Worksheet: Stars and the HR Diagram
... Background: The Hertzsprung-Russell diagram is actually a graph that illustrates the relationship that exists between the average surface temperature of stars and their absolute magnitude, which is how bright they would appear to be if they were al the same distance away. Rather than speak of the br ...
... Background: The Hertzsprung-Russell diagram is actually a graph that illustrates the relationship that exists between the average surface temperature of stars and their absolute magnitude, which is how bright they would appear to be if they were al the same distance away. Rather than speak of the br ...
Life Cycle of a Star
... - Stars are classified by their size, brightness, color, temperature, spectrum and age. ...
... - Stars are classified by their size, brightness, color, temperature, spectrum and age. ...
Astronomy 114 Problem Set # 6 Due: 11 Apr 2007 SOLUTIONS 1
... 1 Why is the temperature of a star’s core so important in determining which nuclear reactions can occur there? Fusion reactions occur when the strong force, the force that binds the neutrons and protons, binds two nuclei in two initially separate atoms. The strong force acts at very short distances. ...
... 1 Why is the temperature of a star’s core so important in determining which nuclear reactions can occur there? Fusion reactions occur when the strong force, the force that binds the neutrons and protons, binds two nuclei in two initially separate atoms. The strong force acts at very short distances. ...
Calculating Main Sequence Lifetimes
... If we remember that the Sun’s mass is 2 × 10 Kg, and knowing the stellar mass, we can calculate the period in which the star burns Hydrogen, which the time it stays as a main sequence star. The star turns off: the star exhausts the Hydrogen in its core and it continues to burn it in shells.. For a ‘ ...
... If we remember that the Sun’s mass is 2 × 10 Kg, and knowing the stellar mass, we can calculate the period in which the star burns Hydrogen, which the time it stays as a main sequence star. The star turns off: the star exhausts the Hydrogen in its core and it continues to burn it in shells.. For a ‘ ...
Stars Powerpoint
... • If the star is massive enough, the collapse will trigger a violent explosion known as a supernova • If the remaining mass of the star is about 1.4 times that of our Sun, the core is unable to support itself and it will collapse further to become a neutron star ...
... • If the star is massive enough, the collapse will trigger a violent explosion known as a supernova • If the remaining mass of the star is about 1.4 times that of our Sun, the core is unable to support itself and it will collapse further to become a neutron star ...
Neutron Stars and Black Holes - School
... Before any evidence of black holes existed they were known to be a theoretical possibility. After a supernova explosion there remains an incredibly dense neutron star. If the mass of the Sun from which it originated was great enough then the neutron star could be a black hole. The gravitational fiel ...
... Before any evidence of black holes existed they were known to be a theoretical possibility. After a supernova explosion there remains an incredibly dense neutron star. If the mass of the Sun from which it originated was great enough then the neutron star could be a black hole. The gravitational fiel ...
Chapter 25 Beyond Our Solar System
... © Pearson Education, Inc., publishing as Pearson Prentice Hall. All rights reserved. ...
... © Pearson Education, Inc., publishing as Pearson Prentice Hall. All rights reserved. ...
SOLUTIONS ASTROPHYSICS – OPTION D 2015-17
... Stellar Evolution Review pp. 521-522 Questions 1. Describe the evolution of a main sequence star of 1 solar mass. See table - ...
... Stellar Evolution Review pp. 521-522 Questions 1. Describe the evolution of a main sequence star of 1 solar mass. See table - ...
Life Cycle of a Star
... The color of a star is dependant on its temperature. Astronomers measure the temperature of each star by its outer most layer or its photosphere. O stars, which are the hottest of the seven categories, are blue in color. M stars, which are the coolest, are red. Within the range of this spectrum, the ...
... The color of a star is dependant on its temperature. Astronomers measure the temperature of each star by its outer most layer or its photosphere. O stars, which are the hottest of the seven categories, are blue in color. M stars, which are the coolest, are red. Within the range of this spectrum, the ...
Name: Period: ______ Date: Light/Astronomy Study Guide What are
... 17. What process fuels a star, and what are the process that cause it to die? The fusion of hydrogen in to helium fuels a star (balance between explosion outwards, and gravity inwards) and when this fuel runs out, the star begins to die. 18. Where/when are the following elements created: a. Light el ...
... 17. What process fuels a star, and what are the process that cause it to die? The fusion of hydrogen in to helium fuels a star (balance between explosion outwards, and gravity inwards) and when this fuel runs out, the star begins to die. 18. Where/when are the following elements created: a. Light el ...
30-2 Directed Reading
... c. the main-sequence stage d. the nebula stage _____ 16. A star that has the same mass as the sun’s mass a. stays on the main sequence for about 10 million years. b. stays on the main sequence for about 10 billion years. c. stays on the main sequence for about 14 billion years. d. stays on the main ...
... c. the main-sequence stage d. the nebula stage _____ 16. A star that has the same mass as the sun’s mass a. stays on the main sequence for about 10 million years. b. stays on the main sequence for about 10 billion years. c. stays on the main sequence for about 14 billion years. d. stays on the main ...
HW2 due - Yale Astronomy
... Sirius A, the brightest star in the sky. Sirius B has a radius of 0.0084 Rsun and a luminosity of 0.026 Lsun. a.) What is its surface temperature? b.) At what wavelength would ...
... Sirius A, the brightest star in the sky. Sirius B has a radius of 0.0084 Rsun and a luminosity of 0.026 Lsun. a.) What is its surface temperature? b.) At what wavelength would ...
Theoretical Problem 3
... 5. The mass and radius of the smallest star. The result found in (4a) suggests that there could be stars of any mass as long as such a relationship is fulfilled; however, this is not true. The gas inside normal stars fusing hydrogen is known to behave approximately as an ideal gas. This means that d ...
... 5. The mass and radius of the smallest star. The result found in (4a) suggests that there could be stars of any mass as long as such a relationship is fulfilled; however, this is not true. The gas inside normal stars fusing hydrogen is known to behave approximately as an ideal gas. This means that d ...
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.