Guess The Spectra!!
... Hydrogen and Helium like the Sun, but is a different color! The color difference is due to temperature. Rigel is 2x as hot as the Sun so it appears blue! ...
... Hydrogen and Helium like the Sun, but is a different color! The color difference is due to temperature. Rigel is 2x as hot as the Sun so it appears blue! ...
Talk
... cannot generate the temperate and pressure needed for fusion beyond helium. These are White Dwarf stars, and in most cases this is nearly the end of their evolution. ...
... cannot generate the temperate and pressure needed for fusion beyond helium. These are White Dwarf stars, and in most cases this is nearly the end of their evolution. ...
THE LIFE CYCLE OF A STAR
... from 2000C to above 30,000C, and the corresponding colors from red to blue-white. The brightest stars have masses 100 times that of the Sun and emit as much light as millions of Suns. They live for less than a million years before exploding as supernovae. The faintest stars are the red dwarfs, less ...
... from 2000C to above 30,000C, and the corresponding colors from red to blue-white. The brightest stars have masses 100 times that of the Sun and emit as much light as millions of Suns. They live for less than a million years before exploding as supernovae. The faintest stars are the red dwarfs, less ...
Study Guide for 3RD Astronomy Exam
... period of 30 years. What is their combined mass? If they are both main sequence stars, what spectral types can they not be? You’ll need to use the appendix in the text on Properties of Main Sequence Stars. ...
... period of 30 years. What is their combined mass? If they are both main sequence stars, what spectral types can they not be? You’ll need to use the appendix in the text on Properties of Main Sequence Stars. ...
Properties of Stars
... your graph. (example: label the white dwarf section, the main sequence section, etc.) 8. What group do most of the stars you graphed belong to? (white dwarf, red giant, main sequence, etc.) 9. Comparing both your chart and the chart on the first page, are any of the 20 nearest or 20 brightest stars ...
... your graph. (example: label the white dwarf section, the main sequence section, etc.) 8. What group do most of the stars you graphed belong to? (white dwarf, red giant, main sequence, etc.) 9. Comparing both your chart and the chart on the first page, are any of the 20 nearest or 20 brightest stars ...
Extraterrestrial Life
... orbits close to the same plane orbits in same direction as Sun’s rotation rotation in the same direction (except Venus and Uranus) planets evenly spaced, increased by a factor of 1.5 to 2 planets sizes and compositions change with distance: terrestrial planets are rocky (iron and silicates) and gas ...
... orbits close to the same plane orbits in same direction as Sun’s rotation rotation in the same direction (except Venus and Uranus) planets evenly spaced, increased by a factor of 1.5 to 2 planets sizes and compositions change with distance: terrestrial planets are rocky (iron and silicates) and gas ...
![2-2 wkst - Home [www.petoskeyschools.org]](http://s1.studyres.com/store/data/009700019_1-9e7a7c15444658cfc76a04a9cf1ba291-300x300.png)
2-2 wkst - Home [www.petoskeyschools.org]
... c. They can be brighter than an entire galaxy for several days. d. They are explosions in which a star throws its outer layers into space. 27. A star that has collapsed under gravity is called a(n) ______________________. 28. A rapidly spinning neutron star is called a(n) ______________________. 29 ...
... c. They can be brighter than an entire galaxy for several days. d. They are explosions in which a star throws its outer layers into space. 27. A star that has collapsed under gravity is called a(n) ______________________. 28. A rapidly spinning neutron star is called a(n) ______________________. 29 ...
Stellar Evolution
... All stars rotate and thus have angular momentum. When a star loses most of its mass in a supernova, the remaining neutron star rotates very quickly. The fastest observed neutron star rotates at 716 revolutions per second. ...
... All stars rotate and thus have angular momentum. When a star loses most of its mass in a supernova, the remaining neutron star rotates very quickly. The fastest observed neutron star rotates at 716 revolutions per second. ...
1 WHY DO THE STARS IN ORION LOOK SO DIFFERENT FROM
... Remember that we said the apparent magnitude of a star is as we observe it from earth and that it is not reflective of a stars true physical character. We can understand more about a stars’ brightness by understanding the relationship of a stars’ luminosity and size. Luminosity shows the relationshi ...
... Remember that we said the apparent magnitude of a star is as we observe it from earth and that it is not reflective of a stars true physical character. We can understand more about a stars’ brightness by understanding the relationship of a stars’ luminosity and size. Luminosity shows the relationshi ...
How Stars Form Powerpoint
... Stars of Other Masses Remember - Main Sequence is a band, rather than a line, because stars of the same mass can have different compositions. Most important: Stars do not move along the Main Sequence! Once they reach it, they are in equilibrium and do not move until their fuel begins to run out. ...
... Stars of Other Masses Remember - Main Sequence is a band, rather than a line, because stars of the same mass can have different compositions. Most important: Stars do not move along the Main Sequence! Once they reach it, they are in equilibrium and do not move until their fuel begins to run out. ...
1. Introduction
... very many, stars pulsate in more complicated manners than the Cepheids. In many instances more than one mode of oscillation is excited simultaneously in a star; these modes may include both radial overtones, in addition to the fundamental, and nonradial modes, where the motion does not preserve sphe ...
... very many, stars pulsate in more complicated manners than the Cepheids. In many instances more than one mode of oscillation is excited simultaneously in a star; these modes may include both radial overtones, in addition to the fundamental, and nonradial modes, where the motion does not preserve sphe ...
Extra-Solar Life: Habitable Zones
... Mercury/Venus too hot Earth – just right Mars – was OK once (?), but now cold Jupiter, Saturn, Uranus, Neptune too cold (though some moons may be OK) ...
... Mercury/Venus too hot Earth – just right Mars – was OK once (?), but now cold Jupiter, Saturn, Uranus, Neptune too cold (though some moons may be OK) ...
Constellation Notes
... How many constellations are there? The sky was divided up into 88 different constellations in 1922. This included 48 ancient constellations listed by the Greek astronomer Ptolemy as well as 40 new constellations. Star Maps The 88 different constellations divide up the entire night sky as seen from a ...
... How many constellations are there? The sky was divided up into 88 different constellations in 1922. This included 48 ancient constellations listed by the Greek astronomer Ptolemy as well as 40 new constellations. Star Maps The 88 different constellations divide up the entire night sky as seen from a ...
File - greenscapes4you
... luminosity, but still much brighter than main sequence stars of same spectral type. The hot, white, small radius stars near the lower left are called white dwarfs. Giants and Supergiants are stars nearing the ends of their lives because they have already exhausted their core hydrogen. Surprisingly, ...
... luminosity, but still much brighter than main sequence stars of same spectral type. The hot, white, small radius stars near the lower left are called white dwarfs. Giants and Supergiants are stars nearing the ends of their lives because they have already exhausted their core hydrogen. Surprisingly, ...
PPT file
... Eventually a red dwarf changes into a very hot, but small, dim white dwarf and quietly burns out ...
... Eventually a red dwarf changes into a very hot, but small, dim white dwarf and quietly burns out ...
HR DIAGRAM ACTIVITY
... 5. Of the stars you plotted, which is nearest to the end of its life? ________________ (name of star) Explain how you determined this. ...
... 5. Of the stars you plotted, which is nearest to the end of its life? ________________ (name of star) Explain how you determined this. ...
Brightness and Temperature of Stars
... A star’s brightness, or luminosity, depends on the star’s surface temperature and size. If two stars have the same surface temperature, the larger star will be more luminous. The Hertzsprung-Russell (H-R) diagram below is a scatter plot that shows the relative temperatures and luminosities of variou ...
... A star’s brightness, or luminosity, depends on the star’s surface temperature and size. If two stars have the same surface temperature, the larger star will be more luminous. The Hertzsprung-Russell (H-R) diagram below is a scatter plot that shows the relative temperatures and luminosities of variou ...
Study Guide for 3RD Astronomy Exam
... Interpret stellar apparent magnitudes and their relationship to brightness Interpret stellar absolute magnitudes and their relationship to luminosity Solve problems relating to the relative brightness or luminosity of two stars given their m or M values. Determine the hottest and coolest stars from ...
... Interpret stellar apparent magnitudes and their relationship to brightness Interpret stellar absolute magnitudes and their relationship to luminosity Solve problems relating to the relative brightness or luminosity of two stars given their m or M values. Determine the hottest and coolest stars from ...
Today`s Powerpoint
... While on Main Sequence, stellar core has H -> He fusion, by p-p chain in stars like Sun or less massive. In more massive stars, “CNO cycle” becomes more important. ...
... While on Main Sequence, stellar core has H -> He fusion, by p-p chain in stars like Sun or less massive. In more massive stars, “CNO cycle” becomes more important. ...
Birth of Elements
... Another interesting fact is that, for most elements, there is a certain temperature at which their emission and absorption lines in a given range are strongest. This is not too surprising since the temperature does decide the energy of the atoms and ions which are emitting light and therefore also d ...
... Another interesting fact is that, for most elements, there is a certain temperature at which their emission and absorption lines in a given range are strongest. This is not too surprising since the temperature does decide the energy of the atoms and ions which are emitting light and therefore also d ...
Bellringer - Madison County Schools
... Astronomers use parallax. They measure how far a star seems to move when Earth moves from one side of the sun to the other. The distance the star seems to move tells an astronomer how far the star is from Earth. ...
... Astronomers use parallax. They measure how far a star seems to move when Earth moves from one side of the sun to the other. The distance the star seems to move tells an astronomer how far the star is from Earth. ...
Integrative Studies 410 Our Place in the Universe
... distance ladder out as far as we can see Cepheids – about 50 million ly • In 1920 Hubble used this technique to measure the distance to Andromeda (about 2 million ly) • Works best for periodic variables ...
... distance ladder out as far as we can see Cepheids – about 50 million ly • In 1920 Hubble used this technique to measure the distance to Andromeda (about 2 million ly) • Works best for periodic variables ...
Folie 1 - univie.ac.at
... massive stars in our Galactic neighbourhood, representing objects which dominate the ecology of our Universe, and also highly evolved giant stars of lower mass to probe the future development of our Sun. The operation policy will be to observe a few fields over a long time span and possibly some sho ...
... massive stars in our Galactic neighbourhood, representing objects which dominate the ecology of our Universe, and also highly evolved giant stars of lower mass to probe the future development of our Sun. The operation policy will be to observe a few fields over a long time span and possibly some sho ...
Stars on the HR Diagram
... knowledge astronomers acquire about stars is through mathematical comparison of data derived from the light (radiation) from stars. The Hertzsprung-Russell (HR) Diagram, widely used in astronomy, is a scatter plot with a distribution of data points that describe a relationship between physical aspec ...
... knowledge astronomers acquire about stars is through mathematical comparison of data derived from the light (radiation) from stars. The Hertzsprung-Russell (HR) Diagram, widely used in astronomy, is a scatter plot with a distribution of data points that describe a relationship between physical aspec ...
Ch. 17 (RGs & WDs)
... the use of instructors in teaching their courses and assessing student learning. Dissemination or sale of any part of this work (including on the World Wide Web) will destroy the integrity of the work and is not permitted. The work and materials ...
... the use of instructors in teaching their courses and assessing student learning. Dissemination or sale of any part of this work (including on the World Wide Web) will destroy the integrity of the work and is not permitted. The work and materials ...
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.