Homework No. 2 Solutions
... from a fluorescent light (the long tube type of lights or the new compact ones that are tubes in a spiral shape). Answer questions 3‐6 using this image and the electromagnetic spectrum shown in the Jan 29 lecture on light. Note that an emission line appears as spike in this type of plot. 3. Wh ...
... from a fluorescent light (the long tube type of lights or the new compact ones that are tubes in a spiral shape). Answer questions 3‐6 using this image and the electromagnetic spectrum shown in the Jan 29 lecture on light. Note that an emission line appears as spike in this type of plot. 3. Wh ...
Transcript - Chandra X
... Mira variable stage of evolution. The end products of these stars are located on the white dwarf in the lower left quadrant of the diagram as they are hot but also extremely dim as they are very compact. Slide 15: Omicron Ceti is also known as Mira. Mira is the prototype of all Mira variable stars. ...
... Mira variable stage of evolution. The end products of these stars are located on the white dwarf in the lower left quadrant of the diagram as they are hot but also extremely dim as they are very compact. Slide 15: Omicron Ceti is also known as Mira. Mira is the prototype of all Mira variable stars. ...
Astronomy - Scioly.org
... e. They are fully connective, and never develop a hydrogen shell fusion zone. 53. What type of spectrum does the gas in a planetary nebula produce? a. A continuous spectrum. b. An emission line spectrum. c. An absorption line spectrum. d. An emission line spectrum superimposed on a continuous spectr ...
... e. They are fully connective, and never develop a hydrogen shell fusion zone. 53. What type of spectrum does the gas in a planetary nebula produce? a. A continuous spectrum. b. An emission line spectrum. c. An absorption line spectrum. d. An emission line spectrum superimposed on a continuous spectr ...
Star and Earth Chemistry Lecture Notes (PDF
... range. Neutrinos can only interact with matter by the weak interaction. A particular nucleus may decay by more than one mode. β-decay and the line of stability There is a, N (neutron number) vs. Z (atomic number) backbone of stability. More neutrons are required at higher Z to reduce the coulombic r ...
... range. Neutrinos can only interact with matter by the weak interaction. A particular nucleus may decay by more than one mode. β-decay and the line of stability There is a, N (neutron number) vs. Z (atomic number) backbone of stability. More neutrons are required at higher Z to reduce the coulombic r ...
Stellar Evolution: Evolution: Birth, Life, and Death of Stars
... existing models of Sun’s structure. This process is known as helioseismology Similar vibrations can be observed in other stars: astroseismology ...
... existing models of Sun’s structure. This process is known as helioseismology Similar vibrations can be observed in other stars: astroseismology ...
10.00 points 10.00 points 10.00 points 10.00 points 10.00 points
... Although the Sun's core has a density much greater than rock it is considered a gaseous object because The Sun's high internal temperatures prevent the atoms from bonding together to form a liquid or a solid. A large fraction of the Sun's interior is made of electromagnetic radiation (light). It is ...
... Although the Sun's core has a density much greater than rock it is considered a gaseous object because The Sun's high internal temperatures prevent the atoms from bonding together to form a liquid or a solid. A large fraction of the Sun's interior is made of electromagnetic radiation (light). It is ...
study guide
... • Jupiter and Saturn are still “collapsing” and releasing heat • All have moons • Some are large, most are captured asteroids ...
... • Jupiter and Saturn are still “collapsing” and releasing heat • All have moons • Some are large, most are captured asteroids ...
chapter16StarBirth
... visible light • Observations of infrared light reveal stars on the other side of the cloud ...
... visible light • Observations of infrared light reveal stars on the other side of the cloud ...
Dark matter
... are easy to detect. Light, and objects that emit light, contribute only 4% of the mass/energy content of the universe. ...
... are easy to detect. Light, and objects that emit light, contribute only 4% of the mass/energy content of the universe. ...
Star Spectra - Renton School District
... A star orbited by a large planet will move in a small circle. This will cause its spectrum to be slightly redshifted part of the time and blueshifted at other times. ...
... A star orbited by a large planet will move in a small circle. This will cause its spectrum to be slightly redshifted part of the time and blueshifted at other times. ...
Vasiliki Pavlidou - Center for Particle and Gravitational Astrophysics
... nearby transient (merger between compact objects ?) GLAST detects it as a very bright transient gamma-ray source. Follow up with Cherenkov detectors - high angular resolution. LIGO detects gravitational wave emission; nature of progenitor known at high confidence A success story Low-energy m ...
... nearby transient (merger between compact objects ?) GLAST detects it as a very bright transient gamma-ray source. Follow up with Cherenkov detectors - high angular resolution. LIGO detects gravitational wave emission; nature of progenitor known at high confidence A success story Low-energy m ...
Lecture notes 10
... collide with nuclei. Occasionally they stick, making larger nuclei. If neutron flux is not too great, these heavier nuclei decay before more neutron captures. Technetium (Tc) has no stable isotopes (all decay). But it is found in the atmospheres of giant stars. Most abundant isotope, 99Tc has a half ...
... collide with nuclei. Occasionally they stick, making larger nuclei. If neutron flux is not too great, these heavier nuclei decay before more neutron captures. Technetium (Tc) has no stable isotopes (all decay). But it is found in the atmospheres of giant stars. Most abundant isotope, 99Tc has a half ...
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.