Star Formation
... object with an accretion disk and jets 4) When the young stellar object begins fusing hydrogen into helium it becomes a true star ...
... object with an accretion disk and jets 4) When the young stellar object begins fusing hydrogen into helium it becomes a true star ...
luminosity1
... given element is in a star. • HD 161817 has much less of all the elements, other than Hydrogen and Helium, than the Sun. • In fact, it has about 0.03 the value of the Sun for all 90 elements. That is 3% the amount in the Sun. The most deficient star known has about 0.001% the Sun. • There are also s ...
... given element is in a star. • HD 161817 has much less of all the elements, other than Hydrogen and Helium, than the Sun. • In fact, it has about 0.03 the value of the Sun for all 90 elements. That is 3% the amount in the Sun. The most deficient star known has about 0.001% the Sun. • There are also s ...
A little bit more to do. Stefan
... given element is in a star. • HD 161817 has much less of all the elements, other than Hydrogen and Helium, than the Sun. • In fact, it has about 0.03 the value of the Sun for all 90 elements. That is 3% the amount in the Sun. The most deficient star known has about 0.001% the Sun. • There are also s ...
... given element is in a star. • HD 161817 has much less of all the elements, other than Hydrogen and Helium, than the Sun. • In fact, it has about 0.03 the value of the Sun for all 90 elements. That is 3% the amount in the Sun. The most deficient star known has about 0.001% the Sun. • There are also s ...
Star Formation, HR Diagram, and the Main Sequence (Professor
... As the core heats up, H fusion runs faster: Core temperature rises Core pressure rises Collapse begins to slow down If the core temperature reaches at least 10 million deg K, the proto-Star becomes a Star ...
... As the core heats up, H fusion runs faster: Core temperature rises Core pressure rises Collapse begins to slow down If the core temperature reaches at least 10 million deg K, the proto-Star becomes a Star ...
The Hertzsprung-Russell Diagram
... variation of their velocity or brightness. To get orbital semimajor axis, you need either the parallax to a visual system or the velocity from a spectroscopic system. In a spectroscopic system, you only have a lower limit unless you know the system tilt. In an eclipsing system, you know everything, ...
... variation of their velocity or brightness. To get orbital semimajor axis, you need either the parallax to a visual system or the velocity from a spectroscopic system. In a spectroscopic system, you only have a lower limit unless you know the system tilt. In an eclipsing system, you know everything, ...
Powerpoint
... Remember 1" (arcsecond) = 1/60 arcmin = 1/3600 degrees If the angle is 0.5", the distance is 2 pc. ...
... Remember 1" (arcsecond) = 1/60 arcmin = 1/3600 degrees If the angle is 0.5", the distance is 2 pc. ...
Mass-Luminosity Relation for White
... as result, obtain a simple proportionality relation between mass and luminosity. The proportionality constant is fortunately independent of the radius and is a function of chemical composition only. In conclusion, we will show qualitatively that the ratio of mass to luminosity is small when the cen ...
... as result, obtain a simple proportionality relation between mass and luminosity. The proportionality constant is fortunately independent of the radius and is a function of chemical composition only. In conclusion, we will show qualitatively that the ratio of mass to luminosity is small when the cen ...
Lab 8: Stellar Classification and the H
... diagram. The hottest, most luminous stars lie at the upper left of the diagram, and the coolest, dimmest stars lie at the lower right. Note that the stars with lower temperatures are placed on the right-hand side of the HR Diagram, so that temperature increases towards the left. Stars at the upper r ...
... diagram. The hottest, most luminous stars lie at the upper left of the diagram, and the coolest, dimmest stars lie at the lower right. Note that the stars with lower temperatures are placed on the right-hand side of the HR Diagram, so that temperature increases towards the left. Stars at the upper r ...
Chapter 10. Stellar Spectra
... of a Black Body that would have the equivalent flux (watts per square meter) as the star does. Note also that we assume when we write the equation above that the star is spherically symmetric and radiates exactly the same amount of flux in all directions. This is generally true for most normal stars ...
... of a Black Body that would have the equivalent flux (watts per square meter) as the star does. Note also that we assume when we write the equation above that the star is spherically symmetric and radiates exactly the same amount of flux in all directions. This is generally true for most normal stars ...
Hertzsprung-Russell Diagram—7 Oct Outline • Thermal radiation
... • For a person, T=273+37=310K. 2.9mm K 0.01mm 10μm 310K ...
... • For a person, T=273+37=310K. 2.9mm K 0.01mm 10μm 310K ...
Neutron star - SharpSchool
... It is now a main sequence star and shines as nuclear fusion produces heat and light The star may remain in this stage for millions or ...
... It is now a main sequence star and shines as nuclear fusion produces heat and light The star may remain in this stage for millions or ...
Life Cycle of the Stars
... A Star is Born • When the core of the matter becomes hot enough, thermonuclear fusion begins. • This means that there is enough heat to turn hydrogen to helium. • Once this has happened a true star has been born. • The star shines with its own light. • A solar wind then blows away the rest of the d ...
... A Star is Born • When the core of the matter becomes hot enough, thermonuclear fusion begins. • This means that there is enough heat to turn hydrogen to helium. • Once this has happened a true star has been born. • The star shines with its own light. • A solar wind then blows away the rest of the d ...
Document
... elements present in the outer layers of the star Deduce both chemical and physical data about stars Chemical composition and surface temperature Speed and direction of motion using the Doppler Effect If source of waves is moving towards us, their frequency is shifted upwards Stars moving t ...
... elements present in the outer layers of the star Deduce both chemical and physical data about stars Chemical composition and surface temperature Speed and direction of motion using the Doppler Effect If source of waves is moving towards us, their frequency is shifted upwards Stars moving t ...
Study Guide- Tools of Astronomy
... 21. How is star size related to length of life cycle? 22. Use figure 3 to answer the following a. Compare the temperature and brightness of Mira to Rigel. b. Compare the temperature and brightness of Procyon B to Procyon A. c. Compare the temperature and brightness of Achernar to Almach. 23. Why can ...
... 21. How is star size related to length of life cycle? 22. Use figure 3 to answer the following a. Compare the temperature and brightness of Mira to Rigel. b. Compare the temperature and brightness of Procyon B to Procyon A. c. Compare the temperature and brightness of Achernar to Almach. 23. Why can ...
Lailaigib Lifecycle Of A Star
... ighmassstars.html http://astronomyonline.org/Stars/LowMassEvolution.asp ...
... ighmassstars.html http://astronomyonline.org/Stars/LowMassEvolution.asp ...
EVOLUION OF SUN LIKE STAR
... .But later starts to collapse and it started heating up and density becomes high and there starts a fight between pressure forces and gravity .And when this forces are out of balance it stared to collapse and become smaller and smaller parts . The smallest part becomes a protostar .Contraction make ...
... .But later starts to collapse and it started heating up and density becomes high and there starts a fight between pressure forces and gravity .And when this forces are out of balance it stared to collapse and become smaller and smaller parts . The smallest part becomes a protostar .Contraction make ...
Powerpoint for today
... Stars' spectra are roughly those of blackbodies. Color depends on surface temperature. A quantitative measure of “color”, and thus temperature, can be made by observing star through various color filters. See text for how this is done. ...
... Stars' spectra are roughly those of blackbodies. Color depends on surface temperature. A quantitative measure of “color”, and thus temperature, can be made by observing star through various color filters. See text for how this is done. ...
main-sequence stars
... more luminous and have diameters from 10-100 times greater than our sun. Super giants are giant stars that have diameters more than 100 times greater than our sun. These giant stars (but relatively cool) are very luminous. ...
... more luminous and have diameters from 10-100 times greater than our sun. Super giants are giant stars that have diameters more than 100 times greater than our sun. These giant stars (but relatively cool) are very luminous. ...
Stellar Temperature & Luminosity Student Page Purpose
... 1. If the peak in the black body curve of a star is at a longer wavelength than the peak wavelength for our Sun, how does the surface temperature of that star compare to our Sun’s surface temperature? 2. Which of the following events will have the largest effect on a star’s brightness — doubling its ...
... 1. If the peak in the black body curve of a star is at a longer wavelength than the peak wavelength for our Sun, how does the surface temperature of that star compare to our Sun’s surface temperature? 2. Which of the following events will have the largest effect on a star’s brightness — doubling its ...
here
... 5: 0.1 and 100 M⊙ . The minimum mass is set by the mass at which it is possible to have H fusion. For M < 0.1 M⊙ , the core is not hot enough for H fusion, and thus the object is not a star (it would be a super-Jupiter or “brown dwarf”). The physics of the upper mass limit is not known. We simply do ...
... 5: 0.1 and 100 M⊙ . The minimum mass is set by the mass at which it is possible to have H fusion. For M < 0.1 M⊙ , the core is not hot enough for H fusion, and thus the object is not a star (it would be a super-Jupiter or “brown dwarf”). The physics of the upper mass limit is not known. We simply do ...
AST 301 Introduction to Astronomy - University of Texas Astronomy
... A Red Giant with helium fusion When helium fusion starts generating energy in the core of a red giant, the core expands and hydrogen fusion in the shell around the core slows down. As a result, less total energy is being generated, and the envelope contracts and warms up some. But pretty soon all o ...
... A Red Giant with helium fusion When helium fusion starts generating energy in the core of a red giant, the core expands and hydrogen fusion in the shell around the core slows down. As a result, less total energy is being generated, and the envelope contracts and warms up some. But pretty soon all o ...
distances
... • The majority of stars lie along a band (not a sharp line) from top left to bottom right called the main sequence. • On the main sequence, hot stars are the most luminous, (top left) and cool stars are the least luminous (bottom right). ...
... • The majority of stars lie along a band (not a sharp line) from top left to bottom right called the main sequence. • On the main sequence, hot stars are the most luminous, (top left) and cool stars are the least luminous (bottom right). ...
Problem Set No. 5
... (b) The element with the highest density is osmium. It has a density of 22.6 gm/cm3 , twice as dense as lead. Yet the H and He inside the sun can be much denser. At what radius is the density of the solar material equal to that of osmium? What is the temperature at that point? Is that temperature hi ...
... (b) The element with the highest density is osmium. It has a density of 22.6 gm/cm3 , twice as dense as lead. Yet the H and He inside the sun can be much denser. At what radius is the density of the solar material equal to that of osmium? What is the temperature at that point? Is that temperature hi ...
Distant Stars Lesson Plan
... How fast the system’s jet streams are moving. Point out that there is a wealth of additional information not included in the ‘How far away is it’ video. ...
... How fast the system’s jet streams are moving. Point out that there is a wealth of additional information not included in the ‘How far away is it’ video. ...
Stellar Evolution II
... Larger clouds of gas (GMCs) tend to fragment into smaller ones before collapsing to form stars – very massive stars are rare • Stars with masses above 50 MSUN are unstable – nuclear reactions in their core produce energy at such a fast rate that they blow off their outer layers, losing mass. ...
... Larger clouds of gas (GMCs) tend to fragment into smaller ones before collapsing to form stars – very massive stars are rare • Stars with masses above 50 MSUN are unstable – nuclear reactions in their core produce energy at such a fast rate that they blow off their outer layers, losing mass. ...