![Stellar Masses and the Main Sequence](http://s1.studyres.com/store/data/016518583_1-1e00cd42c207e1fc82258406bb580493-300x300.png)
Stellar Masses and the Main Sequence
... ~ 4 × 1033 ergs/sec = Luminosity of the Sun ~ 7 × 1010 cm = Radius of the Sun ~ 6.3 × 1018 ergs/gm = Energy from hydrogen fusion ~ 27 MeV = mass defect for hydrogen fusion ~ 0.7% = percent mass defect for hydrogen fusion ~ 0.75 = fraction of hydrogen (by mass) in the Sun ~ 0.23 = fraction of helium ...
... ~ 4 × 1033 ergs/sec = Luminosity of the Sun ~ 7 × 1010 cm = Radius of the Sun ~ 6.3 × 1018 ergs/gm = Energy from hydrogen fusion ~ 27 MeV = mass defect for hydrogen fusion ~ 0.7% = percent mass defect for hydrogen fusion ~ 0.75 = fraction of hydrogen (by mass) in the Sun ~ 0.23 = fraction of helium ...
Hertzsprung-Russell Diagram
... The Main Sequence At one end, the stars are big, hot and bright. Due to their color and size they are called blue giants, and the very largest are blue supergiants. At the other end they are small, cool and dim and are known as red dwarfs. The sun is right in the middle. ...
... The Main Sequence At one end, the stars are big, hot and bright. Due to their color and size they are called blue giants, and the very largest are blue supergiants. At the other end they are small, cool and dim and are known as red dwarfs. The sun is right in the middle. ...
Document
... II. Arrange the sentences in the correct order, according to the text on page 14. a. The latter has a diameter of almost two billion miles. b. If you counted one star a second it would take you more than thirty thousand years to count 100 billion. c. But, during your lifetime, as always, new stars a ...
... II. Arrange the sentences in the correct order, according to the text on page 14. a. The latter has a diameter of almost two billion miles. b. If you counted one star a second it would take you more than thirty thousand years to count 100 billion. c. But, during your lifetime, as always, new stars a ...
Calculating Main Sequence Lifetimes
... stars having larger magnitudes. Don’t confuse the relative magnitude with absolute magnitude. The relative magnitude measures the brightness of a star as it appears in the sky and it depends on the brightness and on the distance; if we put a star at the distance of 10 Parsec (33 year light), its mag ...
... stars having larger magnitudes. Don’t confuse the relative magnitude with absolute magnitude. The relative magnitude measures the brightness of a star as it appears in the sky and it depends on the brightness and on the distance; if we put a star at the distance of 10 Parsec (33 year light), its mag ...
Activity Sheet: Galaxies and Stars
... Matching: Write the letter of the most appropriate term in the blank before each description. _____ 1. ...
... Matching: Write the letter of the most appropriate term in the blank before each description. _____ 1. ...
Stellar Masses and the Main Sequence
... There is also a mass-radius relation for main-sequence stars. When parameterized via a power law, R ∝ Mξ, ξ ~ 0.57 for masses M > 1 M8, and ξ ~ 0.8 for M < 1 M8. ...
... There is also a mass-radius relation for main-sequence stars. When parameterized via a power law, R ∝ Mξ, ξ ~ 0.57 for masses M > 1 M8, and ξ ~ 0.8 for M < 1 M8. ...
R - AMUSE code
... (which we derived). We know the surface temperature (Teff=5780K) is much smaller than its minimum mean temperature (2×106 K). Thus we make two approximations for the surface boundary conditions: ρM=M, ρ = 0 kg/m3 and T = 0K at r=rs i.e. that the star does have a sharp boundary with the surrounding v ...
... (which we derived). We know the surface temperature (Teff=5780K) is much smaller than its minimum mean temperature (2×106 K). Thus we make two approximations for the surface boundary conditions: ρM=M, ρ = 0 kg/m3 and T = 0K at r=rs i.e. that the star does have a sharp boundary with the surrounding v ...
Formation of Stars
... The evolution of protostars can be traced as an evolutionary track using the HR diagram. An evolutionary track charts the change in a star’s temperature and luminosity with time. ...
... The evolution of protostars can be traced as an evolutionary track using the HR diagram. An evolutionary track charts the change in a star’s temperature and luminosity with time. ...
Lecture 13 - Main Sequence Stars
... • We have been focusing on the properties of stars on the main sequence, but the chemical composition of stars change with time as the star burns hydrogen into helium. • This causes the other properties to change with time and we can track these changes via motion of the star in the HR diagram. ...
... • We have been focusing on the properties of stars on the main sequence, but the chemical composition of stars change with time as the star burns hydrogen into helium. • This causes the other properties to change with time and we can track these changes via motion of the star in the HR diagram. ...
Rachel Henning
... is formed first, this is a cloud of dust and gas made from hydrogen and helium, after equilibrium is achieved and the temperature increases a prostar is formed. After that, it is either a brown dwarf or nuclear fusion begins. ...
... is formed first, this is a cloud of dust and gas made from hydrogen and helium, after equilibrium is achieved and the temperature increases a prostar is formed. After that, it is either a brown dwarf or nuclear fusion begins. ...
Stars and Black Holes: Stars A star is a massive, luminous ball of
... A star is a massive, luminous ball of ____________. A star shines because nuclear fusion in its core releases energy that radiates into space. Although in the sky, stars all appear _____________ they are actually all different colours. The ______________ of a star depends on the amount of energy it ...
... A star is a massive, luminous ball of ____________. A star shines because nuclear fusion in its core releases energy that radiates into space. Although in the sky, stars all appear _____________ they are actually all different colours. The ______________ of a star depends on the amount of energy it ...
8hrdiagram1s
... Size of Stars We can relate the temperature and luminosity to the size with the StefanBoltzmann law L = sAT4 or L = 4pR2sT4 ...
... Size of Stars We can relate the temperature and luminosity to the size with the StefanBoltzmann law L = sAT4 or L = 4pR2sT4 ...
universe_pp_4 - Cobb Learning
... •It’s difficult to see the spiral shape of our galaxy because we’re on the inside ...
... •It’s difficult to see the spiral shape of our galaxy because we’re on the inside ...
1) The following questions refer to the HR diagram
... 22) What happens to the surface temperature and luminosity when a protostar radiatively contracts? A) Its surface temperature remains the same and its luminosity decreases. B) Its surface temperature and luminosity remain the same. C) Its surface temperature decreases and its luminosity increases. D ...
... 22) What happens to the surface temperature and luminosity when a protostar radiatively contracts? A) Its surface temperature remains the same and its luminosity decreases. B) Its surface temperature and luminosity remain the same. C) Its surface temperature decreases and its luminosity increases. D ...
Lectures 10 & 11 powerpoint (stellar formation) [movie below]
... Fusion into Heavier Elements Fusion into elements heavier than C, O: ...
... Fusion into Heavier Elements Fusion into elements heavier than C, O: ...
Stars…Giants, Supergiants, Dwarfs….
... technical terminology for a change in the energy which depends on how close the neighbors are, how many of them there are, what direction they are,…… ...
... technical terminology for a change in the energy which depends on how close the neighbors are, how many of them there are, what direction they are,…… ...
Aspire: Star Life Cycle - Easy Peasy All-in
... Our Sun Vega Sirius B I. Click on the image to start the next activity. ...
... Our Sun Vega Sirius B I. Click on the image to start the next activity. ...
HR DIAGRAM ACTIVITY
... 10. If a star is very hot and very dim it belongs in this category ______________________ 11. If a star is very cool and very bright, it belongs in this category __________________ ...
... 10. If a star is very hot and very dim it belongs in this category ______________________ 11. If a star is very cool and very bright, it belongs in this category __________________ ...
The Hertzsprung-Russell Diagram
... In general the hotter the star is the brighter it will be. Thus you would expect stars of the same size but different temperatures to form a diagonal line called an equal radius line. Equal Radius lines can be added to an H-R diagram ...
... In general the hotter the star is the brighter it will be. Thus you would expect stars of the same size but different temperatures to form a diagonal line called an equal radius line. Equal Radius lines can be added to an H-R diagram ...