Virtual HR Diagram Lab
... b. Now manipulate the temperature and luminosity sliders and note the corresponding change in the active location. Fill in the table below. ...
... b. Now manipulate the temperature and luminosity sliders and note the corresponding change in the active location. Fill in the table below. ...
The Family of Stars
... Polaris has just about the same spectral type (and surface temperature) as our sun, but it is 10,000 times brighter. Thus, Polaris’ radius is … the sun’s radius. ...
... Polaris has just about the same spectral type (and surface temperature) as our sun, but it is 10,000 times brighter. Thus, Polaris’ radius is … the sun’s radius. ...
Life Cycles of Stars
... Size Matters • Different size stars go through similar life cycles, however they are different: 1) Low Mass Stars 2) Medium Mass Stars 3) High Mass Stars ...
... Size Matters • Different size stars go through similar life cycles, however they are different: 1) Low Mass Stars 2) Medium Mass Stars 3) High Mass Stars ...
Wednesday, April 17 - Otterbein University
... The Key Tool to understanding Stars: the Hertzsprung-Russell diagram • Hertzsprung-Russell diagram is luminosity vs. spectral type (or temperature) • To obtain a HR diagram: – get the luminosity. This is your y-coordinate. – Then take the spectral type as your x-coordinate, e.g. K5 for Aldebaran. F ...
... The Key Tool to understanding Stars: the Hertzsprung-Russell diagram • Hertzsprung-Russell diagram is luminosity vs. spectral type (or temperature) • To obtain a HR diagram: – get the luminosity. This is your y-coordinate. – Then take the spectral type as your x-coordinate, e.g. K5 for Aldebaran. F ...
Microsoft Power Point version
... Measuring Distances to Stars parallax – apparent wobble of a star due to the Earth’s orbiting of the Sun ...
... Measuring Distances to Stars parallax – apparent wobble of a star due to the Earth’s orbiting of the Sun ...
1. Stellar Evolution – Notes Astronomers classify stars according to
... combination of all the colors that appear in its spectrum. When a beam of sunlight passes through a glass prism, the light is broken into a rainbowcolored band called a spectrum. Because of its electric and magnetic properties, light is also called electromagnetic radiation. It has wavelike properti ...
... combination of all the colors that appear in its spectrum. When a beam of sunlight passes through a glass prism, the light is broken into a rainbowcolored band called a spectrum. Because of its electric and magnetic properties, light is also called electromagnetic radiation. It has wavelike properti ...
THE HERTZSPRUNG-RUSSELL DIAGRAM (H
... NOTE: Absolute Magnitude IS THE SAME THING AS LUMINOSITY ON THE GRAPH DEFINE: absolute magnitude (Pg. 372 if you don’t know) ...
... NOTE: Absolute Magnitude IS THE SAME THING AS LUMINOSITY ON THE GRAPH DEFINE: absolute magnitude (Pg. 372 if you don’t know) ...
SORTING SPECTRA
... Stellar spectra were first observed in the middle of the 19th century. As an aid to understanding, astronomers began classifying the spectra. In 1890, E.C. Pickering and assistants Annie Jump Cannon, Antonia Maury, and Williamina Fleming categorized the stars, lettering them according to the strengt ...
... Stellar spectra were first observed in the middle of the 19th century. As an aid to understanding, astronomers began classifying the spectra. In 1890, E.C. Pickering and assistants Annie Jump Cannon, Antonia Maury, and Williamina Fleming categorized the stars, lettering them according to the strengt ...
Continuous Spectrum Absorption Line Spectrum Emission Line
... broadening.! Increasing the density will broaden the lines because of the subsequent increase in collision rate between atoms.! All stars of a given spectral class have the same temperature, so the width of the absorption lines is a direct measure of the density.! But the larger stars have a more te ...
... broadening.! Increasing the density will broaden the lines because of the subsequent increase in collision rate between atoms.! All stars of a given spectral class have the same temperature, so the width of the absorption lines is a direct measure of the density.! But the larger stars have a more te ...
File - Mr. Goodyear Astronomy
... This increase energy causes an explosion-like occurrence. This cause star to lose large quantities of mass. Also during this time period star sheds off excess gas envelopes, which appears as a ring around star when viewed from a distance. ...
... This increase energy causes an explosion-like occurrence. This cause star to lose large quantities of mass. Also during this time period star sheds off excess gas envelopes, which appears as a ring around star when viewed from a distance. ...
PPT - McMaster Physics and Astronomy
... Main Sequence: Stars confined to well defined band from top left (high T, high L), to bottom right (low T, low L). •Temperature range over main sequence: 3,000K (M type) – 30,000 K (O type); 1 decade in temperature ...
... Main Sequence: Stars confined to well defined band from top left (high T, high L), to bottom right (low T, low L). •Temperature range over main sequence: 3,000K (M type) – 30,000 K (O type); 1 decade in temperature ...
Starlight & Stars - Wayne State University Physics and Astronomy
... Hydrogen strongest; singly-ionized metals ...
... Hydrogen strongest; singly-ionized metals ...
Astronomers classify stars according to their physical characteristics
... •A star’s _apparent_ brightness depends upon how bright it _actually is and its _distance_ from Earth. •A star’s actual brightness (or _absolute magnitude) usually depends on the star’s _size_ and temperature__. •Because stars with _more mass ___ have more __self _gravity, they tend to have _higher_ ...
... •A star’s _apparent_ brightness depends upon how bright it _actually is and its _distance_ from Earth. •A star’s actual brightness (or _absolute magnitude) usually depends on the star’s _size_ and temperature__. •Because stars with _more mass ___ have more __self _gravity, they tend to have _higher_ ...
Exercise 7
... declination (think of this as a space latitude). The declination runs from -90° (celestial south pole) to +90° (celestial north pole). Both of these coordinates are laminated to the metal pole bases. In addition, the stars have been colored according to their spectral classes; blue balls represent O ...
... declination (think of this as a space latitude). The declination runs from -90° (celestial south pole) to +90° (celestial north pole). Both of these coordinates are laminated to the metal pole bases. In addition, the stars have been colored according to their spectral classes; blue balls represent O ...
HR Diagram Lab Handout
... 7. The temperature of the hottest stars is _______________. 8. The color of the hottest stars is ________________. 9. The temperature of the coldest stars is _______________. 10. The color of the coldest stars is ________________. 11. The life expectancy of a very hot star is _______________ years. ...
... 7. The temperature of the hottest stars is _______________. 8. The color of the hottest stars is ________________. 9. The temperature of the coldest stars is _______________. 10. The color of the coldest stars is ________________. 11. The life expectancy of a very hot star is _______________ years. ...
3Nov_2014
... • It works the same with stars! • If we know the total energy output of a star (luminosity), and we can count the number of photons we receive from that star (brightness), we can calculate its distance ...
... • It works the same with stars! • If we know the total energy output of a star (luminosity), and we can count the number of photons we receive from that star (brightness), we can calculate its distance ...
Part 1- The Basics
... • Standard filters, such as U (Ultraviolet), B (Blue) and V (Visual, yellow-green) filters, • Color ratios of a star are the ratios of brightness values obtained through different filters • These ratios are a good measure of the star’s surface temperature; this is an easy way to get temperature ...
... • Standard filters, such as U (Ultraviolet), B (Blue) and V (Visual, yellow-green) filters, • Color ratios of a star are the ratios of brightness values obtained through different filters • These ratios are a good measure of the star’s surface temperature; this is an easy way to get temperature ...
Stars Jeopardy
... On the HR diagram, do stars get brighter as you go up the scale or as you go down? ...
... On the HR diagram, do stars get brighter as you go up the scale or as you go down? ...
Lecture 31 - 2 The Death of Stars: Stellar Recycling Phase 3 -
... Once all of the Hydrogen has been converted to Helium in the star’s core, thermonuclear reactions stop and for the moment there is no internal energy output that can counteract the always present inward pull of the star’s gravity. The pure Helium core now behaves separately from the surrounding laye ...
... Once all of the Hydrogen has been converted to Helium in the star’s core, thermonuclear reactions stop and for the moment there is no internal energy output that can counteract the always present inward pull of the star’s gravity. The pure Helium core now behaves separately from the surrounding laye ...
Distance to Stars
... • 3. Medium Size Star- Our Sun • 4. White dwarf- smaller than the sun, about the size of Earth. • 5. Neutron Star- very small, 20km ...
... • 3. Medium Size Star- Our Sun • 4. White dwarf- smaller than the sun, about the size of Earth. • 5. Neutron Star- very small, 20km ...
Unit 1
... • a. a low mass red giant that varies in size and brightness in an irregular way • b. a big planet • c. a high-mass giant or supergiant star that pulsates regularly in size and brightness • d. a variable emission nebula near a young star ...
... • a. a low mass red giant that varies in size and brightness in an irregular way • b. a big planet • c. a high-mass giant or supergiant star that pulsates regularly in size and brightness • d. a variable emission nebula near a young star ...
SHELL H II REGIONS IN NGC 6334
... • Approach that takes advantage of old archival data that can be compared with more recent observations. • Addresses key parameters in astronomy such as mass, distance, and age. ...
... • Approach that takes advantage of old archival data that can be compared with more recent observations. • Addresses key parameters in astronomy such as mass, distance, and age. ...
December 1, 2011 - Perry Local Schools
... 1. Place the small flashlight on a desk or table near the front of the room. 2. Place the large flashlight on a desk or table near the back of the room. 3. Gather at the front of the room so they can all see both flashlights easily. 4. Turn on both flashlights. 5. Darken the room. 6. Observe and co ...
... 1. Place the small flashlight on a desk or table near the front of the room. 2. Place the large flashlight on a desk or table near the back of the room. 3. Gather at the front of the room so they can all see both flashlights easily. 4. Turn on both flashlights. 5. Darken the room. 6. Observe and co ...
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.