Luminosity
... sequence? – Normal stars that fuse H to He in their cores fall on the main sequence of an H-R diagram – A star’s mass determines its position along the main sequence (high-mass: luminous and blue; low-mass: faint and red) ...
... sequence? – Normal stars that fuse H to He in their cores fall on the main sequence of an H-R diagram – A star’s mass determines its position along the main sequence (high-mass: luminous and blue; low-mass: faint and red) ...
Stars are made of very hot gas. This gas is mostly hydrogen and
... Their higher temperature causes them to burn their fuel faster this means they will not live as long, only about 10 billion years or so Near the end of their lives, these medium sized stars swell up becoming very large When this happens to the Sun it will grow to engulf even the Earth. Eventually it ...
... Their higher temperature causes them to burn their fuel faster this means they will not live as long, only about 10 billion years or so Near the end of their lives, these medium sized stars swell up becoming very large When this happens to the Sun it will grow to engulf even the Earth. Eventually it ...
What tool do astronomers use to understand the evolution of stars?
... t B M B L A 1 300 300 60 Sun's lifetime ~ 10 billion years = 1010 yr = 10 Gyr. Lifetime of 5 solar mass star is 1010 yr/60 ~ 1010/102 yr = 108 yr = 102106 yr = 100 million yr = 100 Myr This is the age of the star cluster. ...
... t B M B L A 1 300 300 60 Sun's lifetime ~ 10 billion years = 1010 yr = 10 Gyr. Lifetime of 5 solar mass star is 1010 yr/60 ~ 1010/102 yr = 108 yr = 102106 yr = 100 million yr = 100 Myr This is the age of the star cluster. ...
The First Stars - Amazon Web Services
... Most of the stars were a tenth of the mass of the sun. Very few were ten solar masses or more. And then there were the sun-like stars. The more massive a star, the more rapidly it aged. Stars radiate by thermonuclear burning of hydrogen in their cores. A helium nucleus has atomic mass four. It consi ...
... Most of the stars were a tenth of the mass of the sun. Very few were ten solar masses or more. And then there were the sun-like stars. The more massive a star, the more rapidly it aged. Stars radiate by thermonuclear burning of hydrogen in their cores. A helium nucleus has atomic mass four. It consi ...
Sirius Star1 - Emmi
... Canis major represented either a two-headed dog, a dog that was a gift from Zeus to Europa, or Orion’s hunting dog, helping him to fight Taurus. ...
... Canis major represented either a two-headed dog, a dog that was a gift from Zeus to Europa, or Orion’s hunting dog, helping him to fight Taurus. ...
Final Exam Review – December 2015
... 27. According to the H–R diagram, which type of stars have the highest surface temperature? ______________________________ 28. According to the H–R diagram, which type of stars are in spectral class B and have low luminosity? ______________________________ 29. According to the H–R diagram, which typ ...
... 27. According to the H–R diagram, which type of stars have the highest surface temperature? ______________________________ 28. According to the H–R diagram, which type of stars are in spectral class B and have low luminosity? ______________________________ 29. According to the H–R diagram, which typ ...
chapter 7 review questions
... 23. The binding energy of the first level in an atom is 2.210-18 J, and the binding energy of the second energy level is 1.610-18 J. What is the energy of the photon that is emitted if an electron moves from the second level to the first? a. ...
... 23. The binding energy of the first level in an atom is 2.210-18 J, and the binding energy of the second energy level is 1.610-18 J. What is the energy of the photon that is emitted if an electron moves from the second level to the first? a. ...
Where is the Sun in the Milk Way?
... • The monochromaDc flux (Fν) is defined as the quanDty of energy in the spectral range between ν and ν+dν emiced per unit surface, per unit Dme in units of erg s-‐1 cm-‐2. • For a blackbody, ...
... • The monochromaDc flux (Fν) is defined as the quanDty of energy in the spectral range between ν and ν+dν emiced per unit surface, per unit Dme in units of erg s-‐1 cm-‐2. • For a blackbody, ...
Stellar Evolution Simulation
... In this activity, you will be tracing the lifecycle of several different types of stars. First, go onto http://www.planetseed.com/laboratory/virtual-experiment-build-your-own-star. You will want to keep this website open as it lists some terms that you might not be familiar with. Read through the pa ...
... In this activity, you will be tracing the lifecycle of several different types of stars. First, go onto http://www.planetseed.com/laboratory/virtual-experiment-build-your-own-star. You will want to keep this website open as it lists some terms that you might not be familiar with. Read through the pa ...
Astronomy 110 Announcements: 11.1 Properties of Stars
... • Oh, Be A Fine Guy, Kiss Me Spectral types are further broken down to sub-classes by numbers from 0 to 9 (hotter to cooler) Lines in a star’s spectrum correspond to a spectral type that reveals its temperature ...
... • Oh, Be A Fine Guy, Kiss Me Spectral types are further broken down to sub-classes by numbers from 0 to 9 (hotter to cooler) Lines in a star’s spectrum correspond to a spectral type that reveals its temperature ...
4. Massive Stars and HII Regions
... stars via the collapse of a very massive dense cloud; this implies very high mass accretion rates; observationally one should be able to observe massive discs and outflows from those objects; 2) by coalescence of lower mass stars in extremely dense cluster environments; – Observational evidence seem ...
... stars via the collapse of a very massive dense cloud; this implies very high mass accretion rates; observationally one should be able to observe massive discs and outflows from those objects; 2) by coalescence of lower mass stars in extremely dense cluster environments; – Observational evidence seem ...
LAB: Star Classification
... ScienceDaily (Dec. 12, 2008) — Astronomy & Astrophysics is publishing observations of the white dwarf KPD 0005+5106. The team who present these observations show that this white dwarf is among the hottest stars known so far, with a temperature of 200,000º K at its surface. Stars of intermediate mass ...
... ScienceDaily (Dec. 12, 2008) — Astronomy & Astrophysics is publishing observations of the white dwarf KPD 0005+5106. The team who present these observations show that this white dwarf is among the hottest stars known so far, with a temperature of 200,000º K at its surface. Stars of intermediate mass ...
Star Life Cycle Web Activity
... (This is #16 online) What is the relationship between the brightness of a star and the relative size of a star? Explain why. (The bigger the star is the ________________ it is because _________________) ...
... (This is #16 online) What is the relationship between the brightness of a star and the relative size of a star? Explain why. (The bigger the star is the ________________ it is because _________________) ...
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.