Activity: Stellar Evolution Scavenger Hunt - Chandra X
... Cassiopeia A is the youngest supernova remnant in our Milky Way Galaxy, believed to be the leftovers of a massive star that exploded over 300 years ago. The material ejected during the supernova smashed into the surrounding gas and dust at about 16 million kilometres per hour. This collision superhe ...
... Cassiopeia A is the youngest supernova remnant in our Milky Way Galaxy, believed to be the leftovers of a massive star that exploded over 300 years ago. The material ejected during the supernova smashed into the surrounding gas and dust at about 16 million kilometres per hour. This collision superhe ...
Homework #2
... Type Ia supernovae discussed so far in class). At what distance, in parsecs, would that supernova have a brightness equal to that of the sun? At what distance would it be 10 times fainter than the sun? Compare that to the distance to the nearest star, Alpha Centauri. (nb. 1 AU = 1/206265 pc). This i ...
... Type Ia supernovae discussed so far in class). At what distance, in parsecs, would that supernova have a brightness equal to that of the sun? At what distance would it be 10 times fainter than the sun? Compare that to the distance to the nearest star, Alpha Centauri. (nb. 1 AU = 1/206265 pc). This i ...
Luminosity
... per second. Sun has a luminosity of 3.90x1026 W (often written as L): it emits 3.90x1026 joules per second in all directions. The energy that arrives at the Earth is only a very small amount when compared will the total energy released by the Sun. ...
... per second. Sun has a luminosity of 3.90x1026 W (often written as L): it emits 3.90x1026 joules per second in all directions. The energy that arrives at the Earth is only a very small amount when compared will the total energy released by the Sun. ...
Solution Key
... This is a reasonable value (which is good since the data was taken from a real paper in the Astrophysical Journal). Globular clusters hang out surrounding the center of our galaxy, outside the galactic plane. We are around 8.5 kpc from the galactic center, so it makes sense that a globular cluster s ...
... This is a reasonable value (which is good since the data was taken from a real paper in the Astrophysical Journal). Globular clusters hang out surrounding the center of our galaxy, outside the galactic plane. We are around 8.5 kpc from the galactic center, so it makes sense that a globular cluster s ...
Astronomy
... ___________ are hot, compact remnant stars whose mass is typically between one and several times that of the Sun, but their size is only 10 km or less. A. White dwarfs B. Neutron stars C. Pulsars D. Black dwarfs ...
... ___________ are hot, compact remnant stars whose mass is typically between one and several times that of the Sun, but their size is only 10 km or less. A. White dwarfs B. Neutron stars C. Pulsars D. Black dwarfs ...
Chapter 4. Orbits
... This means that they are almost not moving at all when at their aphelion points and it turns out that those points are generally way beyond the orbit of Pluto and as much as 1/3 of the way to the nearest star! Nonetheless, the comets do not have hyperbolic orbits, which is the case one gets if the t ...
... This means that they are almost not moving at all when at their aphelion points and it turns out that those points are generally way beyond the orbit of Pluto and as much as 1/3 of the way to the nearest star! Nonetheless, the comets do not have hyperbolic orbits, which is the case one gets if the t ...
File
... million K, the surface would be liquid form, while if it's cooler than that, it would be solid. Below that is a solid crust, about a kilometer thick. This crust is very hard and very smooth. Gravity would probably prevent any irregularities larger than half a centimeter. ...
... million K, the surface would be liquid form, while if it's cooler than that, it would be solid. Below that is a solid crust, about a kilometer thick. This crust is very hard and very smooth. Gravity would probably prevent any irregularities larger than half a centimeter. ...
Study Guide for 3RD Astronomy Exam
... Interpret stellar apparent magnitudes and their relationship to brightness Interpret stellar absolute magnitudes and their relationship to luminosity Solve problems relating to the relative brightness or luminosity of two stars given their m or M values. Determine the hottest and coolest stars from ...
... Interpret stellar apparent magnitudes and their relationship to brightness Interpret stellar absolute magnitudes and their relationship to luminosity Solve problems relating to the relative brightness or luminosity of two stars given their m or M values. Determine the hottest and coolest stars from ...
Reach_for_the_stars_final_questions.doc
... 13. For the sake of convenience, astronomers have divided the sky into 88 constellations. In which of these does the current Polar star, Polaris, lie? (1pt) ...
... 13. For the sake of convenience, astronomers have divided the sky into 88 constellations. In which of these does the current Polar star, Polaris, lie? (1pt) ...
powerpoint
... NEBULA (cloud of gas and dust)… aka the STELLAR NURSERY • The nebula begins to contract due to gravity in response to some interstellar disturbance • One or more PROTOSTARS are formed ...
... NEBULA (cloud of gas and dust)… aka the STELLAR NURSERY • The nebula begins to contract due to gravity in response to some interstellar disturbance • One or more PROTOSTARS are formed ...
Published by the Association Pro ISSI No. 37, May 2016
... The helium produced in the first fusion step now starts to fuse into carbon. This gives the core a short reprieve from further collapse. Once the helium inventory is spent, the star contracts, leaving behind a small, hot and dense ball called a White Dwarf. The shock ...
... The helium produced in the first fusion step now starts to fuse into carbon. This gives the core a short reprieve from further collapse. Once the helium inventory is spent, the star contracts, leaving behind a small, hot and dense ball called a White Dwarf. The shock ...
iptfsummer2014bildsten
... • Secular stability requires that the donor star stay within the Roche radius as mass is lost. • If not stable, then likely some excitement. . ...
... • Secular stability requires that the donor star stay within the Roche radius as mass is lost. • If not stable, then likely some excitement. . ...
Great Migrations & other natural history tales
... (the work on MRI is ongoing… also on whether the disks have sufficient ionization for MRI). ...
... (the work on MRI is ongoing… also on whether the disks have sufficient ionization for MRI). ...
AST 301 Test #3 Friday Nov. 12 Name: 1. a) The Sun is in
... 1. a) The Sun is in hydrostatic equilibrium. What does this mean? What is the definition of hydrostatic equilibrium as we apply it to the Sun? Pressure inside the star pushing it apart balances gravity pulling it together. So it doesn’t change its size. 1. a) The Sun is in thermal equilibrium. What ...
... 1. a) The Sun is in hydrostatic equilibrium. What does this mean? What is the definition of hydrostatic equilibrium as we apply it to the Sun? Pressure inside the star pushing it apart balances gravity pulling it together. So it doesn’t change its size. 1. a) The Sun is in thermal equilibrium. What ...
kd - The HST Treasury Program on Eta Carinae
... favors this type of model rather than an eclipse [8]. At least part of the detected emission came from the primary (Fig. 2). In a normal eclipse model, that fraction of the FUV should have remained visible during the event. But it disappeared; the simplest interpretation is a mass-ejection model. Th ...
... favors this type of model rather than an eclipse [8]. At least part of the detected emission came from the primary (Fig. 2). In a normal eclipse model, that fraction of the FUV should have remained visible during the event. But it disappeared; the simplest interpretation is a mass-ejection model. Th ...
Scientific Justification
... underestimate the true ages. A typical white dwarf with a mass of 0.6 M¯ will begin to crystallize when it reaches Teff ∼ 6000-8000 K, depending on the core composition. More massive white dwarfs have higher central pressures, so they can begin to crystallize at higher temperatures. Prior to the Slo ...
... underestimate the true ages. A typical white dwarf with a mass of 0.6 M¯ will begin to crystallize when it reaches Teff ∼ 6000-8000 K, depending on the core composition. More massive white dwarfs have higher central pressures, so they can begin to crystallize at higher temperatures. Prior to the Slo ...
Test 1, Feb. 2, 2016 - Brock physics
... (b) As the star spins, beams of radiation from it sweep through space. If one of these beams points towards the Earth, we observe a pulse. (c) The star vibrates. (d) The star undergoes nuclear explosions that generate radio emissions. ...
... (b) As the star spins, beams of radiation from it sweep through space. If one of these beams points towards the Earth, we observe a pulse. (c) The star vibrates. (d) The star undergoes nuclear explosions that generate radio emissions. ...
Document
... The wind is depicted spatially in the color plots, with the hue indicating velocity with respect to an observer on the left, and the brightness of the ink indicating emissivity (scaling as density squared). Note the color scale above the third panel. Under each image is the resulting line profile wi ...
... The wind is depicted spatially in the color plots, with the hue indicating velocity with respect to an observer on the left, and the brightness of the ink indicating emissivity (scaling as density squared). Note the color scale above the third panel. Under each image is the resulting line profile wi ...
Structure of Neutron Stars
... Remember about the difference between baryonic and gravitational masses in the case of neutron stars! ...
... Remember about the difference between baryonic and gravitational masses in the case of neutron stars! ...
charts_set_8
... RS for a 3 MSun object is 9 km. Event horizon: imaginary sphere around object, with radius RS . Event horizon ...
... RS for a 3 MSun object is 9 km. Event horizon: imaginary sphere around object, with radius RS . Event horizon ...
H-R Diagram
... compressed into such a small volume that gravity prevents even light from escaping. Since no light can ever reach your eyes from the collapsed core, it appears black, hence the name. The apparent surface of the black hole is the radius at which light just manages to escape. It is called the event ho ...
... compressed into such a small volume that gravity prevents even light from escaping. Since no light can ever reach your eyes from the collapsed core, it appears black, hence the name. The apparent surface of the black hole is the radius at which light just manages to escape. It is called the event ho ...
PG_Lecture_Dec18_2008
... Ca XIX lines formed at ~10 MK, seen at the “impulsive” stage of a solar flare in 1980 with the BCS on SMM. Upflow vels. ~ 200 km/s Spectrum from upflowing plasma ...
... Ca XIX lines formed at ~10 MK, seen at the “impulsive” stage of a solar flare in 1980 with the BCS on SMM. Upflow vels. ~ 200 km/s Spectrum from upflowing plasma ...
Three types of binary stars.
... Visual binaries – Stars that are far enough apart that they can be seen as separate stars through a telescope. They typically have orbital periods that are hundreds of years long. ...
... Visual binaries – Stars that are far enough apart that they can be seen as separate stars through a telescope. They typically have orbital periods that are hundreds of years long. ...
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.