Lecture 6: Properties of Stars The Constellations The Constellations
... mapped many of these “absorption lines” with reasonable accuracy - called Fraunhofer lines. ‘Na D lines’ ...
... mapped many of these “absorption lines” with reasonable accuracy - called Fraunhofer lines. ‘Na D lines’ ...
combined astro show 2013
... #3) An absorption spectrum or dark line spectrum is produced when a gas (in space) comes between the observer and the source of light (Bright line) ...
... #3) An absorption spectrum or dark line spectrum is produced when a gas (in space) comes between the observer and the source of light (Bright line) ...
Spectral Variations of Several RV Tauri Type Stars Patrick Durant
... Stellar distances (d) were derived from the HipparcosTyco parallax database The absolute magnitude (M) was calculated using the ...
... Stellar distances (d) were derived from the HipparcosTyco parallax database The absolute magnitude (M) was calculated using the ...
LT 9: I can describe how a protostar becomes a star.
... The surface temperature drops and it is now a huge, bright, red aging star ...
... The surface temperature drops and it is now a huge, bright, red aging star ...
Compare the following sets of stars using the words: BRIGHTER or
... 1. Spica (dimmer and hotter) and Polaris (brighter and cooler) 2. Betelgeuse (brighter and same cool temperature) and Bernard’s star (dimmer and same cool temp.) 3. Sirius B (brighter and hotter) and Procyon B (dimmer and cooler) 4. Sun (dimmer and cooler) and Vega (brighter and hotter) 5. Alpha Cen ...
... 1. Spica (dimmer and hotter) and Polaris (brighter and cooler) 2. Betelgeuse (brighter and same cool temperature) and Bernard’s star (dimmer and same cool temp.) 3. Sirius B (brighter and hotter) and Procyon B (dimmer and cooler) 4. Sun (dimmer and cooler) and Vega (brighter and hotter) 5. Alpha Cen ...
Stars - Madison County Schools
... – Very large, massive stars burn their fuel much faster than smaller stars – Their main sequence may last only a few hundred thousand years – Smaller stars will live on for billions of years because they burn their fuel much more slowly ...
... – Very large, massive stars burn their fuel much faster than smaller stars – Their main sequence may last only a few hundred thousand years – Smaller stars will live on for billions of years because they burn their fuel much more slowly ...
4 x What Powers the Sun? • Need to provide
... Magnetic field lines short out Î Huge burst of charged particles Due to “winding up” of Sun’s magnetic ...
... Magnetic field lines short out Î Huge burst of charged particles Due to “winding up” of Sun’s magnetic ...
Properties of Stars
... Characteristics of Stars • Color is a clue to a star’s temperature • Very hot (30,000 K) stars emit their light in the blue spectrum, red stars are much cooler, stars with temperatures between 5000 and 6000 K appear yellow • Binary Stars – pairs of stars, pulled together by gravity, that orbit each ...
... Characteristics of Stars • Color is a clue to a star’s temperature • Very hot (30,000 K) stars emit their light in the blue spectrum, red stars are much cooler, stars with temperatures between 5000 and 6000 K appear yellow • Binary Stars – pairs of stars, pulled together by gravity, that orbit each ...
The Life Cycle of Stars
... Click Stars: Lights in the Sky and write out the questions and answers to the following on a sheet of white construction paper to be turned in. Be sure your name and period are on it. 1) What is the name of the brightest star in our night sky? What is the name of the brightest star in all of the kno ...
... Click Stars: Lights in the Sky and write out the questions and answers to the following on a sheet of white construction paper to be turned in. Be sure your name and period are on it. 1) What is the name of the brightest star in our night sky? What is the name of the brightest star in all of the kno ...
1 Astronomical Measurements and Quantities 2 Astronomical Objects
... binaries (=eclipsing variables) and the light curve. [K], [BM]. Stars: properties: Masses of stars - mass of the Sun, mass of binary stars (visual and spectroscopic); Radii of stars - interferometry and lunar occultations (hints) - eclipsing binaries; Properties from spectra - effective temperature ...
... binaries (=eclipsing variables) and the light curve. [K], [BM]. Stars: properties: Masses of stars - mass of the Sun, mass of binary stars (visual and spectroscopic); Radii of stars - interferometry and lunar occultations (hints) - eclipsing binaries; Properties from spectra - effective temperature ...
Integrative Studies 410 Our Place in the Universe
... production rate and available fuel (mass) – Example: Star with 4L and 3M uses 4 times more mass for energy production, but has 3 times more mass, so its life time is a factor ¾=0.75 compared to the sun: 7.5 billion years ([0.75] goes in the box) ...
... production rate and available fuel (mass) – Example: Star with 4L and 3M uses 4 times more mass for energy production, but has 3 times more mass, so its life time is a factor ¾=0.75 compared to the sun: 7.5 billion years ([0.75] goes in the box) ...
Death of Stars
... Lower turn-off point from the main sequence indicates High turn-off point shows there are that there are not many high mass stars left so this high mass stars present, so this cluster is cluster is older - likely to be a globular cluster younger and probably an open cluster Present information by pl ...
... Lower turn-off point from the main sequence indicates High turn-off point shows there are that there are not many high mass stars left so this high mass stars present, so this cluster is cluster is older - likely to be a globular cluster younger and probably an open cluster Present information by pl ...
Lecture 10: The Hertzsprung
... Review of what we know about Stellar Properties Large range of Stellar Luminosities 10-4 to 106 Lsun Large range of Stellar Radii 10-2 to 103 Rsun Modest range of Stellar Temperature 3000 to > 50,000 K Moderate range of Stellar Masses 0.1 to 50 Msun ...
... Review of what we know about Stellar Properties Large range of Stellar Luminosities 10-4 to 106 Lsun Large range of Stellar Radii 10-2 to 103 Rsun Modest range of Stellar Temperature 3000 to > 50,000 K Moderate range of Stellar Masses 0.1 to 50 Msun ...
Section 27.2
... stable part of their life cycle. White dwarfs are hot and dim and cannot be seen without a telescope. Red giants are cool and bright and some can be seen without a telescope. Can you locate blue giants on the H-R diagram? ...
... stable part of their life cycle. White dwarfs are hot and dim and cannot be seen without a telescope. Red giants are cool and bright and some can be seen without a telescope. Can you locate blue giants on the H-R diagram? ...
Astronomy 2
... The original mass of the star determines its temperature and the color. (Big – glows blue, medium – glows yellow-orange, small – glows red) Red Giants / Red Super-giants form as H2 fuel is used up and gravity overpowers released energy, center core contracts while outer layer expands (He2 + He2 → C ...
... The original mass of the star determines its temperature and the color. (Big – glows blue, medium – glows yellow-orange, small – glows red) Red Giants / Red Super-giants form as H2 fuel is used up and gravity overpowers released energy, center core contracts while outer layer expands (He2 + He2 → C ...
red shift blue shift
... Know the equation for parallax: d = distance in parsecs, p = parallax in arc ...
... Know the equation for parallax: d = distance in parsecs, p = parallax in arc ...
Abundance of Elements
... I. Derive the stellar parameters of M dwarfs using the synthetic spectra in the long wavelength region of the optical spectra (over 8000 Å), which is relatively less contaminated by molecular lines as well as telluric lines. Test the synthetic spectrum for K2 III type star : HD 110014 ...
... I. Derive the stellar parameters of M dwarfs using the synthetic spectra in the long wavelength region of the optical spectra (over 8000 Å), which is relatively less contaminated by molecular lines as well as telluric lines. Test the synthetic spectrum for K2 III type star : HD 110014 ...
Name: Period : ______ The Universe – Life and Death of a Star How
... 7. How much larger than our solar system was the cloud that formed our Sun? 8. What is formed when gravity compresses the center of a gas cloud to a scorching 2 million degrees? 9. What is the process in the center of stars where small atoms become big atoms? 10. If you’ve got __________________, yo ...
... 7. How much larger than our solar system was the cloud that formed our Sun? 8. What is formed when gravity compresses the center of a gas cloud to a scorching 2 million degrees? 9. What is the process in the center of stars where small atoms become big atoms? 10. If you’ve got __________________, yo ...
Integrative Studies 410 Our Place in the Universe
... • Cloud contracts/warms, begins radiating; almost all radiated energy escapes • Cloud becomes dense opaque to radiation radiated energy trapped core heats up ...
... • Cloud contracts/warms, begins radiating; almost all radiated energy escapes • Cloud becomes dense opaque to radiation radiated energy trapped core heats up ...
Sample exam 2
... 13. Suppose you are looking at the emission spectrum of gaseous helium. You dutifully write down the wavelengths of emission. You notice a power dial on the side of emission lamp and, just for fun, decide to turn up the power. The color of the helium lamp changes and you look through the spectroscop ...
... 13. Suppose you are looking at the emission spectrum of gaseous helium. You dutifully write down the wavelengths of emission. You notice a power dial on the side of emission lamp and, just for fun, decide to turn up the power. The color of the helium lamp changes and you look through the spectroscop ...
Hertzsprung-Russell Diagram Astronomy Project Purpose: To
... 4.) Determine how many times more or less massive your star is compared to the Sun. You may include actual numeric data if you chose. Example: 10M SUN means 10 times more massive than the Sun. 5.) With the provided formula, determine the star’s lifetime based on its mass and luminosity. You may roun ...
... 4.) Determine how many times more or less massive your star is compared to the Sun. You may include actual numeric data if you chose. Example: 10M SUN means 10 times more massive than the Sun. 5.) With the provided formula, determine the star’s lifetime based on its mass and luminosity. You may roun ...
H-R Diagram - SFA Physics
... Now plot all the stars from Table 7 onto Figure 3. Table 7 is a list of the 30 stars nearest the sun and the majority of these stars are considered to be the most common types of stars in the galaxy. Transfer the main sequence curve from Figure 1 to Figure 3. ...
... Now plot all the stars from Table 7 onto Figure 3. Table 7 is a list of the 30 stars nearest the sun and the majority of these stars are considered to be the most common types of stars in the galaxy. Transfer the main sequence curve from Figure 1 to Figure 3. ...
Stellar classification
In astronomy, stellar classification is the classification of stars based on their spectral characteristics. Light from the star is analyzed by splitting it with a prism or diffraction grating into a spectrum exhibiting the rainbow of colors interspersed with absorption lines. Each line indicates an ion of a certain chemical element, with the line strength indicating the abundance of that ion. The relative abundance of the different ions varies with the temperature of the photosphere. The spectral class of a star is a short code summarizing the ionization state, giving an objective measure of the photosphere's temperature and density.Most stars are currently classified under the Morgan–Keenan (MK) system using the letters O, B, A, F, G, K, and M, a sequence from the hottest (O type) to the coolest (M type). Each letter class is then subdivided using a numeric digit with 0 being hottest and 9 being coolest (e.g. A8, A9, F0, F1 form a sequence from hotter to cooler). The sequence has been expanded with classes for other stars and star-like objects that do not fit in the classical system, such class D for white dwarfs and class C for carbon stars.In the MK system a luminosity class is added to the spectral class using Roman numerals. This is based on the width of certain absorption lines in the star's spectrum which vary with the density of the atmosphere and so distinguish giant stars from dwarfs. Luminosity class 0 or Ia+ stars for hypergiants, class I stars for supergiants, class II for bright giants, class III for regular giants, class IV for sub-giants, class V for main-sequence stars, class sd for sub-dwarfs, and class D for white dwarfs. The full spectral class for the Sun is then G2V, indicating a main-sequence star with a temperature around 5,800K.