www.astro.utu.fi
... stars in galaxy to merge with it via collisions is 1030 year most stars avoid this fate by evaporating from the galaxy Orbit of one star around the central black hole in the Galaxy (ESO) www.eso.org/public/outreach/press-rel/pr-2002/pr-17-02.html ...
... stars in galaxy to merge with it via collisions is 1030 year most stars avoid this fate by evaporating from the galaxy Orbit of one star around the central black hole in the Galaxy (ESO) www.eso.org/public/outreach/press-rel/pr-2002/pr-17-02.html ...
Lecture16
... Classification of Stars Classified by absorption lines in their spectra Annie Jump Cannon at Harvard (1863-1941) classified large numbers of stars (over 400,000!) HD catalog (still used today) From hottest to coolest stars: O, B, A, F, G, K, M Traditional: Oh Be A Fine Guy/Girl Kiss Me! Alternate: ...
... Classification of Stars Classified by absorption lines in their spectra Annie Jump Cannon at Harvard (1863-1941) classified large numbers of stars (over 400,000!) HD catalog (still used today) From hottest to coolest stars: O, B, A, F, G, K, M Traditional: Oh Be A Fine Guy/Girl Kiss Me! Alternate: ...
Chapter 28 Stars and Their Characteristics
... bright a star “appears” to be from Earth. The Apparent Magnitude of a star is affected by Absolute- Magnitude (Volume x Luminosity) and Distance from Observer. Betelgeuse, one of the brightest stars in the Universe, does not appear to be as bright as our Sun, because of its distance from us compared ...
... bright a star “appears” to be from Earth. The Apparent Magnitude of a star is affected by Absolute- Magnitude (Volume x Luminosity) and Distance from Observer. Betelgeuse, one of the brightest stars in the Universe, does not appear to be as bright as our Sun, because of its distance from us compared ...
Teacher Subject Title Concept Context Tek/SE Verb
... science notebook: What do you see when you look up at the sky? Does the sky look the same during the day as it does at night? Other than the Moon, what do we see in the night sky? What do you know about stars? Misconceptions: students may think that all of the stars in a constellation are near each ...
... science notebook: What do you see when you look up at the sky? Does the sky look the same during the day as it does at night? Other than the Moon, what do we see in the night sky? What do you know about stars? Misconceptions: students may think that all of the stars in a constellation are near each ...
Stellar evolution, II
... typically much, much longer than a human lifetime, during some stages of a star's life we can measure changes in its structure. Stars that pulsate may change their pulsational periods, indicating that the star is getting cooler or hotter. ...
... typically much, much longer than a human lifetime, during some stages of a star's life we can measure changes in its structure. Stars that pulsate may change their pulsational periods, indicating that the star is getting cooler or hotter. ...
Astronomy Homework - Life
... 5. As the helium core contracts, temperatures and pressures (increase/decrease). 6. Stars leave the main sequence when (they fuse hydrogen in their cores/they run out of hydrogen to fuse in their cores). 7. Hydrogen begins to fuse in a (shell/core) around the contracting helium core. 8. As the core ...
... 5. As the helium core contracts, temperatures and pressures (increase/decrease). 6. Stars leave the main sequence when (they fuse hydrogen in their cores/they run out of hydrogen to fuse in their cores). 7. Hydrogen begins to fuse in a (shell/core) around the contracting helium core. 8. As the core ...
The H-R Diagram
... luminosities. • Read about apparent magnitudes here, and absolute magnitude here, as well as in the text. We don’t have time in the course to get more mathematical than this ...
... luminosities. • Read about apparent magnitudes here, and absolute magnitude here, as well as in the text. We don’t have time in the course to get more mathematical than this ...
Chapter 11: Stars
... Pioneers of Stellar Classification Williamina Fleming (1857-1911) classified stellar spectra according to the strength of their hydrogen lines: A strongest, B slightly weaker, and O for the weakest. She classified more than 10,000 stars, which Pickering published in 1890. Annie Jump Cannon joined P ...
... Pioneers of Stellar Classification Williamina Fleming (1857-1911) classified stellar spectra according to the strength of their hydrogen lines: A strongest, B slightly weaker, and O for the weakest. She classified more than 10,000 stars, which Pickering published in 1890. Annie Jump Cannon joined P ...
Student Exploration Sheet: Growing Plants
... and catalog the thousands of star spectra that had been collected by the Harvard Observatory. He hired several women to do the work, paying them 25 cents a day. The most prominent of these women was Annie Jump Cannon, who devised a classification system still used today. Harvard Classification Schem ...
... and catalog the thousands of star spectra that had been collected by the Harvard Observatory. He hired several women to do the work, paying them 25 cents a day. The most prominent of these women was Annie Jump Cannon, who devised a classification system still used today. Harvard Classification Schem ...
O star
... The degree of ionization is determined by the (1) temperature and (2) the density or pressure (pressure is proportional to density times temperature). A higher density at the same temperature leads to a lower ionizationrecombination goes faster- while the converse is true at lower density. Because s ...
... The degree of ionization is determined by the (1) temperature and (2) the density or pressure (pressure is proportional to density times temperature). A higher density at the same temperature leads to a lower ionizationrecombination goes faster- while the converse is true at lower density. Because s ...
Characterizing Stars - Department of Physics and Astronomy
... • The original letter classifications originated from the late 1800s and early 1900s ...
... • The original letter classifications originated from the late 1800s and early 1900s ...
Constellation Part II readingConstellation Part II reading(es)
... Why Do Most Stars and Constellations Move? The stars are distant objects. Their distances vary, but they are all very far away. Excluding our Sun, the nearest star, Proxima Centauri, is more than 4 light years away. As Earth spins on its axis, we, as Earth-bound observers, spin past this background ...
... Why Do Most Stars and Constellations Move? The stars are distant objects. Their distances vary, but they are all very far away. Excluding our Sun, the nearest star, Proxima Centauri, is more than 4 light years away. As Earth spins on its axis, we, as Earth-bound observers, spin past this background ...
Last time: Star Clusters (sec. 19.6)
... sun’s mass and lower), and CNO cycle (dominates in stars more massive than sun; see More Precisely 20-1). Stable, lasts most of star’s lifetime. (Will explain why this is so stable in lecture.) [You already know how lifetime varies with mass.] Depletion of H in core [see Fig. 20.2]. Starting in cent ...
... sun’s mass and lower), and CNO cycle (dominates in stars more massive than sun; see More Precisely 20-1). Stable, lasts most of star’s lifetime. (Will explain why this is so stable in lecture.) [You already know how lifetime varies with mass.] Depletion of H in core [see Fig. 20.2]. Starting in cent ...
ppt
... Because of differential rotation, any radial feature gets wound up very tightly (see figure). ...
... Because of differential rotation, any radial feature gets wound up very tightly (see figure). ...
The Sun, Stars, and Beyond
... • Edwin Hubble ~1929 observed all distant galaxies moving away from us, indicating expansion • Einstein’s General Theory of Relativity mathematically predicts the curvature of space, like in a Black Hole. • This curvature is observed and measured regularly because it changes as time passes and the U ...
... • Edwin Hubble ~1929 observed all distant galaxies moving away from us, indicating expansion • Einstein’s General Theory of Relativity mathematically predicts the curvature of space, like in a Black Hole. • This curvature is observed and measured regularly because it changes as time passes and the U ...
Stellar Properties
... b=spectral class, c=distance measurements 2. Which type of star is hotter? a=G2V, b=A1II, c=M4III, d=O1Ia e=K7IV 3. The sun’s spectrum is perfect continuous spectrum. a=ture, b=false, c=we don’t know! 4. Which type of star is more stable? a=G2V, b=A1II, c=M4III, d=O1Ia e=K7IV 5. H-R diagram is a plo ...
... b=spectral class, c=distance measurements 2. Which type of star is hotter? a=G2V, b=A1II, c=M4III, d=O1Ia e=K7IV 3. The sun’s spectrum is perfect continuous spectrum. a=ture, b=false, c=we don’t know! 4. Which type of star is more stable? a=G2V, b=A1II, c=M4III, d=O1Ia e=K7IV 5. H-R diagram is a plo ...
Star Light, Star Bright: Exploring how stars are classified
... 1. Ensure that students understand what type of information is known about each star by examining the sun as a class. 2. Make sure children notice each star has a name, a color, a temperature and a luminosity value. 3. Make sure they understand the luminosity is compared to the sun's luminosity such ...
... 1. Ensure that students understand what type of information is known about each star by examining the sun as a class. 2. Make sure children notice each star has a name, a color, a temperature and a luminosity value. 3. Make sure they understand the luminosity is compared to the sun's luminosity such ...
Basic Properties of Stars
... Astronomers don’t quote watts (or gigawatts) for stars. Instead they use either • The solar luminosity, i.e., a star that is equal in brightness to the Sun has 1 L. Note the symbol means “Sun”. • An absolute magnitude system ...
... Astronomers don’t quote watts (or gigawatts) for stars. Instead they use either • The solar luminosity, i.e., a star that is equal in brightness to the Sun has 1 L. Note the symbol means “Sun”. • An absolute magnitude system ...
s%nffi - mrtavares
... The brightness of the rnain-sequence stars is also related to their irlass. The hottest blue stars are about 50 times more massive than the sun, while the coolest red stars are only 1/10 as massive. Therefore, on the H-R diagram, the main-sequence stars appear in decreasing order, from hotter, rnore ...
... The brightness of the rnain-sequence stars is also related to their irlass. The hottest blue stars are about 50 times more massive than the sun, while the coolest red stars are only 1/10 as massive. Therefore, on the H-R diagram, the main-sequence stars appear in decreasing order, from hotter, rnore ...
1. absolute brightness -
... classification of stars according to their spectral characteristics. • They are classified according to the spectral lines observed, originally the amount of Hydrogen the lines seemed to indicate. • Today they are ranked in order of surface temperature. O, B, A, F, G, K, M from hottest to coolest. ...
... classification of stars according to their spectral characteristics. • They are classified according to the spectral lines observed, originally the amount of Hydrogen the lines seemed to indicate. • Today they are ranked in order of surface temperature. O, B, A, F, G, K, M from hottest to coolest. ...
GEARS Workshop Monday - Georgia Southern University
... • Astronomers want nothing more than to classify and categorize – just like every other scientist • First thing we do is try to plot things on graphs to see if there is a pattern • Let’s plot two intrinsic properties against one another. ...
... • Astronomers want nothing more than to classify and categorize – just like every other scientist • First thing we do is try to plot things on graphs to see if there is a pattern • Let’s plot two intrinsic properties against one another. ...
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.