Astro 10 Practice Test 3
... its core, what would we observe if we could look at the star from the outside? a. The intense energy from the `shell hydrogen burning’ would cause it to contract and cool off, moving down and to the left on the H-R diagram. b. This transition doesn’t actually have any visible effect on the surface o ...
... its core, what would we observe if we could look at the star from the outside? a. The intense energy from the `shell hydrogen burning’ would cause it to contract and cool off, moving down and to the left on the H-R diagram. b. This transition doesn’t actually have any visible effect on the surface o ...
Stars, H-R and Life Cycle of Star
... Two astronomers discovered a relationship between the absolute magnitude (real brightness) of a star and its surface temperature. They plotted the data on a graph. ...
... Two astronomers discovered a relationship between the absolute magnitude (real brightness) of a star and its surface temperature. They plotted the data on a graph. ...
Protostars and planets
... TGMC . 10 K as opposed to T ∼ 6000 K for Hi in the diffuse ISM. Random velocities within the cloud are highly supersonic, v ∼ (GM/D)1/2 ∼ 5 km s−1 vs. cs = (1.4kB T /2mH )1/2 ∼ 0.3 km s−1 . Thus it is expected that the random motions dissipate via shocks on a dynamical timescale (Gρ̄)−1/2 ∼ 107 yr, ...
... TGMC . 10 K as opposed to T ∼ 6000 K for Hi in the diffuse ISM. Random velocities within the cloud are highly supersonic, v ∼ (GM/D)1/2 ∼ 5 km s−1 vs. cs = (1.4kB T /2mH )1/2 ∼ 0.3 km s−1 . Thus it is expected that the random motions dissipate via shocks on a dynamical timescale (Gρ̄)−1/2 ∼ 107 yr, ...
The Sun PPT
... The Sun is a star! There are an incredible amount of stars in the universe. Yay! What is a star…? A star is a huge sphere of very hot, glowing gas. Stars produce their own light and energy by a process called nuclear fusion. Fusion happens when lighter elements are forced to become heavier elements ...
... The Sun is a star! There are an incredible amount of stars in the universe. Yay! What is a star…? A star is a huge sphere of very hot, glowing gas. Stars produce their own light and energy by a process called nuclear fusion. Fusion happens when lighter elements are forced to become heavier elements ...
Stars - PAMS-Doyle
... • The nearest galaxy to ours is called the "Sagittarius Dwarf" and it is about 60 000 light years away from our own galaxy (the Milky Way). Assuming we can get a vehicle to reach the speed of light, it would take 60 000 years for a vehicle to travel to this galaxy. • Given current technology, it is ...
... • The nearest galaxy to ours is called the "Sagittarius Dwarf" and it is about 60 000 light years away from our own galaxy (the Milky Way). Assuming we can get a vehicle to reach the speed of light, it would take 60 000 years for a vehicle to travel to this galaxy. • Given current technology, it is ...
solutions
... relationship between absolute magnitude, luminosity, classification, and effective temperature of stars. The diagram was proposed by Ejnar Hertzsprung and Henry Norris Russell in 1910. There are several forms of the Hertzsprung-Russell diagram. The original diagram displayed the spectral type of sta ...
... relationship between absolute magnitude, luminosity, classification, and effective temperature of stars. The diagram was proposed by Ejnar Hertzsprung and Henry Norris Russell in 1910. There are several forms of the Hertzsprung-Russell diagram. The original diagram displayed the spectral type of sta ...
Multiple choice test questions 1, Winter Semester
... 40 degrees above your horizon. Then you must be located at ________. A) latitude 40 degrees north B) latitude 50 degrees south C) latitude 40 degrees south D) longitude 40 degrees 8) During the period each year when we see Mars undergoing apparent retrograde motion in our sky, what is really going o ...
... 40 degrees above your horizon. Then you must be located at ________. A) latitude 40 degrees north B) latitude 50 degrees south C) latitude 40 degrees south D) longitude 40 degrees 8) During the period each year when we see Mars undergoing apparent retrograde motion in our sky, what is really going o ...
3 rd stage of a star`s life = red giant
... The gravity of a passing star or the shock wave from a nearby supernova may cause the nebula to contract. 1. Matter in the gas cloud will begin to come together into a dense region called a protostar. 2. As the protostar continues to condense, it heats up. 3. Eventually, it reaches a critical mass a ...
... The gravity of a passing star or the shock wave from a nearby supernova may cause the nebula to contract. 1. Matter in the gas cloud will begin to come together into a dense region called a protostar. 2. As the protostar continues to condense, it heats up. 3. Eventually, it reaches a critical mass a ...
formation2
... by gravity, it fragments into smaller pockets of gas which go on to form individual stars. • The result is a star cluster. The more massive pockets from massive stars, the less massive form smaller stars, like the Sun ...
... by gravity, it fragments into smaller pockets of gas which go on to form individual stars. • The result is a star cluster. The more massive pockets from massive stars, the less massive form smaller stars, like the Sun ...
CHAPTER 32 1. What is happening inside a star that isn`t happening
... 6. Name each body from our solar system described below. a. Oxygen rich atmosphere and running water ____________________________ b. Thick atmosphere causing the Greenhouse Effect ____________________________ c. ...
... 6. Name each body from our solar system described below. a. Oxygen rich atmosphere and running water ____________________________ b. Thick atmosphere causing the Greenhouse Effect ____________________________ c. ...
Introduction to Astronomy
... How much energy is released? For each kilogram of hydrogen converted to helium, the mass decreases by 7 grams, so the energy released is 6 x 1014 ...
... How much energy is released? For each kilogram of hydrogen converted to helium, the mass decreases by 7 grams, so the energy released is 6 x 1014 ...
Quiz #4 – The Electromagnetic Spectrum and Stars
... The ___________________ will determine the evolutionary course a star will take. ...
... The ___________________ will determine the evolutionary course a star will take. ...
Star project
... • Stars are born when clouds of dust and gas have a gravitational disturbance, like a nearby supernova. Clumps begin to form in the cloud, and compress and heat up. Eventually, a protostar is formed, which is the core of the star. • The protostar heats up so much and collects so much dust and gas th ...
... • Stars are born when clouds of dust and gas have a gravitational disturbance, like a nearby supernova. Clumps begin to form in the cloud, and compress and heat up. Eventually, a protostar is formed, which is the core of the star. • The protostar heats up so much and collects so much dust and gas th ...
Type II supernova
A Type II supernova (plural: supernovae or supernovas) results from the rapid collapse and violent explosion of a massive star. A star must have at least 8 times, and no more than 40–50 times, the mass of the Sun (M☉) for this type of explosion. It is distinguished from other types of supernovae by the presence of hydrogen in its spectrum. Type II supernovae are mainly observed in the spiral arms of galaxies and in H II regions, but not in elliptical galaxies.Stars generate energy by the nuclear fusion of elements. Unlike the Sun, massive stars possess the mass needed to fuse elements that have an atomic mass greater than hydrogen and helium, albeit at increasingly higher temperatures and pressures, causing increasingly shorter stellar life spans. The degeneracy pressure of electrons and the energy generated by these fusion reactions are sufficient to counter the force of gravity and prevent the star from collapsing, maintaining stellar equilibrium. The star fuses increasingly higher mass elements, starting with hydrogen and then helium, progressing up through the periodic table until a core of iron and nickel is produced. Fusion of iron or nickel produces no net energy output, so no further fusion can take place, leaving the nickel-iron core inert. Due to the lack of energy output allowing outward pressure, equilibrium is broken.When the mass of the inert core exceeds the Chandrasekhar limit of about 1.4 M☉, electron degeneracy alone is no longer sufficient to counter gravity and maintain stellar equilibrium. A cataclysmic implosion takes place within seconds, in which the outer core reaches an inward velocity of up to 23% of the speed of light and the inner core reaches temperatures of up to 100 billion kelvin. Neutrons and neutrinos are formed via reversed beta-decay, releasing about 1046 joules (100 foes) in a ten-second burst. The collapse is halted by neutron degeneracy, causing the implosion to rebound and bounce outward. The energy of this expanding shock wave is sufficient to accelerate the surrounding stellar material to escape velocity, forming a supernova explosion, while the shock wave and extremely high temperature and pressure briefly allow for theproduction of elements heavier than iron. Depending on initial size of the star, the remnants of the core form a neutron star or a black hole. Because of the underlying mechanism, the resulting nova is also described as a core-collapse supernova.There exist several categories of Type II supernova explosions, which are categorized based on the resulting light curve—a graph of luminosity versus time—following the explosion. Type II-L supernovae show a steady (linear) decline of the light curve following the explosion, whereas Type II-P display a period of slower decline (a plateau) in their light curve followed by a normal decay. Type Ib and Ic supernovae are a type of core-collapse supernova for a massive star that has shed its outer envelope of hydrogen and (for Type Ic) helium. As a result, they appear to be lacking in these elements.