in the c ...
... The iron atoms in a massive star begin to absorb energy rather than release energy – after nuclear fusion stops. This energy is released in an explosion called a supernova. This explosion can appear as bright as a million suns. During the explosion, the heat is so tremendous that iron atoms in the c ...
THE LIFE CYCLE OF A STAR
... A star is a luminous globe of gas producing its own heat and light by nuclear reactions (nuclear fusion). They are born from nebulae and consist mostly of hydrogen and helium gas. Surface temperatures range from 2000C to above 30,000C, and the corresponding colors from red to blue-white. The brighte ...
... A star is a luminous globe of gas producing its own heat and light by nuclear reactions (nuclear fusion). They are born from nebulae and consist mostly of hydrogen and helium gas. Surface temperatures range from 2000C to above 30,000C, and the corresponding colors from red to blue-white. The brighte ...
HOMEWORK #1
... The figure below shows the lightcurve of the star HD 179070 as an orbiting exoplanet transits in front of the star every 2.785755 days and eclipses some of the star’s brightness. From the star’s spectrum, we know the star has a mass of 1.3 MSun and a radius of 1.9 RSun. Based on the relative amount ...
... The figure below shows the lightcurve of the star HD 179070 as an orbiting exoplanet transits in front of the star every 2.785755 days and eclipses some of the star’s brightness. From the star’s spectrum, we know the star has a mass of 1.3 MSun and a radius of 1.9 RSun. Based on the relative amount ...
HOMEWORK #1
... The figure below shows the lightcurve of the star HD 179070 as an orbiting exoplanet transits in front of the star every 2.785755 days and eclipses some of the star’s brightness. From the star’s spectrum, we know the star has a mass of 1.3 MSun and a radius of 1.9 RSun. Based on the relative amount ...
... The figure below shows the lightcurve of the star HD 179070 as an orbiting exoplanet transits in front of the star every 2.785755 days and eclipses some of the star’s brightness. From the star’s spectrum, we know the star has a mass of 1.3 MSun and a radius of 1.9 RSun. Based on the relative amount ...
MASS – LUMINOSITY RELATION FOR MASSIVE STARS
... Near the stellar surface we have Mr ≈ M and Lr ≈ L, and adopting κ ≈ κe = const, we may integrate equation (s2.3) to obtain ...
... Near the stellar surface we have Mr ≈ M and Lr ≈ L, and adopting κ ≈ κe = const, we may integrate equation (s2.3) to obtain ...
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.