Goal: To understand the lifetime of a star and how the
... • 4 protons have more mass than 1 Helium atom. • So, when you fuse protons into helium, you loose mass. • Mass is a form of energy. • Once again, energy is always conserved! • So, you gain energy (in forms of photons and neutrinos). ...
... • 4 protons have more mass than 1 Helium atom. • So, when you fuse protons into helium, you loose mass. • Mass is a form of energy. • Once again, energy is always conserved! • So, you gain energy (in forms of photons and neutrinos). ...
interactive.hr.diagram
... To receive credit, you must answer in complete sentences! Don’t be afraid to think! 1) What is plotted along the horizontal axis of an H-R Diagram? ...
... To receive credit, you must answer in complete sentences! Don’t be afraid to think! 1) What is plotted along the horizontal axis of an H-R Diagram? ...
Astronomy 112: The Physics of Stars Class 9 Notes: Polytropes With
... dm and thickness dr, which is at a distance r from the center of the star and has a mass m interior to it. The shell has density ρ, pressure P , temperature T , and opacity κ. The radiation flux passing through it is F , and the shell generates energy via nuclear reactions at a rate per unit mass q. ...
... dm and thickness dr, which is at a distance r from the center of the star and has a mass m interior to it. The shell has density ρ, pressure P , temperature T , and opacity κ. The radiation flux passing through it is F , and the shell generates energy via nuclear reactions at a rate per unit mass q. ...
Deep HST Imaging of M33: Reliability and Recovery of the Star
... • Integrated SFH is not exponentially declining, SFR has been roughly constant, or even increased in past several Gyr ...
... • Integrated SFH is not exponentially declining, SFR has been roughly constant, or even increased in past several Gyr ...
Rotational spin-up in the 30-Myr
... one of the fundamental quantities, like mass and metallicity, defining the star’s properties and evolution. Rotation influences the star’s internal structure and the mixing processes in the stellar interior that are reflected in surface elemental abundances. It is also the main driver for magnetic a ...
... one of the fundamental quantities, like mass and metallicity, defining the star’s properties and evolution. Rotation influences the star’s internal structure and the mixing processes in the stellar interior that are reflected in surface elemental abundances. It is also the main driver for magnetic a ...
Life Cycle of a Star
... The Universe is believed to have been formed from a very dense fireball _____________ of years ago. As the fireball expanded and cooled stars and galaxies formed. The fireball explosion is often called the ___ ________. The explosion threw all the material outwards; that is why scientists believe th ...
... The Universe is believed to have been formed from a very dense fireball _____________ of years ago. As the fireball expanded and cooled stars and galaxies formed. The fireball explosion is often called the ___ ________. The explosion threw all the material outwards; that is why scientists believe th ...
5Stars_Part_Two
... 3. Neutron stars are the size of towns. 4. Some Neutron stars spin a thousand times a second. 5. The pressure is so high in the core atomic nuclei cannot exist. 6. The outer envelope is about a mile thick - a crust of nuclei and electrons. 7. The core is a super-fluid. ...
... 3. Neutron stars are the size of towns. 4. Some Neutron stars spin a thousand times a second. 5. The pressure is so high in the core atomic nuclei cannot exist. 6. The outer envelope is about a mile thick - a crust of nuclei and electrons. 7. The core is a super-fluid. ...
Section 14
... If the white dwarf is part of a system of two or more stars, it can lead to an interesting effect. As the non-white dwarf star produces energy, it is also emitting mass. This mass can accumulate on the surface of the white dwarf. If enough mass accumulates, it can lead to fusion processes within it ...
... If the white dwarf is part of a system of two or more stars, it can lead to an interesting effect. As the non-white dwarf star produces energy, it is also emitting mass. This mass can accumulate on the surface of the white dwarf. If enough mass accumulates, it can lead to fusion processes within it ...
Mass and Age determination for low
... model comparison), giving as observational constraints effective ...
... model comparison), giving as observational constraints effective ...
Low mass stars
... just have to measure the magnitudes of the stars and then calculate the luminosity. This was done for lots of binary star systems, and the resulting data plotted (Luminosity as a function of Mass). The resulting correlation is only really valid for Main Sequence stars! When the observed masses and l ...
... just have to measure the magnitudes of the stars and then calculate the luminosity. This was done for lots of binary star systems, and the resulting data plotted (Luminosity as a function of Mass). The resulting correlation is only really valid for Main Sequence stars! When the observed masses and l ...
Stars: Their Life and Afterlife
... overcome the electron degeneracy pressure, and the star would contract and heat to the point where further fusion – and evolution – were possible. Second, at about this mass a process called “neutronization” becomes possible: the most energetic electrons in the gas would have enough energy to bind w ...
... overcome the electron degeneracy pressure, and the star would contract and heat to the point where further fusion – and evolution – were possible. Second, at about this mass a process called “neutronization” becomes possible: the most energetic electrons in the gas would have enough energy to bind w ...
Lecture 13 - Star Formation
... • Space between the stars within a galaxy is not empty. • The interstellar medium (ISM) consists of gas and dust. • Gas is mainly hydrogen, but also contains other elements and molecules. • Density is typically around 1 atom per cubic centimeter. ...
... • Space between the stars within a galaxy is not empty. • The interstellar medium (ISM) consists of gas and dust. • Gas is mainly hydrogen, but also contains other elements and molecules. • Density is typically around 1 atom per cubic centimeter. ...
Ch. 20
... will destroy the integrity of the work and is not permitted. The work and materials from it should never be made available to students except by instructors using the accompanying text in their classes. All recipients of this work are expected to abide by these restrictions and to honor the intended ...
... will destroy the integrity of the work and is not permitted. The work and materials from it should never be made available to students except by instructors using the accompanying text in their classes. All recipients of this work are expected to abide by these restrictions and to honor the intended ...
Gravity simplest fusion
... • When a neutron star forms, the pull of gravity is so great that it overrides the electron degeneracy pressure of the atoms of the star. • The electrons are forced into their respective nuclei, where they combine with protons to form neutrons. This greatly decreases the size of each atom, and allow ...
... • When a neutron star forms, the pull of gravity is so great that it overrides the electron degeneracy pressure of the atoms of the star. • The electrons are forced into their respective nuclei, where they combine with protons to form neutrons. This greatly decreases the size of each atom, and allow ...
galaxies - GEOCITIES.ws
... – If a star has between 1.4 and 9 solar masses, it will become a neutron star. – A neutron star is a star made entirely of neutrons, as the name suggests. After a star goes supernova, the remaining core collapses. Gravity shrinks and condenses it into a sphere about the size of Manhattan (fifteen mi ...
... – If a star has between 1.4 and 9 solar masses, it will become a neutron star. – A neutron star is a star made entirely of neutrons, as the name suggests. After a star goes supernova, the remaining core collapses. Gravity shrinks and condenses it into a sphere about the size of Manhattan (fifteen mi ...
Stellar Stability and the Chandrasekhar Limit
... object which is produced when a low to medium mass star dies. These stars are not heavy enough to generate the core temperatures required to fuse carbon in nucleosynthesis reactions. After one has become a red giant during its helium-burning phase, it will shed its outer layers to form a planetary n ...
... object which is produced when a low to medium mass star dies. These stars are not heavy enough to generate the core temperatures required to fuse carbon in nucleosynthesis reactions. After one has become a red giant during its helium-burning phase, it will shed its outer layers to form a planetary n ...
Stars and Stellar Evolution The Hertzsprung
... enter an excited state and then jump down to the ground state emitting visible photons. This process is known as fluorescence. ...
... enter an excited state and then jump down to the ground state emitting visible photons. This process is known as fluorescence. ...
How are galaxies classified
... A: If the star is massive enough, the collapse of the star will trigger a violent explosion known as a supernova. A: Supernovas are very bright and can cause a brief (few months) burst of radiation that can outshine an entire galaxy. A: During this explosion, a supernova can give off as much energy ...
... A: If the star is massive enough, the collapse of the star will trigger a violent explosion known as a supernova. A: Supernovas are very bright and can cause a brief (few months) burst of radiation that can outshine an entire galaxy. A: During this explosion, a supernova can give off as much energy ...
Chapter 9 powerpoint presentation
... where ’ is the vertical optical depth. The frequency dependence in is taken care of by the Rossland Mean opacity. Take two moments of the R.T.E. which means integrate over solid angle, d, to get the first moment. Then multiply by Cos and integrate again to get the second moment. After some al ...
... where ’ is the vertical optical depth. The frequency dependence in is taken care of by the Rossland Mean opacity. Take two moments of the R.T.E. which means integrate over solid angle, d, to get the first moment. Then multiply by Cos and integrate again to get the second moment. After some al ...
Stellar Evolution after the Main Sequence
... Stellar Evolution after the Main Sequence Low Mass Stars ...
... Stellar Evolution after the Main Sequence Low Mass Stars ...
Microsoft Word - LifeCycleInteractive
... Star Quiz (Part 2) 21. Why does the outer shell of the star expand? 22. As the outer shell of the star expands, the surface temperature of the star decreases. Helium burning is much hotter than hydrogen burning. Why would the surface temperature decrease? Close quiz window. 23. The red giant is the ...
... Star Quiz (Part 2) 21. Why does the outer shell of the star expand? 22. As the outer shell of the star expands, the surface temperature of the star decreases. Helium burning is much hotter than hydrogen burning. Why would the surface temperature decrease? Close quiz window. 23. The red giant is the ...