![12.748 Lecture 2 Cosmic Abundances, Nucleosynthesis and](http://s1.studyres.com/store/data/017352777_1-964c7b87b7d390bed9726246dbde8012-300x300.png)
12.748 Lecture 2 Cosmic Abundances, Nucleosynthesis and
... If the star is sufficiently massive, say greater than three solar masses, not even the rigidity of the neutrons is enough to hold gravity back. The thing that gives the neutrons their rigidity is not what you might think: is is the quantum mechanical resistance to having more than one particle in th ...
... If the star is sufficiently massive, say greater than three solar masses, not even the rigidity of the neutrons is enough to hold gravity back. The thing that gives the neutrons their rigidity is not what you might think: is is the quantum mechanical resistance to having more than one particle in th ...
The Birth of Stars Guiding Questions • Because stars shine by
... 5. When a star forms, why does it end up with only a fraction of the available matter? 6. What do star clusters tell us about the formation of stars? 7. Where in the Galaxy does star formation take place? 8. How can the death of one star trigger the birth of many other stars? ...
... 5. When a star forms, why does it end up with only a fraction of the available matter? 6. What do star clusters tell us about the formation of stars? 7. Where in the Galaxy does star formation take place? 8. How can the death of one star trigger the birth of many other stars? ...
The Birth of Stars
... 5. When a star forms, why does it end up with only a fraction of the available matter? 6. What do star clusters tell us about the formation of stars? 7. Where in the Galaxy does star formation take place? 8. How can the death of one star trigger the birth of many other stars? ...
... 5. When a star forms, why does it end up with only a fraction of the available matter? 6. What do star clusters tell us about the formation of stars? 7. Where in the Galaxy does star formation take place? 8. How can the death of one star trigger the birth of many other stars? ...
Stages - A Summary - University of Dayton
... Slight contraction over millions of years finally results in a perfect, continued balance between outward luminosity and inward gravity. Our star has reached the Zero Age Main Sequence, where it will stay for over 90% of its life, virtually unchanged externally. [Note : Stars of different masses exp ...
... Slight contraction over millions of years finally results in a perfect, continued balance between outward luminosity and inward gravity. Our star has reached the Zero Age Main Sequence, where it will stay for over 90% of its life, virtually unchanged externally. [Note : Stars of different masses exp ...
F p = Fraction of good stars with planets
... fP = Fraction of good stars with planets ne = number of planets per star in ecoshell fl = fraction of planets on which life develops fi = fraction that develop intelligence fc = fraction that reach electromagnetic ...
... fP = Fraction of good stars with planets ne = number of planets per star in ecoshell fl = fraction of planets on which life develops fi = fraction that develop intelligence fc = fraction that reach electromagnetic ...
Stars - HMXEarthScience
... 1. Large clouds of dust and gas are pulled together by gravity (these clouds are called nebulae) 2. Gases in the nebula contract due to gravity, resulting in the formation of a protostar. 3. Pressure and temperature increase until the gases “ignite” and nuclear fusion begins 4. Once the star has ful ...
... 1. Large clouds of dust and gas are pulled together by gravity (these clouds are called nebulae) 2. Gases in the nebula contract due to gravity, resulting in the formation of a protostar. 3. Pressure and temperature increase until the gases “ignite” and nuclear fusion begins 4. Once the star has ful ...
Star in a Box Worksheet - Beginning with solutions
... 4. In which stage of its life does the Sun spend the longest time? The Sun spends the most time on the main sequence. 5. In which stage of life will the Sun undergo the most change? T he Sun undergoes the most change in size, luminosity and temperature between the two asymptotic giant branches. 6 ...
... 4. In which stage of its life does the Sun spend the longest time? The Sun spends the most time on the main sequence. 5. In which stage of life will the Sun undergo the most change? T he Sun undergoes the most change in size, luminosity and temperature between the two asymptotic giant branches. 6 ...
LESSON 4, STARS
... red giant, and finally, a white dwarf. A more-massive star: begins as a nebula, becomes a protostar, a main-sequence star, a very massive star, a supergiant, a supernova, and finally, either a neutron star (pulsar) or a black hole. ...
... red giant, and finally, a white dwarf. A more-massive star: begins as a nebula, becomes a protostar, a main-sequence star, a very massive star, a supergiant, a supernova, and finally, either a neutron star (pulsar) or a black hole. ...
About SDSS - Astro Projects
... SDSS mainly imaged the area around the North Galactic Pole (RA = 193 deg, Dec = 27 deg). This is a point directly 'above' our position in the Milky Way Galaxy. Because of this the survey includes hardly any supernova remnants or planetary nebulae. This is because these objects are remnants of dead s ...
... SDSS mainly imaged the area around the North Galactic Pole (RA = 193 deg, Dec = 27 deg). This is a point directly 'above' our position in the Milky Way Galaxy. Because of this the survey includes hardly any supernova remnants or planetary nebulae. This is because these objects are remnants of dead s ...
Steve Holmes - KWFN October 22 2012 speaker
... supernova is the end-of-life explosion of a large star. This explosion occurs within a matter of seconds, and appears as a major brightening that fades out over several weeks or months. The event sends out a high-speed shock wave that is visible as a supernova remnant: a shell-like dust cloud that e ...
... supernova is the end-of-life explosion of a large star. This explosion occurs within a matter of seconds, and appears as a major brightening that fades out over several weeks or months. The event sends out a high-speed shock wave that is visible as a supernova remnant: a shell-like dust cloud that e ...
Chapter 19 Star Formation
... to begin. They gradually cool off and become dark “clinkers.” A protostar must have 0.08 the mass of the Sun (which is 80 times the mass of Jupiter) in order to become dense and hot enough that fusion can begin. If the mass of the “failed star” is about 12 Jupiter masses or more, it is luminous when ...
... to begin. They gradually cool off and become dark “clinkers.” A protostar must have 0.08 the mass of the Sun (which is 80 times the mass of Jupiter) in order to become dense and hot enough that fusion can begin. If the mass of the “failed star” is about 12 Jupiter masses or more, it is luminous when ...
Solutions
... for the Milky Way and Andromeda galaxies, only using frisbees or dinner plates to represent the disks of these Galaxies. Comment on what this says about how often you might expect to see galaxy/galaxy collisions in the Universe compared to star/star collisions in our Galaxy. (For the size of our Gal ...
... for the Milky Way and Andromeda galaxies, only using frisbees or dinner plates to represent the disks of these Galaxies. Comment on what this says about how often you might expect to see galaxy/galaxy collisions in the Universe compared to star/star collisions in our Galaxy. (For the size of our Gal ...
Astro 1 & 100 Levine Homework Stars Name:____________________________
... 7. Draw a line to represent the main sequence. (2 points) 8. Mark the location of the Sun and label it (it’s a G-type star). (2 points) ...
... 7. Draw a line to represent the main sequence. (2 points) 8. Mark the location of the Sun and label it (it’s a G-type star). (2 points) ...
Chapter 12. Basic Equations of Stellar Structure
... Earth could not have been around form more than 20 million years or so and there certainly could not have been life on this planet for longer than that, since life requires sunlight to exist. The geologists and biologists of that era were sure, however, that the slow processes of geologic and biolog ...
... Earth could not have been around form more than 20 million years or so and there certainly could not have been life on this planet for longer than that, since life requires sunlight to exist. The geologists and biologists of that era were sure, however, that the slow processes of geologic and biolog ...
Homework 5
... In Shu 5.11 you computed how long it takes a photon to leak out of the sun. This is comparable to the time it would take all the radiant energy inside the sun to escape. As you’ve just shown, there’s much more energy than this present in the plasma, in the form of the kinetic energy of the particles ...
... In Shu 5.11 you computed how long it takes a photon to leak out of the sun. This is comparable to the time it would take all the radiant energy inside the sun to escape. As you’ve just shown, there’s much more energy than this present in the plasma, in the form of the kinetic energy of the particles ...
Spectroscopy Lecture 10
... – Found Sirius B at Northwestern’s Dearborn Observatory Procyon B found in 1895 at Lick – Was it a star that had cooled and dimmed? Spectrum of 40 Eri B observed – an A star! – It must be hot – Must have small radius to be so faint – The first “w hite dwarf” Adams found Sirius B is also an A star ...
... – Found Sirius B at Northwestern’s Dearborn Observatory Procyon B found in 1895 at Lick – Was it a star that had cooled and dimmed? Spectrum of 40 Eri B observed – an A star! – It must be hot – Must have small radius to be so faint – The first “w hite dwarf” Adams found Sirius B is also an A star ...
SupernovaExplosionPhysics_8pages
... the remainder resulting from subsequent steps. 5. The collapse ends when the core reaches nuclear density. Actually, the density exceeds nuclear briefly by what is estimated to be a factor of 2 to 3. This is discussed with some more detail in Section 4.3 below. 6. The core now strongly bounces back ...
... the remainder resulting from subsequent steps. 5. The collapse ends when the core reaches nuclear density. Actually, the density exceeds nuclear briefly by what is estimated to be a factor of 2 to 3. This is discussed with some more detail in Section 4.3 below. 6. The core now strongly bounces back ...
Lab 9
... such a way that the apparent size of a galaxy is related to its distance from Earth. This is method similar to the main-sequence fitting we did in an earlier exercise for star clusters. Figure 8.1 shows the images and visible spectra of five elliptical galaxies. The spectrum of each galaxy is shown ...
... such a way that the apparent size of a galaxy is related to its distance from Earth. This is method similar to the main-sequence fitting we did in an earlier exercise for star clusters. Figure 8.1 shows the images and visible spectra of five elliptical galaxies. The spectrum of each galaxy is shown ...
The Family of Stars
... The flux received from both stars is the same, but star B is 5 times more luminous than star A, so star B must be further away. The flux received from both stars is the same, but star B is 100 times more luminous than star A, so star B must be further away. Both stars are equally luminous, but the f ...
... The flux received from both stars is the same, but star B is 5 times more luminous than star A, so star B must be further away. The flux received from both stars is the same, but star B is 100 times more luminous than star A, so star B must be further away. Both stars are equally luminous, but the f ...