Jeopardy 2015
... An interstellar cloud is disturbed and begins to gravitationally collapse, fragments,It heats up and spins faster. When the core temperature reaches 100 mill K, nuclear fusion begins (H into He). When outward pressure equals inward pressure the star enters the main sequence. ...
... An interstellar cloud is disturbed and begins to gravitationally collapse, fragments,It heats up and spins faster. When the core temperature reaches 100 mill K, nuclear fusion begins (H into He). When outward pressure equals inward pressure the star enters the main sequence. ...
(0 = not at all, 10 = totally) (no wrong answers)
... - How we use parallax to measure distances to nearby stars. - Basic properties on each of the major kinds of stars. - What kinds of stars are in the local stellar neighborhood - How we measure luminosity and magnitude - How to calculate apparent and absolute magnitude - The basic structure and compo ...
... - How we use parallax to measure distances to nearby stars. - Basic properties on each of the major kinds of stars. - What kinds of stars are in the local stellar neighborhood - How we measure luminosity and magnitude - How to calculate apparent and absolute magnitude - The basic structure and compo ...
Stars - Red, Blue, Old, New pt.2
... • Most stars have temps between 3000 K and 30,000 K. • Stars have wide range in luminosity. Some are 10s of 1000s of times more luminous than sun; others much less luminous. • Masses range from 0.07 to 120 times mass of sun • Diameters planet-sized to 100s x sun ...
... • Most stars have temps between 3000 K and 30,000 K. • Stars have wide range in luminosity. Some are 10s of 1000s of times more luminous than sun; others much less luminous. • Masses range from 0.07 to 120 times mass of sun • Diameters planet-sized to 100s x sun ...
Lecture 9: Hydrostatic Equilibrium
... surface of the star. Winds are a common feature of massive stars. Also, at some point, the radiation pressure may make it impossible to form a more luminous star than a certain limit. This is known as the Eddington limit and we’ll talk about it more later. It sets a limit on the luminosity that an o ...
... surface of the star. Winds are a common feature of massive stars. Also, at some point, the radiation pressure may make it impossible to form a more luminous star than a certain limit. This is known as the Eddington limit and we’ll talk about it more later. It sets a limit on the luminosity that an o ...
1. If a star`s temperature is doubled but radius is kept constant, by
... 1. If a star’s temperature is doubled but radius is kept constant, by how much does its luminosity go up by? 1a. Goes up by a factor of 24 = 16. 2. If a star’s temperature is increased by a factor of three, four, five and six, but in every case its radius is kept constant, what happens to its lumino ...
... 1. If a star’s temperature is doubled but radius is kept constant, by how much does its luminosity go up by? 1a. Goes up by a factor of 24 = 16. 2. If a star’s temperature is increased by a factor of three, four, five and six, but in every case its radius is kept constant, what happens to its lumino ...
The Hertzsprung-Russell diagram and the nature of stars
... • Physical argument 1: what holds stars up? • Physical argument 2: what powers the stars (where do they get their energy supply?) ...
... • Physical argument 1: what holds stars up? • Physical argument 2: what powers the stars (where do they get their energy supply?) ...
of the star. - Colyton High School
... final outcome is the _____________________ Medium mass Massive star XI. Now click on the in the Interactive Lab more near the top of the page. Play through all 5 steps by hitting the play button. Do NOT click “Check Answers”…it will only waste your time. 12) Explain how a supernova (in step 5) can e ...
... final outcome is the _____________________ Medium mass Massive star XI. Now click on the in the Interactive Lab more near the top of the page. Play through all 5 steps by hitting the play button. Do NOT click “Check Answers”…it will only waste your time. 12) Explain how a supernova (in step 5) can e ...
Stellar Masses and the Main Sequence
... There is also a mass-radius relation for main-sequence stars. When parameterized by R ∝ Mξ, ξ ~ 0.57 for M > 1 M, and ξ ~ 0.8 for M < 1 M." ...
... There is also a mass-radius relation for main-sequence stars. When parameterized by R ∝ Mξ, ξ ~ 0.57 for M > 1 M, and ξ ~ 0.8 for M < 1 M." ...
Life Cycle of STARS
... • Are stars BORN??? • Take a moment to think about our own Sun, and write down an idea about how it was formed using what we have learned so far. ...
... • Are stars BORN??? • Take a moment to think about our own Sun, and write down an idea about how it was formed using what we have learned so far. ...
STAR FORMATION (Ch. 19) The basics: GRAVITY vs. PRESSURE
... These were almost certainly the first objects to be formed in our Galaxy. Note: Abundances of all elements heavier than carbon are very small compared to the sun and most other stars (because they formed when the Galaxy was relatively “pollution free”— we’ll return to this). Make sure you understand ...
... These were almost certainly the first objects to be formed in our Galaxy. Note: Abundances of all elements heavier than carbon are very small compared to the sun and most other stars (because they formed when the Galaxy was relatively “pollution free”— we’ll return to this). Make sure you understand ...
Chapter19
... fusion. By the time the center of the star becomes hot enough for helium fusion, all of the hydrogen has been fused into helium. Their nuclei have greater positive charges than hydrogen, so a higher temperature is required for the nuclei to have enough energy to overcome the repulsive electrical for ...
... fusion. By the time the center of the star becomes hot enough for helium fusion, all of the hydrogen has been fused into helium. Their nuclei have greater positive charges than hydrogen, so a higher temperature is required for the nuclei to have enough energy to overcome the repulsive electrical for ...
File
... Variation in brightness displays a regular pattern over time All extrinsic variables are periodic e.g. Eclipsing Binaries, Rotating Variable Stars Cepheids are periodic variables (they are intrinsic) Variation in brightness is not repeating over time (irregular variation) E.g. Novae, Supernovas, Eru ...
... Variation in brightness displays a regular pattern over time All extrinsic variables are periodic e.g. Eclipsing Binaries, Rotating Variable Stars Cepheids are periodic variables (they are intrinsic) Variation in brightness is not repeating over time (irregular variation) E.g. Novae, Supernovas, Eru ...
H-R Diagrams
... If we plot a graph of luminosity against temperature for lots of stars we get a graph like this… ...
... If we plot a graph of luminosity against temperature for lots of stars we get a graph like this… ...
AY1 Homework for Quiz 2: Spring 2017
... 24. Why don’t White Dwarfs collapse to smaller radius due to gravity? (check any that are correct). ____ A. They are supported by hydrogen fusion ____ B. All white dwarfs are in the process of slowly ...
... 24. Why don’t White Dwarfs collapse to smaller radius due to gravity? (check any that are correct). ____ A. They are supported by hydrogen fusion ____ B. All white dwarfs are in the process of slowly ...
Ch. 14 Formation of Stars
... cool interiors, which makes them more opaque to photons. • As a result, radiation cannot easily flow through any part of them, so they only have convective zones. No radiative zones. • Core convective zone • “Stars” between 0.08 and 0.012 solar masses are not really stars at all; called “brown dwa ...
... cool interiors, which makes them more opaque to photons. • As a result, radiation cannot easily flow through any part of them, so they only have convective zones. No radiative zones. • Core convective zone • “Stars” between 0.08 and 0.012 solar masses are not really stars at all; called “brown dwa ...
Stellar Evolution – Test Review Answers
... The greater the mass of a main-sequence star, the greater its luminosity (and also the greater its radius and surface temperature). In other words, stars that are higher up (brighter) on the main sequence are more massive, larger, and hotter. 19. Describe the beginning of a star’s life. The birth of ...
... The greater the mass of a main-sequence star, the greater its luminosity (and also the greater its radius and surface temperature). In other words, stars that are higher up (brighter) on the main sequence are more massive, larger, and hotter. 19. Describe the beginning of a star’s life. The birth of ...
Powerpoint of lecture 14
... • For solar composition, model HR diagram agrees satisfactorily with observations, remembering that models are zero age and observed stars have range of ages – see blackboard sketch ...
... • For solar composition, model HR diagram agrees satisfactorily with observations, remembering that models are zero age and observed stars have range of ages – see blackboard sketch ...
Document
... In the early part of this century, astronomer Ejnar Hertzsprung studied the luminosities and types of stars. Soon, he and American astronomer, Henry Russell, developed a graphical representation comparing a star’s temperature against its luminosity (also called absolute magnitude) and types of stars ...
... In the early part of this century, astronomer Ejnar Hertzsprung studied the luminosities and types of stars. Soon, he and American astronomer, Henry Russell, developed a graphical representation comparing a star’s temperature against its luminosity (also called absolute magnitude) and types of stars ...
Dim Stars - granthamkuehl
... In our study of Stars The students will be able to Determine color, temp., brightness and Size of a star And show what they learned by Interpreting the HR Diagram ...
... In our study of Stars The students will be able to Determine color, temp., brightness and Size of a star And show what they learned by Interpreting the HR Diagram ...
CBradleyLoutl
... . Most of a star is hydrogen, less than a quarter is helium, maybe 1 part per thousand will be heavier elements. . Looking at what wavelengths of light are present on emission/absorption spectra will tell exact constituents. Examples: - Age: . For a star around one solar mass, it takes a few million ...
... . Most of a star is hydrogen, less than a quarter is helium, maybe 1 part per thousand will be heavier elements. . Looking at what wavelengths of light are present on emission/absorption spectra will tell exact constituents. Examples: - Age: . For a star around one solar mass, it takes a few million ...
File - Mr. Goodyear Astronomy
... to main sequence, 1st discovered in constellation in Taurus. Stars are the same mass, as main sequence, but they are significantly more luminous because their radii are larger. Temperature in core is to low for nuclear fusion. Powered by gravitational energy. (Size rage: 1000 X diameter of sun) last ...
... to main sequence, 1st discovered in constellation in Taurus. Stars are the same mass, as main sequence, but they are significantly more luminous because their radii are larger. Temperature in core is to low for nuclear fusion. Powered by gravitational energy. (Size rage: 1000 X diameter of sun) last ...
Document
... j. How is it possible that Canopus is more luminous than Achernar, given their respective spectral types? Canopus is cooler than Achernar; therefore, the only way Canopus can be more luminous is because it is LARGER. 2. List the evolutionary stages of the Sun’s life cycle & describe how its size (Ra ...
... j. How is it possible that Canopus is more luminous than Achernar, given their respective spectral types? Canopus is cooler than Achernar; therefore, the only way Canopus can be more luminous is because it is LARGER. 2. List the evolutionary stages of the Sun’s life cycle & describe how its size (Ra ...