Life Cycle of Stars
... At each step write a short explanation of what is happening during that stage. Fill the entire poster with you cycle. You may want to sketch it out in your notebook before you start on the poster paper. Due at end of period at back table. Make sure your name is on it. ...
... At each step write a short explanation of what is happening during that stage. Fill the entire poster with you cycle. You may want to sketch it out in your notebook before you start on the poster paper. Due at end of period at back table. Make sure your name is on it. ...
Pulsating variable stars and the Hertzsprung
... of their lives in this category before evolving up the scale. Class O and B stars in this category are actually very bright and luminous and generally ...
... of their lives in this category before evolving up the scale. Class O and B stars in this category are actually very bright and luminous and generally ...
The Birth, Life, and Death of Stars
... Responsible for reviving interest in GR after WWII Responsible for coining the term “black hole” J.A. Wheeler’s “No Hair Theorem” BH are completely characterized by 3 observable properties – Mass: by its influence on “satellites” orbiting the BH – Charge: by its influence on far-away charges – Angul ...
... Responsible for reviving interest in GR after WWII Responsible for coining the term “black hole” J.A. Wheeler’s “No Hair Theorem” BH are completely characterized by 3 observable properties – Mass: by its influence on “satellites” orbiting the BH – Charge: by its influence on far-away charges – Angul ...
For instance, two hydrogen atoms may fuse together to form one
... elements fuse into heavier ones is called nuclear fusion. Nuclear fusion releases huge amounts of energy. When the core of a clump becomes a hot, dense ball of hydrogen gas fusing into helium gas, a star is born. Astronomers classify stars based on their age, color, and brightness. These characteris ...
... elements fuse into heavier ones is called nuclear fusion. Nuclear fusion releases huge amounts of energy. When the core of a clump becomes a hot, dense ball of hydrogen gas fusing into helium gas, a star is born. Astronomers classify stars based on their age, color, and brightness. These characteris ...
HR Diagram
... luminous it is. If you observe the H-R diagram on the cover of the lab, it is clear that there are fewer luminous stars as compared to the less luminous ones. In terms of the diagram, there are more stars on the lower end than the higher end of the main sequence on the absolute magnitude axis (which ...
... luminous it is. If you observe the H-R diagram on the cover of the lab, it is clear that there are fewer luminous stars as compared to the less luminous ones. In terms of the diagram, there are more stars on the lower end than the higher end of the main sequence on the absolute magnitude axis (which ...
Teacher Guide - Astronomy Outreach at UT Austin
... life cycles. Students perform a play as members of an interview with several different stars. As the play progresses, students develop an understanding of the most fundamental concepts in stellar astronomy. The most important ideas are repeated through out the play. At the conclusion of the activity ...
... life cycles. Students perform a play as members of an interview with several different stars. As the play progresses, students develop an understanding of the most fundamental concepts in stellar astronomy. The most important ideas are repeated through out the play. At the conclusion of the activity ...
What is a Star?
... – Rods distinguish shades of color while cones distinguish color in general. – Cones do not work well with low light, so one is not easily able to distinguish between colors of stars. ...
... – Rods distinguish shades of color while cones distinguish color in general. – Cones do not work well with low light, so one is not easily able to distinguish between colors of stars. ...
(a) Because the core of heavy-mass star never reaches high enough
... 7. Which of the following is the right description of the main sequence stars? (a) Stars on the main sequence are all fusing hydrogen into helium in their cores. (b) Stars on the main sequence are all fusing helium into carbon in their cores. (c) Stars on the main sequence are all fusing carbon int ...
... 7. Which of the following is the right description of the main sequence stars? (a) Stars on the main sequence are all fusing hydrogen into helium in their cores. (b) Stars on the main sequence are all fusing helium into carbon in their cores. (c) Stars on the main sequence are all fusing carbon int ...
Stars and Galaxies part 3
... 400 light-years away, and is most accurate for close stars. • FYI: Hipparcos was a satellite that operated between 1989 and 1993. Its purpose was the accurate measurement of the positions of celestial objects. This permitted the relatively accurate determination of distance to stars up to 400 light ...
... 400 light-years away, and is most accurate for close stars. • FYI: Hipparcos was a satellite that operated between 1989 and 1993. Its purpose was the accurate measurement of the positions of celestial objects. This permitted the relatively accurate determination of distance to stars up to 400 light ...
presentation source
... Radio Astronomy finds the Neutral ISM 1951 Ewen & Purcell detect 21-cm emission from interstellar hydrogen out the window of Harvard’s Jefferson Labs (appreciated as massive amounts of gas, but not concentrated on Bok Globules…) ...
... Radio Astronomy finds the Neutral ISM 1951 Ewen & Purcell detect 21-cm emission from interstellar hydrogen out the window of Harvard’s Jefferson Labs (appreciated as massive amounts of gas, but not concentrated on Bok Globules…) ...
Siriusposter
... The ROSAT all-sky x-ray and extreme ultraviolet (EUV) surveys discovered many new hot white dwarfs. At these energies, white dwarfs are far brighter than most normal stars, and with ROSAT’s help we have been able to identify over 20 of these degenerate objects in binaries with bright, normal compani ...
... The ROSAT all-sky x-ray and extreme ultraviolet (EUV) surveys discovered many new hot white dwarfs. At these energies, white dwarfs are far brighter than most normal stars, and with ROSAT’s help we have been able to identify over 20 of these degenerate objects in binaries with bright, normal compani ...
of a Star
... The Size (Radius) of a Star We already know: flux increases with surface temperature (~ T4); hotter stars are brighter ...
... The Size (Radius) of a Star We already know: flux increases with surface temperature (~ T4); hotter stars are brighter ...
Heavy Metal from Ancient Superstars
... of Stars The chemical compositions of stars reflect the star formation histories of stellar populations The complexity of the Milky Way’s history is reflected in the compositions of its stars ...
... of Stars The chemical compositions of stars reflect the star formation histories of stellar populations The complexity of the Milky Way’s history is reflected in the compositions of its stars ...
Gravitational redshifts
... synthetic line profiles) are shorter than laboratory values due to convective blueshift. Curves before and after mid-transit (µ = 0.21, 0.59, 0.87) are not exact mirror images due to intrinsic stellar line asymmetries. This simulation from a CO5BOLD model predicts the behavior of an Fe I line ( 620 ...
... synthetic line profiles) are shorter than laboratory values due to convective blueshift. Curves before and after mid-transit (µ = 0.21, 0.59, 0.87) are not exact mirror images due to intrinsic stellar line asymmetries. This simulation from a CO5BOLD model predicts the behavior of an Fe I line ( 620 ...
Starbirth and Interstellar Matter
... C. small (micrometers), made of ices, rocks, and metals. D. large (meters), made of ices, rocks, and metals. 5. A way to form hydrogen molecules in interstellar space is by: A. collisions of hydrogen atoms. B. collisions of hydrogen ions. C. collisions of interstellar dust grains. D. sticking and bo ...
... C. small (micrometers), made of ices, rocks, and metals. D. large (meters), made of ices, rocks, and metals. 5. A way to form hydrogen molecules in interstellar space is by: A. collisions of hydrogen atoms. B. collisions of hydrogen ions. C. collisions of interstellar dust grains. D. sticking and bo ...
Document
... 4. What steps are involved in forming a star like the Sun? 5. When a star forms, why does it end up with only a fraction of the available matter? 6. What do star clusters tell us about the formation of stars? 7. Where in the Galaxy does star formation take place? 8. How can the death of one star tri ...
... 4. What steps are involved in forming a star like the Sun? 5. When a star forms, why does it end up with only a fraction of the available matter? 6. What do star clusters tell us about the formation of stars? 7. Where in the Galaxy does star formation take place? 8. How can the death of one star tri ...
Hertzsprung-Russell Diagrams
... Hertzsprung - Russell Diagram The Hertzsprung -Russell (H-R) Diagram is a graph that plots stars color (spectral type or surface temperature) vs. its luminosity (intrinsic brightness or absolute magnitude). On it, astronomers plot stars' color, temperature, luminosity, spectral type, and evolutiona ...
... Hertzsprung - Russell Diagram The Hertzsprung -Russell (H-R) Diagram is a graph that plots stars color (spectral type or surface temperature) vs. its luminosity (intrinsic brightness or absolute magnitude). On it, astronomers plot stars' color, temperature, luminosity, spectral type, and evolutiona ...
ASTRONOMY: WHAT DO YOU NEED TO KNOW
... What is the interstellar medium and what is it made of? Low density dust and gas What is a nebula? A visible cloud of dust and gas Be able to identify the three types of nebulae and give their characteristics: (formation, color) Emission nebulae: are produced when a star (temperatures > 25000K) exci ...
... What is the interstellar medium and what is it made of? Low density dust and gas What is a nebula? A visible cloud of dust and gas Be able to identify the three types of nebulae and give their characteristics: (formation, color) Emission nebulae: are produced when a star (temperatures > 25000K) exci ...
Stars and Nebulae
... from the apparent magnitude, or brightness of the star seen from Earth. A star's absolute magnitude is how bright it would appear when seen from a distance of 10 parsecs (33 light-years). The other system uses roman numerals, with the lowest numeral (I) for the most luminous stars (supergiants) and ...
... from the apparent magnitude, or brightness of the star seen from Earth. A star's absolute magnitude is how bright it would appear when seen from a distance of 10 parsecs (33 light-years). The other system uses roman numerals, with the lowest numeral (I) for the most luminous stars (supergiants) and ...
Characteristics of Stars
... f. shines brightly in the center of a distant galaxy because of the friction of material spiraling around it ...
... f. shines brightly in the center of a distant galaxy because of the friction of material spiraling around it ...
Slide 1
... appears when viewed from Earth; it depends on the absolute brightness but also on the distance of the star: ...
... appears when viewed from Earth; it depends on the absolute brightness but also on the distance of the star: ...
RR animation
... RR Lyrae stars pulse in a manner similar to Cepheid variables, so the mechanism for the pulsation is thought to be similar, but the nature and histories of these stars is thought to be rather different. (The average absolute magnitude of an RR Lyrae is 0.75, only 40 or 50 times brighter than our Sun ...
... RR Lyrae stars pulse in a manner similar to Cepheid variables, so the mechanism for the pulsation is thought to be similar, but the nature and histories of these stars is thought to be rather different. (The average absolute magnitude of an RR Lyrae is 0.75, only 40 or 50 times brighter than our Sun ...
Astro 210 Lecture 4 Sept. 4, 2013 Announcements: • PS 1 available
... Q: how do we know they are giant? a rare few: hot but luminous: “supergiants” not rare but dim and hard to find: very hot but very low-L objects: “white dwarfs” Q: how do we know they are teeny? ...
... Q: how do we know they are giant? a rare few: hot but luminous: “supergiants” not rare but dim and hard to find: very hot but very low-L objects: “white dwarfs” Q: how do we know they are teeny? ...
Stellar Spectral Classes
... The constellation Cassiopeia contains another star with an apparent magnitude of 2.2, absolute magnitude of –4.6 and a surface temperature of 12 000 K. Calculate, for this star, (i) ...
... The constellation Cassiopeia contains another star with an apparent magnitude of 2.2, absolute magnitude of –4.6 and a surface temperature of 12 000 K. Calculate, for this star, (i) ...
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.